Chandra Reveals Elementary Nature of Cassiopeia A

Where do most of the elements essential for life on Earth come from? The answer: inside the furnaces of stars and the explosions that mark the end of some stars' lives.

Astronomers have long studied exploded stars and their remains — known as "supernova remnants" — to better understand exactly how stars produce and then disseminate many of the elements observed on Earth, and in the cosmos at large.

Due to its unique evolutionary status, Cassiopeia A (Cas A) is one of the most intensely studied of these supernova remnants. A new image from NASA's Chandra X-ray Observatory shows the location of different elements in the remains of the explosion: silicon (red), sulfur (yellow), calcium (green) and iron (purple). Each of these elements produces X-rays within narrow energy ranges, allowing maps of their location to be created. The blue color shows high energy X-ray emission, and the blue outer ring in particular is a representation of the expanding blast wave.

X-ray telescopes such as Chandra are important to study supernova remnants and the elements they produce because these events generate extremely high temperatures — millions of degrees — even thousands of years after the explosion. This means that many supernova remnants, including Cas A, glow most strongly at X-ray wavelengths that are undetectable with other types of telescopes.

Chandra's sharp X-ray vision allows astronomers to gather detailed information about the elements that objects like Cas A produce. For example, they are not only able to identify many of the elements that are present, but how much of each are being expelled into interstellar space.

https://chandra.harvard.edu/photo/2017/casa_life/

#space #nova #astrophotography #photography #science #astronomy #physics #nature #NASA #education

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An image from NASA’s Chandra X-ray Observatory shows the location of several elements produced by the explosion of a massive star. Cassiopeia A is a well-known supernova remnant located about 11,000 light years from Earth. Supernova remnants and the elements they produce are very hot — millions of degrees — and glow strongly in X-ray light. Chandra's sharp X-ray vision allows scientists to determine both the amount and location of these crucial elements objects like Cas A produce. Credit: NASA/CXC/SAO Historical Date: December 12, 2017

[...]
X-ray telescopes such as Chandra are important to study supernova remnants and the elements they produce because these events generate extremely high temperatures — millions of degrees — even thousands of years after the explosion. This means that many supernova remnants, including Cas A, glow most strongly at X-ray wavelengths that are undetectable with other types of telescopes.

Chandra's sharp X-ray vision allows astronomers to gather detailed information about the elements that objects like Cas A produce. For example, they are not only able to identify many of the elements that are present, but how much of each are being expelled into interstellar space.

The Chandra data indicate that the supernova that produced Cas A has churned out prodigious amounts of key cosmic ingredients. Cas A has dispersed about 10,000 Earth masses worth of sulfur alone, and about 20,000 Earth masses of silicon. The iron in Cas A has the mass of about 70,000 times that of the Earth, and astronomers detect a whopping one million Earth masses worth of oxygen being ejected into space from Cas A, equivalent to about three times the mass of the Sun. (Even though oxygen is the most abundant element in Cas A, its X-ray emission is spread across a wide range of energies and cannot be isolated in this image, unlike the other elements that are shown.)

While the exact date is not confirmed https://chandra.harvard.edu/graphics/resources/illustrations/historicsnr_infograph.pdf, many experts think that the stellar explosion that created Cas A occurred around the year 1680 in Earth's timeframe. Astronomers estimate that the doomed star was about five times the mass of the Sun just before it exploded. The star is estimated to have started its life with a mass about 16 times that of the Sun, and lost roughly two-thirds of this mass in a vigorous wind blowing off the star several hundred thousand years before the explosion. [...]

https://chandra.harvard.edu/photo/2017/casa_life/

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Location of elements in Cassiopeia A. Credit: NASA/CXC/SAO

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Periodic Table of Elements. Astronomers have found other elements in Cas A in addition to the ones shown in this new Chandra image. Carbon, nitrogen, phosphorus and hydrogen have also been detected using various telescopes that observe different parts of the electromagnetic spectrum. Combined with the detection of oxygen, this means all of the elements needed to make DNA, the molecule that carries genetic information, are found in Cas A. Oxygen is the most abundant element in the human body (about 65% by mass), calcium helps form and maintain healthy bones and teeth, and iron is a vital part of red blood cells that carry oxygen through the body. All of the oxygen in the Solar System comes from exploding massive stars. About half of the calcium and about 40% of the iron also come from these explosions, with the balance of these elements being supplied by explosions of smaller mass, white dwarf stars. Credit: NASA/CXC/K. Divona; Reference: SDSS blog, J. Johnson

[...]
Earlier in its lifetime, the star began fusing hydrogen and helium in its core into heavier elements through the process known as "nucleosynthesis." The energy made by the fusion of heavier and heavier elements balanced the star against the force of gravity. These reactions continued until they formed iron in the core of the star. At this point, further nucleosynthesis would consume rather than produce energy, so gravity then caused the star to implode and form a dense stellar core known as a neutron star.

The exact means by which a massive explosion is produced after the implosion is complicated, and a subject of intense study, but eventually the infalling material outside the neutron star was transformed by further nuclear reactions as it was expelled outward by the supernova explosion.

Chandra has repeatedly observed Cas A since the telescope was launched into space in 1999. The different datasets have revealed new information about the neutron star in Cas A, the details of the explosion, and specifics of how the debris is ejected into space.

* Credits:
NASA's Marshall Space Flight Center in Huntsville, Alabama, manages the Chandra program for NASA's Science Mission Directorate in Washington. The Smithsonian Astrophysical Observatory in Cambridge, Massachusetts, controls Chandra's science and flight operations.

https://chandra.harvard.edu/photo/2017/casa_life/

** Note by grobi:
"To upload this video, I converted it and compressed it to a smaller file-size under linux with the free software ffmpeg and the corresponding command:

'ffmpeg -i video_in.mkv -vcodec libx265 -crf 28 video_out.mp4'

Maybe you would like to post a corresponding video on a scientifically related topic, but it is perhaps too big? Then try ffmpeg."

#space #nova #astrophotography #photography #science #astronomy #physics #nature #NASA #education

Astronomers Solve Mystery of ‘Green Monster’ Feature in Cassiopeia A | Sci.News
[...]
Although astronomers think that this happened around the year 1680, there are no verifiable historical records to confirm this.

A curious structure dubbed the Green Monster was first identified in infrared data from the NASA/ESA/CSA James Webb Space Telescope in April 2023, but its origin was not clear.

However, by combining the Webb data with X-rays from NASA’s Chandra X-ray Observatory, astronomers think they have hunted down the source of this feature.

“We already suspected the Green Monster was created by a blast wave from the exploded star slamming into material surrounding it. Chandra helped us clinch the case,” said Dr. Jacco Vink, an astronomer at the University of Amsterdam.

When a massive star exploded to create Cassiopeia A about 340 years ago, from Earth’s perspective, it created a ball of matter and light that expanded outward. In the outer parts of Cassiopeia A the blast wave is striking surrounding gas that was ejected by the star between about 10,000 and 100,000 years before the explosion.

That formed a favorable environment for dust formation after the ejected stellar material cooled down.

The Chandra data reveal hot gas, mostly from supernova debris including elements like silicon and iron, but also from energetic electrons spiraling around magnetic field lines in the blast wave.

These electrons light up as thin arcs near the blast wave, and also show up in parts of the interior.

Webb highlights infrared emission from dust that is warmed up because it is embedded in the hot gas seen by Chandra, and from much cooler supernova debris.

Despite this chaotic stellar scene, the Green Monster clearly stood out in the original Webb image.
[...]
https://www.sci.news/astronomy/green-monster-feature-cassiopeia-a-12593.html

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New research suggests that the Green Monster — a curious structure first spotted in Webb data in April 2023 — came from that blast wave slamming into material surrounding the Cassiopeia A supernova remnant. This composite image shows the Green Monster structure within the supernova remnant Cassiopeia A. * Image credit: NASA / CXC / SAO / ESA / STScI / CSA / Milisavljevic et al. / JPL / Caltech / J. Schmidt / K. Arcand.

Using NASA’s James Webb Space Telescope, astronomers uncovered a mysterious feature within the remnant, nicknamed the “Green Monster,” alongside a puzzling network of ejecta filaments forming a web of oxygen-rich material. When combined with X-rays from Chandra, the data helped astronomers shed light on the origin of the Green Monster and revealed new insights into the explosion that created Cas A about 340 years ago, from Earth’s perspective.

https://www.nasa.gov/missions/chandra/nasas-chandra-releases-new-3d-models-of-cosmic-objects/#hds-sidebar-nav-1

#space #nova #astrophotography #photography #science #astronomy #physics #nature #NASA #education

How Stars Explode:
Four Ways to Make a Supernova

What makes a star go boom? By understanding supernovae – stellar explosions – scientists can unlock mysteries that are key to what we are made of and the fate of our universe.

https://exoplanets.nasa.gov/news/1493/kepler-beyond-planets-finding-exploding-stars/

CREDIT
Jet Propulsion Laboratory

#space #nova #supernova #astrophotography #photography #science #physics #astronomy #nature #NASA #ESA

2021 August 18
The picture shows a wide field image M57, the Ring Nebula, showing several outer rings not normally seen.

Rings Around the Ring Nebula
* Image Credit: Hubble, Large Binocular Telescope, Subaru Telescope
https://hla.stsci.edu/
http://www.lbto.org/
https://subarutelescope.org/en/;
* Composition & Copyright: Robert Gendler
http://www.robgendlerastropics.com/Biography2.html

Explanation:
The Ring Nebula (M57), is more complicated than it appears through a small telescope. The easily visible central ring is about one light-year across, but this remarkably deep exposure - a collaborative effort combining data from three different large telescopes - explores the looping filaments of glowing gas extending much farther from the nebula's central star. This composite image includes red light emitted by hydrogen as well as visible and infrared light. The Ring Nebula is an elongated planetary nebula, a type of nebula created when a Sun-like star evolves to throw off its outer atmosphere to become a white dwarf star. The Ring Nebula is about 2,500 light-years away toward the musical constellation Lyra.
http://www.robgendlerastropics.com/M57-HST-LBT.html

https://apod.nasa.gov/apod/random_apod.html

#space #nova #astrophotography #photography #science #astronomy #physics #nature #NASA #education #flowers

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2021 August 18 The picture shows a wide field image M57, the Ring Nebula, showing several outer rings not normally seen. Rings Around the Ring Nebula * Image Credit: Hubble, Large Binocular Telescope, Subaru Telescope; * Composition & Copyright: Robert Gendler Explanation: The Ring Nebula (M57), is more complicated than it appears through a small telescope. The easily visible central ring is about one light-year across, but this remarkably deep exposure - a collaborative effort combining data from three different large telescopes - explores the looping filaments of glowing gas extending much farther from the nebula's central star. This composite image includes red light emitted by hydrogen as well as visible and infrared light. The Ring Nebula is an elongated planetary nebula, a type of nebula created when a Sun-like star evolves to throw off its outer atmosphere to become a white dwarf star. The Ring Nebula is about 2,500 light-years away toward the musical constellation Lyra. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply. NASA Web Privacy Policy and Important Notices A service of: ASD at NASA / GSFC & Michigan Tech. U.

This video begins with a ground-based view of the constellation Lyra and zooms into Hubble’s image of the Ring Nebula. It ends with a 3-D model that showcases the structure of the nebula.

Credit:
NASA, ESA, and G. Bacon, F. Summers and Mary Estacion (STScI)

#space #nova #astrophotography #photography #science #astronomy #physics #nature #NASA #education

10 Years ago ..

2016 February 9

The Rise and Fall of Supernova 2015F
* Video Credit & Copyright: Changsu Choi & Myungshin Im (Seoul National University)
https://physics.snu.ac.kr/en

Explanation:
Sit back and watch a star explode. The actual supernova occurred back when dinosaurs roamed the Earth, but images of the spectacular event began arriving last year. Supernova 2015F was discovered in nearby spiral galaxy NGC 2442 by Berto Monard in 2015 March and was unusually bright -- enough to be seen with only a small telescope. The pattern of brightness variation indicated a Type Ia supernova -- a type of stellar explosion that results when an Earth-size white dwarf gains so much mass that its core crosses the threshold of nuclear fusion, possibly caused by a lower mass white-dwarf companion spiraling into it. Finding and tracking Type Ia supernovae are particularly important because their intrinsic brightness can be calibrated, making their apparent brightness a good measure of their distance -- and hence useful toward calibrating the distance scale of the entire universe. The featured video tracked the stellar disruption from before explosion images arrived, as it brightened, and for several months as the fission-powered supernova glow faded. The remnants of SN2015F are now too dim to see without a large telescope. Just yesterday, however, the night sky lit up once again, this time with an even brighter supernova in an even closer galaxy: Centaurus A.

https://apod.nasa.gov/apod/ap160209.html

#space #nova #supernova #astrophotography #photography #science #physics #astronomy #nature #NASA #ESA

Type Ia supernova

From Wikipedia, the free encyclopedia

At the core of a planetary nebula, Henize 2-428, two white dwarf stars slightly under one solar mass each are expected to merge and create a Type Ia supernova destroying both in about 700 million years (artist's impression).

A Type Ia supernova (read: "type one-A") is a type of supernova that occurs in binary systems (two stars orbiting one another) in which one of the stars is a white dwarf. The other star can be anything from a giant star to an even smaller white dwarf.

Physically, carbon–oxygen white dwarfs with a low rate of rotation are limited to below 1.44 solar masses (M☉). Beyond this "critical mass", they reignite and in some cases trigger a supernova explosion; this critical mass is often referred to as the Chandrasekhar mass, but is marginally different from the absolute Chandrasekhar limit, where electron degeneracy pressure is unable to prevent catastrophic collapse. If a white dwarf gradually accretes mass from a binary companion, or merges with a second white dwarf, the general hypothesis is that a white dwarf's core will reach the ignition temperature for carbon fusion as it approaches the Chandrasekhar mass. Within a few seconds of initiation of nuclear fusion, a substantial fraction of the matter in the white dwarf undergoes a runaway reaction, releasing enough energy (1×1044 J) to unbind the star in a supernova explosion.

The Type Ia category of supernova produces a fairly consistent peak luminosity because of the fixed critical mass at which a white dwarf will explode. Their consistent peak luminosity allows these explosions to be used as standard candles to measure the distance to their host galaxies: the visual magnitude of a type Ia supernova, as observed from Earth, indicates its distance from Earth.
[...]
More Info in ALT-Texts

Read more:
https://en.wikipedia.org/wiki/Type_Ia_supernova

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This artist’s impression video shows the central part of the planetary nebula Henize 2-428. The core of this unique object consists of two white dwarf stars, each with a mass a little less than that of the Sun. They are expected to slowly draw closer to each other and merge in around 700 million years. This event will create a dazzling supernova of Type Ia and destroy both stars. CREDIT ESO/L. Calçada 1) [...] The Type Ia supernova is a subcategory in the Minkowski–Zwicky supernova classification scheme, which was devised by German-American astronomer Rudolph Minkowski and Swiss astronomer Fritz Zwicky. There are several means by which a supernova of this type can form, but they share a common underlying mechanism. Theoretical astronomers long believed the progenitor star for this type of supernova is a white dwarf, and empirical evidence for this was found in 2014 when a Type Ia supernova was observed in the galaxy Messier 82. When a slowly-rotating carbon–oxygen white dwarf accretes matter from a companion, it can exceed the Chandrasekhar limit of about 1.44 M☉, beyond which it can no longer support its weight with electron degeneracy pressure. In the absence of a countervailing process, the white dwarf would collapse to form a neutron star, in an accretion-induced non-ejective process, as normally occurs in the case of a white dwarf that is primarily composed of magnesium, neon, and oxygen. [...]

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2) G299 Type Ia supernova remnant. G299 was left over by a particular class of supernovas called Type Ia. Astronomers think that a Type Ia supernova is a thermonuclear explosion – involving the fusion of elements and release of vast amounts of energy − of a white dwarf star in a tight orbit with a companion star. If the white dwarf’s partner is a typical, Sun-like star, the white dwarf can become unstable and explode as it draws material from its companion. Alternatively, the white dwarf is in orbit with another white dwarf, the two may merge and can trigger an explosion. [...] The current view among astronomers who model Type Ia supernova explosions, however, is that this limit is never actually attained and collapse is never initiated. Instead, the increase in pressure and density due to the increasing weight raises the temperature of the core, and as the white dwarf approaches about 99% of the limit, a period of convection ensues, lasting approximately 1,000 years. At some point in this simmering phase, a deflagration flame front is born, powered by carbon fusion. The details of the ignition are still unknown, including the location and number of points where the flame begins. Oxygen fusion is initiated shortly thereafter, but this fuel is not consumed as completely as carbon. Once fusion begins, the temperature of the white dwarf increases. [...]

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The Progenitor of a Type Ia Supernova CREDIT NASA, ESA and A. Feild (STScI); vectorisation by chris 3) [...] A main sequence star supported by thermal pressure can expand and cool which automatically regulates the increase in thermal energy. However, degeneracy pressure is independent of temperature; white dwarfs are unable to regulate temperature in the manner of normal stars, so they are vulnerable to runaway fusion reactions. The flare accelerates dramatically, in part due to the Rayleigh–Taylor instability and interactions with turbulence. It is still a matter of considerable debate whether this flare transforms into a supersonic detonation from a subsonic deflagration. Regardless of the exact details of how the supernova ignites, it is generally accepted that a substantial fraction of the carbon and oxygen in the white dwarf fuses into heavier elements within a period of only a few seconds, with the accompanying release of energy increasing the internal temperature to billions of degrees. The energy released (1–2×1044 J) is more than sufficient to unbind the star; that is, the individual particles making up the white dwarf gain enough kinetic energy to fly apart from each other. The star explodes violently and releases a shock wave in which matter is typically ejected at speeds on the order of 5,000–20,000 km/s, roughly 6% of the speed of light. The energy released in the explosion also causes an extreme increase in luminosity. [...]

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Supercomputer simulation of the explosion phase of the deflagration-to-detonation model of supernova formation. 4) [...] The typical visual absolute magnitude of Type Ia supernovae is Mv = −19.3 (about 5 billion times brighter than the Sun), with little variation. The Type Ia supernova leaves no compact remnant, but the whole mass of the former white dwarf dissipates through space. The theory of this type of supernova is similar to that of novae, in which a white dwarf accretes matter more slowly and does not approach the Chandrasekhar limit. In the case of a nova, the infalling matter causes a hydrogen fusion surface explosion that does not disrupt the star. Type Ia supernovae differ from Type II supernovae, which are caused by the cataclysmic explosion of the outer layers of a massive star as its core collapses, powered by release of gravitational potential energy via neutrino emission. One model for the formation of this category of supernova is a close binary star system. The progenitor binary system consists of main sequence stars, with the primary possessing more mass than the secondary. Being greater in mass, the primary is the first of the pair to evolve onto the asymptotic giant branch, where the star's envelope expands considerably. If the two stars share a common envelope then the system can lose significant amounts of mass, reducing the angular momentum, orbital radius and period. [...]

2025 February 3
A starfield is shown with a large spherical nebula in the center. The nebula shows a great deal of internal structure.

Wolf-Rayet Star 124: Stellar Wind Machine
* Image Credit: Hubble Legacy Archive, NASA, ESA
https://hla.stsci.edu/
https://www.nasa.gov/
https://www.esa.int/
* Processing & License: Judy Schmidt
https://www.flickr.com/photos/geckzilla/

Explanation:
Some stars explode in slow motion. Rare, massive Wolf-Rayet stars are so tumultuous and hot that they are slowly disintegrating right before our telescopes. Glowing gas globs each typically over 30 times more massive than the Earth are being expelled by violent stellar winds. Wolf-Rayet star WR 124, visible near the featured image center, is thus creating the surrounding nebula known as M1-67, which spans six light years across. Details of why this star has been slowly blowing itself apart over the past 20,000 years remains a topic of research. WR 124 lies 15,000 light-years away towards the constellation of the Arrow (Sagitta). The fate of any given Wolf-Rayet star likely depends on how massive it is, but many are thought to end their lives with spectacular explosions such as supernovas or gamma-ray bursts.

https://apod.nasa.gov/apod/ap250203.html

#space #nova #supernova #astrophotography #photography #science #physics #astronomy #nature #NASA #ESA

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2025 February 3 A starfield is shown with a large spherical nebula in the center. The nebula shows a great deal of internal structure. Wolf-Rayet Star 124: Stellar Wind Machine * Image Credit: Hubble Legacy Archive, NASA, ESA * Processing & License: Judy Schmidt Explanation: Some stars explode in slow motion. Rare, massive Wolf-Rayet stars are so tumultuous and hot that they are slowly disintegrating right before our telescopes. Glowing gas globs each typically over 30 times more massive than the Earth are being expelled by violent stellar winds. Wolf-Rayet star WR 124, visible near the featured image center, is thus creating the surrounding nebula known as M1-67, which spans six light years across. Details of why this star has been slowly blowing itself apart over the past 20,000 years remains a topic of research. WR 124 lies 15,000 light-years away towards the constellation of the Arrow (Sagitta). The fate of any given Wolf-Rayet star likely depends on how massive it is, but many are thought to end their lives with spectacular explosions such as supernovas or gamma-ray bursts. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

2018 April 19

NGC 7635: The Bubble Nebula
* Image Credit: NASA, ESA, Hubble Heritage Team -
https://www.nasa.gov/
https://www.spacetelescope.org/
https://heritage.stsci.edu/
* Reprocessing by Maksim Kakitsev
https://www.flickr.com/photos/wildespace/39512823160/

Explanation:
Blown by the wind from a massive star, this interstellar apparition has a surprisingly familiar shape. Cataloged as NGC 7635, it is also known simply as The Bubble Nebula. Although it looks delicate, the 7 light-year diameter bubble offers evidence of violent processes at work. Above and left of the Bubble's center is a hot, O-type star, several hundred thousand times more luminous and some 45 times more massive than the Sun. A fierce stellar wind and intense radiation from that star has blasted out the structure of glowing gas against denser material in a surrounding molecular cloud. The intriguing Bubble Nebula and associated cloud complex lie a mere 7,100 light-years away toward the boastful constellation Cassiopeia. This sharp, tantalizing view of the cosmic bubble is a composite of Hubble Space Telescope image data from 2016, reprocessed to present the nebula's intense narrowband emission in an approximate true color scheme.

https://apod.nasa.gov/apod/ap180419.html

#space #nova #supernova #astrophotography #photography #science #physics #astronomy #nature #NASA #ESA

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2018 April 19 NGC 7635: The Bubble Nebula * Image Credit: NASA, ESA, Hubble Heritage Team - * Reprocessing by Maksim Kakitsev Explanation: Blown by the wind from a massive star, this interstellar apparition has a surprisingly familiar shape. Cataloged as NGC 7635, it is also known simply as The Bubble Nebula. Although it looks delicate, the 7 light-year diameter bubble offers evidence of violent processes at work. Above and left of the Bubble's center is a hot, O-type star, several hundred thousand times more luminous and some 45 times more massive than the Sun. A fierce stellar wind and intense radiation from that star has blasted out the structure of glowing gas against denser material in a surrounding molecular cloud. The intriguing Bubble Nebula and associated cloud complex lie a mere 7,100 light-years away toward the boastful constellation Cassiopeia. This sharp, tantalizing view of the cosmic bubble is a composite of Hubble Space Telescope image data from 2016, reprocessed to present the nebula's intense narrowband emission in an approximate true color scheme. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply. NASA Web Privacy Policy and Important Notices A service of: ASD at NASA / GSFC & Michigan Tech. U.

2002 August 30

Semeis 147: Supernova Remnant
* Credit & Copyright: Steve Mandel

Explanation:
It's easy to get lost following the intricate filaments in this stunningly detailed image of faint supernova remnant Simeis 147. Seen towards the constellation Taurus it covers nearly 3 degrees (6 full moons) on the sky corresponding to a width of 150 light-years at the stellar debris cloud's estimated distance of 3,000 light-years. On three separate nights in December 2001 and January 2002 astronomer Steve Mandel accumulated a total of over eight hours of exposure time to compose this image. He used an astronomical CCD camera, telephoto lens, and his specially designed adapter to allow such wide-field digital imaging. He also used a narrow H-alpha filter to transmit only the the light from recombining hydrogen atoms in the expanding nebulosity, defining the regions of shocked, glowing gas. This supernova remnant has an apparent age of about 100,000 years (light from the original explosion first reached Earth 100,000 years ago) but it is not the only aftermath of the massive stellar explosion. The cosmic catastrophe also left behind a spinning neutron star or pulsar, all that remains of the star's dense core.

https://apod.nasa.gov/apod/ap020830.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA

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2002 August 30 Semeis 147: Supernova Remnant * Credit & Copyright: Steve Mandel Explanation: It's easy to get lost following the intricate filaments in this stunningly detailed image of faint supernova remnant Simeis 147. Seen towards the constellation Taurus it covers nearly 3 degrees (6 full moons) on the sky corresponding to a width of 150 light-years at the stellar debris cloud's estimated distance of 3,000 light-years. On three separate nights in December 2001 and January 2002 astronomer Steve Mandel accumulated a total of over eight hours of exposure time to compose this image. He used an astronomical CCD camera, telephoto lens, and his specially designed adapter to allow such wide-field digital imaging. He also used a narrow H-alpha filter to transmit only the the light from recombining hydrogen atoms in the expanding nebulosity, defining the regions of shocked, glowing gas. This supernova remnant has an apparent age of about 100,000 years (light from the original explosion first reached Earth 100,000 years ago) but it is not the only aftermath of the massive stellar explosion. The cosmic catastrophe also left behind a spinning neutron star or pulsar, all that remains of the star's dense core. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (USRA) NASA Technical Rep.: Jay Norris. Specific rights apply. A service of: LHEA at NASA/ GSFC & Michigan Tech. U.

2025 July 22

A Double Detonation Supernova
* Image Credit: ESO, P. Das et al.; Background stars (NASA/Hubble): K. Noll et al.
https://www.eso.org/
https://www.unsw.edu.au/hdr/priyam-das
https://science.nasa.gov/mission/hubble/

Explanation:
Can some supernovas explode twice? Yes, when the first explosion acts like a detonator for the second. This is a leading hypothesis for the cause of supernova remnant (SNR) 0509-67.5. In this two-star system, gravity causes the larger and fluffier star to give up mass to a smaller and denser white dwarf companion. Eventually the white dwarf's near-surface temperature goes so high that it explodes, creating a shock wave that goes both out and in -- and so triggers a full Type Ia supernova near the center. Recent images of the SNR 0509-67.5 system, like the featured image from the Very Large Telescope in Chile, show two shells with radii and compositions consistent with the double detonation hypothesis. This system, SNR 0509-67.5 is also famous for two standing mysteries: why its bright supernova wasn't noted 400 years ago, and why no visible companion star remains.
https://www.eso.org/public/images/eso2511a/
https://ui.adsabs.harvard.edu/abs/2025NatAs.tmp..135D/abstract

https://en.wikipedia.org/wiki/Detonator
https://apod.nasa.gov/apod/ap970219.html
https://en.wikipedia.org/wiki/Roche_lobe
https://apod.nasa.gov/apod/ap950910.html
https://science.nasa.gov/universe/stars/types/#white-dwarfs

https://en.wikipedia.org/wiki/Type_Ia_supernova

https://apod.nasa.gov/apod/ap250722.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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2025 July 22 A nearly circular nebula with two rings is shown. The outer ring appears orange while while the inner rings is more complex and appears blue. A Double Detonation Supernova * Image Credit: ESO, P. Das et al.; Background stars (NASA/Hubble): K. Noll et al. Explanation: Can some supernovas explode twice? Yes, when the first explosion acts like a detonator for the second. This is a leading hypothesis for the cause of supernova remnant (SNR) 0509-67.5. In this two-star system, gravity causes the larger and fluffier star to give up mass to a smaller and denser white dwarf companion. Eventually the white dwarf's near-surface temperature goes so high that it explodes, creating a shock wave that goes both out and in -- and so triggers a full Type Ia supernova near the center. Recent images of the SNR 0509-67.5 system, like the featured image from the Very Large Telescope in Chile, show two shells with radii and compositions consistent with the double detonation hypothesis. This system, SNR 0509-67.5 is also famous for two standing mysteries: why its bright supernova wasn't noted 400 years ago, and why no visible companion star remains. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

Animation of a double-detonation supernova

This animation illustrates the supernova remnant SNR 0509-67.5, the leftovers of a star that died with a double-detonation. These two blasts imprinted a characteristic layered structure in the expanding material around the star. At the end of the animation we show a real image captured with ESO’s Very Large Telescope (VLT), which displays different chemical elements in different colours. The are two concentric shells of calcium, seen here in blue, a telltale sign that the star met its end with two detonations.

For more details, check: https://www.eso.org/public/news/eso2511/.

Credit:

ESO/M. Kornmesser/P. Das et al. Background stars, final image (Hubble): K. Noll et al.

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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This animation illustrates the supernova remnant SNR 0509-67.5, the leftovers of a star that died with a double-detonation. These two blasts imprinted a characteristic layered structure in the expanding material around the star. At the end of the animation we show a real image captured with ESO’s Very Large Telescope (VLT), which displays different chemical elements in different colours. The are two concentric shells of calcium, seen here in blue, a telltale sign that the star met its end with two detonations. Credit: ESO/M. Kornmesser/P. Das et al. Background stars, final image (Hubble): K. Noll et al.

2012 January 12

The Case of the Missing Supernova Companion
* Image Credit:
** X-ray: NASA/CXC/SAO/J.
Hughes et al.
https://chandra.harvard.edu/
https://www.physics.rutgers.edu/~jackph/
** Optical: NASA/ESA/Hubble Heritage Team (STScI /AURA)
https://science.nasa.gov/mission/hubble/multimedia/hubble-images/
https://www.stsci.edu/

Explanation:
Where's the other star? At the center of this supernova remnant should be the companion star to the star that blew up. Identifying this star is important for understanding just how Type Ia supernova detonate, which in turn could lead to a better understanding of why the brightness of such explosions are so predictable, which in turn is key to calibrating the entire nature of our universe. The trouble is that even a careful inspection of the center of SNR 0509-67.5 has not found any star at all. This indicates that the companion is intrinsically very faint -- much more faint that many types of bright giant stars that had been previous candidates. In fact, the implication is that the companion star might have to be a faint white dwarf, similar to -- but less massive than -- the star that detonated. SNR 0509-67.5 is shown above in both visible light, shining in red as imaged by the Hubble Space Telescope, and X-ray light, shown in false-color green as imaged by the Chandra X-ray Observatory. Putting your cursor over the picture will highlight the central required location for the missing companion star.

https://apod.nasa.gov/apod/ap120112.html#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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2012 January 12 The Case of the Missing Supernova Companion * Image Credit: ** X-ray: NASA/CXC/SAO/J. Hughes et al., ** Optical: NASA/ESA/Hubble Heritage Team (STScI /AURA) Explanation: Where's the other star? At the center of this supernova remnant should be the companion star to the star that blew up. Identifying this star is important for understanding just how Type Ia supernova detonate, which in turn could lead to a better understanding of why the brightness of such explosions are so predictable, which in turn is key to calibrating the entire nature of our universe. The trouble is that even a careful inspection of the center of SNR 0509-67.5 has not found any star at all. This indicates that the companion is intrinsically very faint -- much more faint that many types of bright giant stars that had been previous candidates. In fact, the implication is that the companion star might have to be a faint white dwarf, similar to -- but less massive than -- the star that detonated. SNR 0509-67.5 is shown above in both visible light, shining in red as imaged by the Hubble Space Telescope, and X-ray light, shown in false-color green as imaged by the Chandra X-ray Observatory. Putting your cursor over the picture will highlight the central required location for the missing companion star. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply.

2011 January 25

The Rippled Red Ribbons of SNR 0509
* Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA); Acknowledgment: J. Hughes (Rutgers U.)
https://www.nasa.gov/
https://www.spacetelescope.org/
https://heritage.stsci.edu/
https://www.stsci.edu/portal/
https://www.aura-astronomy.org/

Explanation:
What is causing the picturesque ripples of supernova remnant SNR 0509-67.5? The ripples, as well as the greater nebula, were imaged in unprecedented detail by the Hubble Space Telescope in 2006 and again late last year. The red color was recoded by a Hubble filter that left only the light emitted by energetic hydrogen. The precise reason for the ripples remains unknown, with two considered origin hypotheses relating them to relatively dense portions of either ejected or impacted gas. The reason for the broader red glowing ring is more clear, with expansion speed and light echos relating it to a classic Type Ia supernova explosion that must have occurred about 400 years earlier. SNR 0509 currently spans about 23 light years and lies about 160,000 light years away toward the constellation of the dolphinfish (Dorado) in the Large Magellanic Cloud. The expanding ring carries with it another great mystery, however: why wasn't this supernova seen 400 years ago when light from the initial blast should have passed the Earth?
https://en.wikipedia.org/wiki/SNR_0509-67.5

https://apod.nasa.gov/apod/ap110125.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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2011 January 25 The Rippled Red Ribbons of SNR 0509 * Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA); Acknowledgment: J. Hughes (Rutgers U.) Explanation: What is causing the picturesque ripples of supernova remnant SNR 0509-67.5? The ripples, as well as the greater nebula, were imaged in unprecedented detail by the Hubble Space Telescope in 2006 and again late last year. The red color was recoded by a Hubble filter that left only the light emitted by energetic hydrogen. The precise reason for the ripples remains unknown, with two considered origin hypotheses relating them to relatively dense portions of either ejected or impacted gas. The reason for the broader red glowing ring is more clear, with expansion speed and light echos relating it to a classic Type Ia supernova explosion that must have occurred about 400 years earlier. SNR 0509 currently spans about 23 light years and lies about 160,000 light years away toward the constellation of the dolphinfish (Dorado) in the Large Magellanic Cloud. The expanding ring carries with it another great mystery, however: why wasn't this supernova seen 400 years ago when light from the initial blast should have passed the Earth? Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply. NASA Web Privacy Policy and Important Notices A service of: ASD at NASA / GSFC & Michigan Tech. U.

Double detonation: new image shows remains of star destroyed by pair of explosions

2 July 2025

For the first time, astronomers have obtained visual evidence that a star met its end by detonating twice. By studying the centuries-old remains of supernova SNR 0509-67.5 with the European Southern Observatory’s Very Large Telescope (ESO’s VLT), they have found patterns that confirm its star suffered a pair of explosive blasts. Published today, this discovery shows some of the most important explosions in the Universe in a new light.

Most supernovae are the explosive deaths of massive stars, but one important variety comes from an unassuming source. White dwarfs, the small, inactive cores left over after stars like our Sun burn out their nuclear fuel, can produce what astronomers call a Type Ia supernova.

"The explosions of white dwarfs play a crucial role in astronomy,” says Priyam Das, a PhD student at the University of New South Wales Canberra, Australia, who led the study on SNR 0509-67.5 published today in Nature Astronomy. Much of our knowledge of how the Universe expands rests on Type Ia supernovae, and they are also the primary source of iron on our planet, including the iron in our blood. “Yet, despite their importance, the long-standing puzzle of the exact mechanism triggering their explosion remains unsolved," he adds.

All models that explain Type Ia supernovae begin with a white dwarf in a pair of stars. If it orbits close enough to the other star in this pair, the dwarf can steal material from its partner. In the most established theory behind Type Ia supernovae, the white dwarf [...]

VIDEO:
Zooming into a star that detonated twice

For more details, check: https://www.eso.org/public/news/eso2511/.

Credit:

ESO/L. Calçada/N. Risinger (skysurvey.org)/VMC Survey/Digitized Sky Survey 2/P. Das et al. Background stars (Hubble): K. Noll et al. Music: Azul Cobalto

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

2008 January 15

Double Supernova Remnants DEM L316
* Credit & Copyright: Gemini Observatory, GMOS-South, NSF
https://www.gemini.edu/
https://www.nsf.gov/

Explanation:
Are these two supernova shells related? To help find out, the 8-meter Gemini Telescope located high atop a mountain in Chile was pointed at the unusual, huge, double-lobed cloud dubbed DEM L316. The resulting image, shown above, yields tremendous detail. Inspection of the image as well as data taken by the orbiting Chandra X-Ray Observatory indicate how different the two supernova remnants are. In particular, the smaller shell appears to be the result of Type Ia supernova where a white dwarf exploded, while the larger shell appears to be the result of a Type II supernova where a massive normal star exploded. Since those two stellar types evolve on such different time scales, they likely did not form together and so are likely not physically associated. Considering also that no evidence exists that the shells are colliding, the two shells are now hypothesized to be superposed by chance. DEM L316 lies about 160,000 light years away in the neighboring Large Magellanic Cloud (LMC) galaxy, spans about 140 light-years across, and appears toward the southern constellation of the Swordfish (Dorado).

https://apod.nasa.gov/apod/ap080115.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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2008 January 15 Double Supernova Remnants DEM L316 * Credit & Copyright: Gemini Observatory, GMOS-South, NSF Explanation: Are these two supernova shells related? To help find out, the 8-meter Gemini Telescope located high atop a mountain in Chile was pointed at the unusual, huge, double-lobed cloud dubbed DEM L316. The resulting image, shown above, yields tremendous detail. Inspection of the image as well as data taken by the orbiting Chandra X-Ray Observatory indicate how different the two supernova remnants are. In particular, the smaller shell appears to be the result of Type Ia supernova where a white dwarf exploded, while the larger shell appears to be the result of a Type II supernova where a massive normal star exploded. Since those two stellar types evolve on such different time scales, they likely did not form together and so are likely not physically associated. Considering also that no evidence exists that the shells are colliding, the two shells are now hypothesized to be superposed by chance. DEM L316 lies about 160,000 light years away in the neighboring Large Magellanic Cloud (LMC) galaxy, spans about 140 light-years across, and appears toward the southern constellation of the Swordfish (Dorado). Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply. NASA Web Privacy Policy and Important Notices A service of: ASD at NASA / GSFC & Michigan Tech. U.

2025 July 29

A Helix Nebula Deep Field
* Image Credit & Copyright: George Chatzifrantzis
https://app.astrobin.com/u/pithagoras#gallery

Explanation:
Is the Helix Nebula looking at you? No, not in any biological sense, but it does look quite like an eye. The Helix Nebula is so named because it also appears that you are looking down the axis of a helix. In actuality, it is now understood to have a surprisingly complex geometry, including radial filaments and extended outer loops. The Helix Nebula (aka NGC 7293) is one of brightest and closest examples of a planetary nebula, a gas cloud created at the end of the life of a Sun-like star. The remnant central stellar core, destined to become a white dwarf star, glows in light so energetic it causes the previously expelled gas to fluoresce. The featured picture, taken in red, green, and blue but highlighted by light emitted primarily by hydrogen was created from 12 hours of exposure through a personal telescope located in Greece. A close-up of the inner edge of the Helix Nebula shows complex gas knots the origin of which are still being researched.
https://chandra.harvard.edu/deadstar/helix.html
https://en.wikipedia.org/wiki/Helix_Nebula
https://en.wikipedia.org/wiki/Planetary_nebula

https://mathworld.wolfram.com/Helix.html
http://www.astronomyknowhow.com/hydrogen-alpha.htm
https://youtu.be/WnWIt0iz00A

https://apod.nasa.gov/apod/ap250729.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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2025 July 29 A nearly circular nebula with a blue core surrounded by small white knots, an orange ring and expansive red strucures. A Helix Nebula Deep Field * Image Credit & Copyright: George Chatzifrantzis Explanation: Is the Helix Nebula looking at you? No, not in any biological sense, but it does look quite like an eye. The Helix Nebula is so named because it also appears that you are looking down the axis of a helix. In actuality, it is now understood to have a surprisingly complex geometry, including radial filaments and extended outer loops. The Helix Nebula (aka NGC 7293) is one of brightest and closest examples of a planetary nebula, a gas cloud created at the end of the life of a Sun-like star. The remnant central stellar core, destined to become a white dwarf star, glows in light so energetic it causes the previously expelled gas to fluoresce. The featured picture, taken in red, green, and blue but highlighted by light emitted primarily by hydrogen was created from 12 hours of exposure through a personal telescope located in Greece. A close-up of the inner edge of the Helix Nebula shows complex gas knots the origin of which are still being researched. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

2023 May 7

The Helix Nebula from CFHT
* Image Credit: CFHT, Coelum, MegaCam, J.-C. Cuillandre (CFHT) & G. A. Anselmi (Coelum)
https://www.cfht.hawaii.edu/
https://www.coelum.com/
https://www.cfht.hawaii.edu/Instruments/Imaging/Megacam/
https://www.cfht.hawaii.edu/~jcc/

Explanation:
Will our Sun look like this one day? The Helix Nebula is one of brightest and closest examples of a planetary nebula, a gas cloud created at the end of the life of a Sun-like star. The outer gasses of the star expelled into space appear from our vantage point as if we are looking down a helix. The remnant central stellar core, destined to become a white dwarf star, glows in light so energetic it causes the previously expelled gas to fluoresce. The Helix Nebula, given a technical designation of NGC 7293, lies about 700 light-years away towards the constellation of the Water Bearer (Aquarius) and spans about 2.5 light-years. The featured picture was taken with the Canada-France-Hawaii Telescope (CFHT) located atop a dormant volcano in Hawaii, USA. A close-up of the inner edge of the Helix Nebula shows complex gas knots of unknown origin.
https://en.wikipedia.org/wiki/Aquarius_(constellation)

https://apod.nasa.gov/apod/ap230507.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

Alt...

2023 May 7 A colorful circular nebula is shown that is beige in the center, red further out, and gas violet rings even further out. The Helix Nebula from CFHT * Image Credit: CFHT, Coelum, MegaCam, J.-C. Cuillandre (CFHT) & G. A. Anselmi (Coelum) Explanation: Will our Sun look like this one day? The Helix Nebula is one of brightest and closest examples of a planetary nebula, a gas cloud created at the end of the life of a Sun-like star. The outer gasses of the star expelled into space appear from our vantage point as if we are looking down a helix. The remnant central stellar core, destined to become a white dwarf star, glows in light so energetic it causes the previously expelled gas to fluoresce. The Helix Nebula, given a technical designation of NGC 7293, lies about 700 light-years away towards the constellation of the Water Bearer (Aquarius) and spans about 2.5 light-years. The featured picture was taken with the Canada-France-Hawaii Telescope (CFHT) located atop a dormant volcano in Hawaii, USA. A close-up of the inner edge of the Helix Nebula shows complex gas knots of unknown origin. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply. NASA Web Privacy Policy and Important Notices A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

Helix Nebula Zoom

The Helix Nebula, NGC 7293, lies about 700 light-years away in the constellation of Aquarius (the Water Bearer). It is one of the closest and most spectacular examples of a planetary nebula. These exotic objects have nothing to do with planets, but are the final blooming of Sun-like stars before their retirement as white dwarfs. Shells of gas are blown off from a star’s surface, often in intricate and beautiful patterns, and shine under the harsh ultraviolet radiation from the faint, but very hot, central star. The main ring of the Helix Nebula is about two light-years across or half the distance between the Sun and its closest stellar neighbour.

[...] * see ALT-Text

Although the Helix looks very much like a doughnut, studies have shown that it possibly consists of at least two separate discs with outer rings and filaments. The brighter inner disc seems to be expanding at about 100 000 km/h and to have taken about 12 000 years to have formed.

Because the Helix is relatively close — it covers an area of the sky about a quarter of the full Moon — it can be studied in much greater detail than most other planetary nebulae and has been found to have an unexpected and complex structure. All around the inside of the ring are small blobs, known as “cometary knots”, with faint tails extending away from the central star. They look remarkably like droplets of liquid running down a sheet of glass. Although they look tiny, each knot is about as large as our Solar System. These knots have been extensively studied, both with the ESO Very Large Telescope and with the NASA/ESA Hubble Space Telescope, but remain only partially understood.

https://www.eso.org/public/videos/eso0907a/

CREDIT
ESO
(European Organisation for Astronomical Research in the Southern Hemisphere)

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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Zoom Into The Helix Nebula The Helix Nebula, NGC 7293, lies about 700 light-years away in the constellation of Aquarius (the Water Bearer). It is one of the closest and most spectacular examples of a planetary nebula. These exotic objects have nothing to do with planets, but are the final blooming of Sun-like stars before their retirement as white dwarfs. Shells of gas are blown off from a stars surface, often in intricate and beautiful patterns, and shine under the harsh ultraviolet radiation from the faint, but very hot, central star. The main ring of the Helix Nebula is about two light-years across or half the distance between the Sun and its closest stellar neighbour. * [Despite being photographically very spectacular the Helix is hard to see visually as its light is thinly spread over a large area of sky and the history of its discovery is rather obscure. It first appears in a list of new objects compiled by the German astronomer Karl Ludwig Harding in 1824. The name Helix comes from the rough corkscrew shape seen in the earlier photographs.] Although the Helix looks very much like a doughnut, studies have shown that it possibly consists of at least two separate discs with outer rings and filaments. The brighter inner disc seems to be expanding at about 100 000 km/h and to have taken about 12 000 years to have formed. CREDIT ESO (European Organisation for Astronomical Research in the Southern Hemisphere )

2008 April 13

Curious Cometary Knots in the Helix Nebula
* Credit: C. R. O'Dell and K. Handron (Rice University), NASA
http://www.nasa.gov/

Explanation:
What causes unusual knots of gas and dust in planetary nebulas? Seen also in the Ring Nebula, the Dumbbell Nebula and NGC 2392, the knots' existence was not initially predicted and their origins are still not well understood. Pictured above is a fascinating image of the Helix Nebula by the Hubble Space Telescope showing tremendous detail of its mysterious gaseous knots. The above cometary knots have masses similar to the Earth but have radii typically several times the orbit of Pluto. One hypothesis for the fragmentation and evolution of the knots includes existing gas being driven out by a less dense but highly energetic stellar wind of the central evolving star. The Helix Nebula is the closest example of a planetary nebula created at the end of the life of a Sun-like star. The Helix Nebula, given a technical designation of NGC 7293, lies about 700 light-years away towards the constellation of Aquarius.

https://en.wikipedia.org/wiki/Rayleigh%E2%80%93Taylor_instability
https://en.wikipedia.org/wiki/Stellar_wind
https://ui.adsabs.harvard.edu/abs/2020MNRAS.491..758A/abstract

https://apod.nasa.gov/apod/ap080413.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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2008 April 13 Curious Cometary Knots in the Helix Nebula * Credit: C. R. O'Dell and K. Handron (Rice University), NASA Explanation: What causes unusual knots of gas and dust in planetary nebulas? Seen also in the Ring Nebula, the Dumbbell Nebula and NGC 2392, the knots' existence was not initially predicted and their origins are still not well understood. Pictured above is a fascinating image of the Helix Nebula by the Hubble Space Telescope showing tremendous detail of its mysterious gaseous knots. The above cometary knots have masses similar to the Earth but have radii typically several times the orbit of Pluto. One hypothesis for the fragmentation and evolution of the knots includes existing gas being driven out by a less dense but highly energetic stellar wind of the central evolving star. The Helix Nebula is the closest example of a planetary nebula created at the end of the life of a Sun-like star. The Helix Nebula, given a technical designation of NGC 7293, lies about 700 light-years away towards the constellation of Aquarius. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply. NASA Web Privacy Policy and Important Notices A service of: ASD at NASA / GSFC & Michigan Tech. U.

From Wikipedia, the free encyclopedia

[...]
The Helix Nebula is thought to be shaped like a prolate spheroid with strong density concentrations toward the filled disk along the equatorial plane, whose major axis is inclined about 21° to 37° from our vantage point. The size of the inner disk is 8×19 arcmin in diameter (0.52 pc); the outer torus is 12×22 arcmin in diameter (0.77 pc); and the outer-most ring is about 25 arcmin in diameter (1.76 pc). The outer-most ring appears flattened on one side due to it colliding with the ambient interstellar medium.

Expansion of the whole planetary nebula structure is estimated to have occurred in the last 6,560 years, and 12,100 years for the inner disk. Spectroscopically, the outer ring's expansion rate is 40 km/s, and about 32 km/s for the inner disk.
The Helix Nebula was the first planetary nebula discovered to contain cometary knots. Its main ring contains knots of nebulosity, which have now been detected in several nearby planetary nebulae, especially those with a molecular envelope like the Ring nebula and the Dumbbell Nebula.

These knots are radially symmetrical (from the CS) and are described as "cometary", each centered on a core of neutral molecular gas and containing bright local photoionization fronts or cusps towards the central star and tails away from it. All tails extend away from the Planetary Nebula Nucleus (PNN) in a radial direction. Excluding the tails, each knot is approximately the size of the Solar System, while each of the cusp knots are optically thick due to Lyc photons from the CS. There are about 40,000 cometary knots in the Helix Nebula.
[...] * more in the ALT-Text

CREDIT
+ Text excerpt
by Contributors to Wikimedia projects
+ Video credit
Magnetosheath (YT)
https://www.youtube.com/channel/UC2wcz4CLDO7CrSKOUl9o8qg/about

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

2021 October 14

NGC 7293: The Helix Nebula
* Image Credit & Copyright: Ignacio Diaz Bobillo
https://www.pampaskies.com/gallery3/index.php

Explanation:
A mere seven hundred light years from Earth, toward the constellation Aquarius, a sun-like star is dying. Its last few thousand years have produced the Helix Nebula (NGC 7293), a well studied and nearby example of a Planetary Nebula, typical of this final phase of stellar evolution. A total of 90 hours of exposure time have gone in to creating this expansive view of the nebula. Combining narrow band image data from emission lines of hydrogen atoms in red and oxygen atoms in blue-green hues, it shows remarkable details of the Helix's brighter inner region about 3 light-years across. The white dot at the Helix's center is this Planetary Nebula's hot, central star. A simple looking nebula at first glance, the Helix is now understood to have a surprisingly complex geometry.
https://www.pampaskies.com/gallery3/Deep-Space-Objects/Helix_Oxygen_crop2_small
https://science.nasa.gov/missions/hubble/a-new-twist-on-an-old-nebula/

https://apod.nasa.gov/apod/ap211014.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

Alt...

2021 October 14 NGC 7293: The Helix Nebula * Image Credit & Copyright: Ignacio Diaz Bobillo Explanation: A mere seven hundred light years from Earth, toward the constellation Aquarius, a sun-like star is dying. Its last few thousand years have produced the Helix Nebula (NGC 7293), a well studied and nearby example of a Planetary Nebula, typical of this final phase of stellar evolution. A total of 90 hours of exposure time have gone in to creating this expansive view of the nebula. Combining narrow band image data from emission lines of hydrogen atoms in red and oxygen atoms in blue-green hues, it shows remarkable details of the Helix's brighter inner region about 3 light-years across. The white dot at the Helix's center is this Planetary Nebula's hot, central star. A simple looking nebula at first glance, the Helix is now understood to have a surprisingly complex geometry. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply. NASA Web Privacy Policy and Important Notices A service of: ASD at NASA / GSFC & Michigan Tech. U.

2009 December 31

Dust and the Helix Nebula
* NASA, JPL-Caltech, Kate Su (Steward Obs., U. Arizona), et al.
http://ssc.spitzer.caltech.edu/
https://astro.arizona.edu/
https://arxiv.org/abs/astro-ph/0702296
http://www.nasa.gov/home/index.html

Explanation:
Dust makes this cosmic eye look red. The eerie Spitzer Space Telescope image shows infrared radiation from the well-studied Helix Nebula (NGC 7293) a mere 700 light-years away in the constellation Aquarius. The two light-year diameter shroud of dust and gas around a central white dwarf has long been considered an excellent example of a planetary nebula, representing the final stages in the evolution of a sun-like star. But the Spitzer data show the nebula's central star itself is immersed in a surprisingly bright infrared glow. Models suggest the glow is produced by a dust debris disk. Even though the nebular material was ejected from the star many thousands of years ago, the close-in dust could be generated by collisions in a reservoir of objects analogous to our own solar system's Kuiper Belt or cometary Oort cloud. Formed in the distant planetary system, the comet-like bodies would have otherwise survived even the dramatic late stages of the star's evolution.

https://coolcosmos.ipac.caltech.edu//
http://maps.seds.org/Stars_en/Fig/aquarius.html
https://apod.nasa.gov/apod/ap041210.html
http://www2.ess.ucla.edu/~jewitt/kb.html
!> https://en.wikipedia.org/wiki/Stellar_evolution

https://apod.nasa.gov/apod/ap091231.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

Alt...

2009 December 31 Dust and the Helix Nebula * NASA, JPL-Caltech, Kate Su (Steward Obs., U. Arizona), et al. Explanation: Dust makes this cosmic eye look red. The eerie Spitzer Space Telescope image shows infrared radiation from the well-studied Helix Nebula (NGC 7293) a mere 700 light-years away in the constellation Aquarius. The two light-year diameter shroud of dust and gas around a central white dwarf has long been considered an excellent example of a planetary nebula, representing the final stages in the evolution of a sun-like star. But the Spitzer data show the nebula's central star itself is immersed in a surprisingly bright infrared glow. Models suggest the glow is produced by a dust debris disk. Even though the nebular material was ejected from the star many thousands of years ago, the close-in dust could be generated by collisions in a reservoir of objects analogous to our own solar system's Kuiper Belt or cometary Oort cloud. Formed in the distant planetary system, the comet-like bodies would have otherwise survived even the dramatic late stages of the star's evolution. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply. NASA Web Privacy Policy and Important Notices A service of: ASD at NASA / GSFC & Michigan Tech. U.

2006 January 12

Infrared Helix
* Credit: J. Hora (Harvard-Smithsonian CfA) et al., (SSC/Caltech), JPL-Caltech, NASA
https://www.cfa.harvard.edu/
https://irsa.ipac.caltech.edu/data/SPITZER/docs/
http://www.jpl.nasa.gov/
http://www.nasa.gov/home/index.html

Explanation:
Over six hundred light years from Earth, in the constellation Aquarius, a sun-like star is dying. Its last few thousand years have produced the Helix Nebula (NGC 7293), a well studied and nearby example of a Planetary Nebula, typical of this final phase of stellar evolution. Emission in this infrared Spitzer Space Telescope image of the Helix comes mostly from the nebula's molecular hydrogen gas. The gas appears to be clumpy, forming thousands of comet-shaped knots each spanning about twice the size of our solar system. Bluer, more energetic radiation is seen to come from the heads with redder emission from the tails, suggesting that they are more shielded from the central star's winds and intense ultraviolet radiation. The nebula itself is about 2.5 light-years across. The Sun is expected to go through its own Planetary Nebula phase ... in another 5 billion years.

!> http://hawastsoc.org/deepsky/aqr/index.html

https://apod.nasa.gov/apod/ap060112.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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2006 January 12 Infrared Helix * Credit: J. Hora (Harvard-Smithsonian CfA) et al., (SSC/Caltech), JPL-Caltech, NASA Explanation: Over six hundred light years from Earth, in the constellation Aquarius, a sun-like star is dying. Its last few thousand years have produced the Helix Nebula (NGC 7293), a well studied and nearby example of a Planetary Nebula, typical of this final phase of stellar evolution. Emission in this infrared Spitzer Space Telescope image of the Helix comes mostly from the nebula's molecular hydrogen gas. The gas appears to be clumpy, forming thousands of comet-shaped knots each spanning about twice the size of our solar system. Bluer, more energetic radiation is seen to come from the heads with redder emission from the tails, suggesting that they are more shielded from the central star's winds and intense ultraviolet radiation. The nebula itself is about 2.5 light-years across. The Sun is expected to go through its own Planetary Nebula phase ... in another 5 billion years. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (USRA) NASA Web Site Statements, Warnings, and Disclaimers NASA Official: Jay Norris. Specific rights apply. A service of: EUD at NASA / GSFC & Michigan Tech. U.

2025 July 31

Supernova 2025rbs in NGC 7331
* Image Credit: Ben Godson (University of Warwick)
https://warwick.ac.uk/fac/sci/physics/research/astro/people/bengodson/

Explanation:
A long time ago in a galaxy 50 million light-years away, a star exploded. Light from that supernova was first detected by telescopes on planet Earth on July 14th though, and the extragalactic transient is now known to astronomers as supernova 2025rbs. Presently the brightest supernova in planet Earth's sky, 2025rbs is a Type Ia supernova, likely caused by the thermonuclear detonation of a white dwarf star that accreted material from a companion in a binary star system. Type Ia supernovae are used as standard candles to establish the distance scale of the universe. The host galaxy of 2025rbs is NGC 7331. Itself a bright spiral galaxy in the northern constellation Pegasus, NGC 7331 is often touted as an analog to our own Milky Way.
https://goto-observatory.org/bright-supernova-2025rbs-discovered-by-goto/
https://www.wis-tns.org/object/2025rbs
https://rochesterastronomy.org/supernova.html

https://apod.nasa.gov/apod/ap250731.html

#space #supernova #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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2025 July 31 Supernova 2025rbs in NGC 7331 * Image Credit: Ben Godson (University of Warwick) Explanation: A long time ago in a galaxy 50 million light-years away, a star exploded. Light from that supernova was first detected by telescopes on planet Earth on July 14th though, and the extragalactic transient is now known to astronomers as supernova 2025rbs. Presently the brightest supernova in planet Earth's sky, 2025rbs is a Type Ia supernova, likely caused by the thermonuclear detonation of a white dwarf star that accreted material from a companion in a binary star system. Type Ia supernovae are used as standard candles to establish the distance scale of the universe. The host galaxy of 2025rbs is NGC 7331. Itself a bright spiral galaxy in the northern constellation Pegasus, NGC 7331 is often touted as an analog to our own Milky Way. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

Type Ia Supernovae
By jmbrill

Roman will use type Ia supernovae to measure cosmic distances, which will help us understand how the universe has expanded over time.

* Video Credit:
NASA Goddard's Scientific Visualization Studio

Roman will see thousands of exploding stars called supernovae across vast stretches of time and space. Using these observations, astronomers aim to shine a light on several cosmic mysteries – primarily dark energy. Roman will use type Ia supernovae to measure cosmic distances, which will help us understand how the universe has expanded over time.

Roman’s supernova survey will help clear up clashing measurements of how fast the universe is currently expanding, and even provide a new way to probe the distribution of dark matter, which is detectable only through its gravitational effects. One of the mission’s primary science goals involves using supernovae to help pin down the nature of dark energy – the unexplained cosmic pressure that’s speeding up the expansion of the universe.

Roman will use multiple methods to investigate dark energy. One involves surveying the sky for a special type of exploding star, called a type Ia supernova.

Many supernovae occur when massive stars run out of fuel, rapidly collapse under their own weight, and then explode because of strong shock waves that propel out of their interiors. These supernovae occur about once every 50 years in our Milky Way galaxy. But evidence shows that type Ia supernovae originate from some binary star systems that contain at least one white dwarf – the small, hot core remnant of a Sun-like star. Type Ia supernovae are much rarer, happening roughly once every 500 years in the Milky Way.
[...]
Read more in next reply

https://science.nasa.gov/mission/roman-space-telescope/type-ia-supernovae/

You might also be interested in:
TOPIC> "As Far As We Can See" https://defcon.social/@grobi/114626118056153533

#space #supernova #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

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NASA’s upcoming Nancy Grace Roman Space Telescope will see thousands of exploding stars called supernovae across vast stretches of time and space. Using these observations, astronomers aim to shine a light on several cosmic mysteries, providing a window onto the universe’s distant past and hazy present. Read more: http://www.nasa.gov/feature/goddard/2... Roman’s supernova survey will help clear up clashing measurements of how fast the universe is currently expanding, and even provide a new way to probe the distribution of dark matter, which is detectable only through its gravitational effects. One of the mission’s primary science goals involves using supernovae to help pin down the nature of dark energy – the unexplained cosmic pressure that’s speeding up the expansion of the universe. Roman will use multiple methods to investigate dark energy. One involves surveying the sky for a special type of exploding star, called a type Ia supernova. Music: "Relentless Data" from Universal Production Music Video credit: NASA's Goddard Space Flight Center Scott Wiessinger (USRA): Producer Ashley Balzer (ADNET): Science Writer Adriana Manrique Gutierrez (USRA): Lead Animator Claire Andreoli (NASA/GSFC): Public Affairs Officer Barb Mattson (University of Maryland College Park): Narrator Scott Wiessinger (USRA): Animator Scott Wiessinger (USRA): Writer Scott Wiessinger (USRA): Editor

By jmbrill

[...]
In some cases, the dwarf may siphon material from its companion. This ultimately triggers a runaway reaction that detonates the thief once it reaches a specific point where it has gained so much mass that it becomes unstable. Astronomers have also found evidence supporting another scenario, involving two white dwarfs that spiral toward each other until they merge. If their combined mass is high enough that it leads to instability, they, too, may produce a type Ia supernova.

These explosions peak at a similar, known intrinsic brightness, making type Ia supernovae so-called standard candles – objects or events that emit a specific amount of light, allowing scientists to find their distance with a straightforward formula. Because of this, astronomers can determine how far away the supernovae are by simply measuring how bright they appear.

Astronomers will also use Roman to study the light of these supernovae to find out how quickly they appear to be moving away from us. By comparing how fast they’re receding at different distances, scientists will trace cosmic expansion over time. This will help us understand whether and how dark energy has changed throughout the history of the universe.

Previous type Ia supernova surveys have concentrated on the relatively nearby universe, largely due to instrument limitations. Roman’s infrared vision, gigantic field of view, and exquisite sensitivity will dramatically extend the search, pulling the cosmic curtains far enough aside to allow astronomers to spot thousands of distant type Ia supernovae.

Roman will study dark energy’s influence in detail over more than half of the universe’s history, when it was between about 4 and 12 billion years old. Exploring this relatively unprobed region will help scientists add crucial pieces to the dark energy puzzle.

Video Credit:
NGSVS

https://science.nasa.gov/mission/roman-space-telescope/type-ia-supernovae/

#space #supernova #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA #education

2025 August 22

A Tale of Two Nebulae
* Image Credit & Copyright: Kent Biggs
https://www.kentbiggs.com/index.htm

Explanation:
This colorful telescopic view towards the musical northern constellation Lyra reveals the faint outer halos and brighter central ring-shaped region of M57, popularly known as the Ring Nebula. To modern astronomers M57 is a well-known planetary nebula. With a central ring about one light-year across, M57 is definitely not a planet though, but the gaseous shroud of one of the Milky Way's dying sun-like stars. Roughly the same apparent size as M57, the fainter and more often overlooked barred spiral galaxy at the left is IC 1296. In fact, over 100 years ago IC 1296 would have been known as a spiral nebula. By chance the pair are in the same field of view, and while they appear to have similar sizes they are actually very far apart. At a distance of a mere 2,000 light-years M57 is well within our own Milky Way galaxy. Extragalactic IC 1296 (aka PGC62532) is more like 200,000,000 light-years distant. That's about 100,000 times farther away than M57 but since they appear roughly similar in size, former spiral nebula IC 1296 must also be about 100,000 times larger than planetary nebula M57. Look closely at the sharp 21st century astroimage to spot even more distant background galaxies scattered through the frame.
https://www.kentbiggs.com/images/planetaries/M57.htm
https://webbtelescope.org/contents/media/images/01H82G0PP38P6PBXQ11BEVSMY0

https://en.wikipedia.org/wiki/Planetary_nebula
https://physics.weber.edu/palen/phsx1040/lectures/lplanneb.html
https://courses.ems.psu.edu/astro801/content/l9_p2.html

https://apod.nasa.gov/apod/ap250822.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA

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2025 August 22 A Tale of Two Nebulae * Image Credit & Copyright: Kent Biggs Explanation: This colorful telescopic view towards the musical northern constellation Lyra reveals the faint outer halos and brighter central ring-shaped region of M57, popularly known as the Ring Nebula. To modern astronomers M57 is a well-known planetary nebula. With a central ring about one light-year across, M57 is definitely not a planet though, but the gaseous shroud of one of the Milky Way's dying sun-like stars. Roughly the same apparent size as M57, the fainter and more often overlooked barred spiral galaxy at the left is IC 1296. In fact, over 100 years ago IC 1296 would have been known as a spiral nebula. By chance the pair are in the same field of view, and while they appear to have similar sizes they are actually very far apart. At a distance of a mere 2,000 light-years M57 is well within our own Milky Way galaxy. Extragalactic IC 1296 (aka PGC62532) is more like 200,000,000 light-years distant. That's about 100,000 times farther away than M57 but since they appear roughly similar in size, former spiral nebula IC 1296 must also be about 100,000 times larger than planetary nebula M57. Look closely at the sharp 21st century astroimage to spot even more distant background galaxies scattered through the frame. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply.

2025 August 24

The Spinning Pulsar of the Crab Nebula
* Image Credit: NASA: X-ray: Chandra (CXC)
https://www.nasa.gov/
https://chandra.harvard.edu/
* Optical: Hubble (STScI)
https://www.stsci.edu/hst
* Infrared: Spitzer (JPL-Caltech)
https://www.spitzer.caltech.edu/

Explanation:
At the core of the Crab Nebula lies a city-sized, magnetized neutron star spinning 30 times a second. Known as the Crab Pulsar, it is the bright spot in the center of the gaseous swirl at the nebula's core. About twelve light-years across, the spectacular picture frames the glowing gas, cavities and swirling filaments near the Crab Nebula's center. The featured picture combines visible light from the Hubble Space Telescope in purple, X-ray light from the Chandra X-ray Observatory in blue, and infrared light from the Spitzer Space Telescope in red. Like a cosmic dynamo, the Crab pulsar powers the emission from the nebula, driving a shock wave through surrounding material and accelerating the spiraling electrons. With more mass than the Sun and the density of an atomic nucleus,the spinning pulsar is the collapsed core of a massive star that exploded. The outer parts of the Crab Nebula are the expanding remnants of the star's component gases. The supernova explosion was witnessed on planet Earth in the year 1054.
https://chandra.harvard.edu/photo/2018/crab/
https://chandra.harvard.edu/chronicle/0201/vela.html
https://apod.nasa.gov/apod/ap010602.html
https://en.wikipedia.org/wiki/Crab_Pulsar
https://en.wikipedia.org/wiki/Neutron_star
http://hyperphysics.phy-astr.gsu.edu/hbase/Nuclear/nucuni.html

https://defcon.social/@grobi/114793535752274563
https://defcon.social/@grobi/114793623955569092

https://apod.nasa.gov/apod/ap250824.html

#space #nebula #supernova #pulsar #astrophotography #photography #science #astronomy #physics #nature #NASA

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2025 August 24 The featured image shows the center of the Crab Nebula in colors mapped to Hubble, Chandra, and Spitzer space telescopes. The Crab pulsar appears in the center surrounded by a spinning disk. The Spinning Pulsar of the Crab Nebula * Image Credit: NASA: X-ray: Chandra (CXC) * Optical: Hubble (STScI) * Infrared: Spitzer (JPL-Caltech) Explanation: At the core of the Crab Nebula lies a city-sized, magnetized neutron star spinning 30 times a second. Known as the Crab Pulsar, it is the bright spot in the center of the gaseous swirl at the nebula's core. About twelve light-years across, the spectacular picture frames the glowing gas, cavities and swirling filaments near the Crab Nebula's center. The featured picture combines visible light from the Hubble Space Telescope in purple, X-ray light from the Chandra X-ray Observatory in blue, and infrared light from the Spitzer Space Telescope in red. Like a cosmic dynamo, the Crab pulsar powers the emission from the nebula, driving a shock wave through surrounding material and accelerating the spiraling electrons. With more mass than the Sun and the density of an atomic nucleus,the spinning pulsar is the collapsed core of a massive star that exploded. The outer parts of the Crab Nebula are the expanding remnants of the star's component gases. The supernova explosion was witnessed on planet Earth in the year 1054. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn

2022 March 4

The Multiwavelength Crab
* Image Credit: NASA, ESA, G. Dubner (IAFE, CONICET-University of Buenos Aires) et al.;
A. Loll et al.; T. Temim et al.; F. Seward et al.; VLA/NRAO/AUI/NSF; Chandra/CXC;
Spitzer/JPL-Caltech; XMM-Newton/ESA; Hubble/STScI

https://arxiv.org/abs/1704.02968

Explanation:
The Crab Nebula is cataloged as M1, the first object on Charles Messier's famous list of things which are not comets. In fact, the Crab is now known to be a supernova remnant, expanding debris from massive star's death explosion, witnessed on planet Earth in 1054 AD. This brave new image offers a 21st century view of the Crab Nebula by presenting image data from across the electromagnetic spectrum as wavelengths of visible light. From space, Chandra (X-ray) XMM-Newton (ultraviolet), Hubble (visible), and Spitzer (infrared), data are in purple, blue, green, and yellow hues. From the ground, Very Large Array radio wavelength data is shown in red. One of the most exotic objects known to modern astronomers, the Crab Pulsar, a neutron star spinning 30 times a second, is the bright spot near picture center. Like a cosmic dynamo, this collapsed remnant of the stellar core powers the Crab's emission across the electromagnetic spectrum. Spanning about 12 light-years, the Crab Nebula is 6,500 light-years away in the constellation Taurus.

https://apod.nasa.gov/apod/ap220304.html

#space #nebula #pulsar #astrophotography #photography #science #astronomy #physics #nature #NASA

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2022 March 4 The Multiwavelength Crab * Image Credit: NASA, ESA, G. Dubner (IAFE, CONICET-University of Buenos Aires) et al.; A. Loll et al.; T. Temim et al.; F. Seward et al.; VLA/NRAO/AUI/NSF; Chandra/CXC; Spitzer/JPL-Caltech; XMM-Newton/ESA; Hubble/STScI Explanation: The Crab Nebula is cataloged as M1, the first object on Charles Messier's famous list of things which are not comets. In fact, the Crab is now known to be a supernova remnant, expanding debris from massive star's death explosion, witnessed on planet Earth in 1054 AD. This brave new image offers a 21st century view of the Crab Nebula by presenting image data from across the electromagnetic spectrum as wavelengths of visible light. From space, Chandra (X-ray) XMM-Newton (ultraviolet), Hubble (visible), and Spitzer (infrared), data are in purple, blue, green, and yellow hues. From the ground, Very Large Array radio wavelength data is shown in red. One of the most exotic objects known to modern astronomers, the Crab Pulsar, a neutron star spinning 30 times a second, is the bright spot near picture center. Like a cosmic dynamo, this collapsed remnant of the stellar core powers the Crab's emission across the electromagnetic spectrum. Spanning about 12 light-years, the Crab Nebula is 6,500 light-years away in the constellation Taurus. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply.

The ultimate movie (SOUND ON!) of the millisecond pulsar in the heart of the Crab Nebula, a spinning neutron star rotating once every 33 milliseconds, or 30 times each second.
This nasahubble movie shows dynamic rings, wisps and jets of matter and antimatter around the pulsar in the Crab Nebula as observed in optical light. The Crab Pulsar is one of very few pulsars to be identified optically. The optical pulsar is roughly 20 kilometres (12 mi) in diameter.

CREDIT
NASA/nasahubble

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA

2024 July 23

The Crab Nebula from Visible to X-Ray
* Image Credit: NASA, ESA, ASI, Hubble, Chandra, IXPE
https://www.nasa.gov/
https://www.esa.int/
https://www.asi.it/
https://science.nasa.gov/mission/hubble/
https://www.nasa.gov/mission/chandra-x-ray-observatory/
https://www.nasa.gov/mission/imaging-x-ray-polarimetry-explorer-ixpe/

Explanation:
What powers the Crab Nebula? A city-sized magnetized neutron star spinning around 30 times a second. Known as the Crab Pulsar, it is the bright spot in the center of the gaseous swirl at the nebula's core. About 10 light-years across, the spectacular picture of the Crab Nebula (M1) frames a swirling central disk and complex filaments of surrounding and expanding glowing gas. The picture combines visible light from the Hubble Space Telescope in red and blue with X-ray light from the Chandra X-ray Observatory shown in white, and diffuse X-ray emission detected by Imaging X-ray Polarimetry Explorer (IXPE) in diffuse purple. The central pulsar powers the Crab Nebula's emission and expansion by slightly slowing its spin rate, which drives out a wind of energetic electrons. The featured image released today, the 25th Anniversary of the launch of NASA's flagship-class X-ray Observatory: Chandra.

https://apod.nasa.gov/apod/ap240723.html

#space #nebula #pulsar #astrophotography #photography #science #astronomy #physics #matter #antimatter #nature #NASA #ESA #ASI

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2024 July 23 A multi-colored nebula is shown that is the expanding remnant of an exploded star. The central white and purple colors show X-ray light, while the outer red and blue colors show visible light. The Crab Nebula from Visible to X-Ray * Image Credit: NASA, ESA, ASI, Hubble, Chandra, IXPE Explanation: What powers the Crab Nebula? A city-sized magnetized neutron star spinning around 30 times a second. Known as the Crab Pulsar, it is the bright spot in the center of the gaseous swirl at the nebula's core. About 10 light-years across, the spectacular picture of the Crab Nebula (M1) frames a swirling central disk and complex filaments of surrounding and expanding glowing gas. The picture combines visible light from the Hubble Space Telescope in red and blue with X-ray light from the Chandra X-ray Observatory shown in white, and diffuse X-ray emission detected by Imaging X-ray Polarimetry Explorer (IXPE) in diffuse purple. The central pulsar powers the Crab Nebula's emission and expansion by slightly slowing its spin rate, which drives out a wind of energetic electrons. The featured image released today, the 25th Anniversary of the launch of NASA's flagship-class X-ray Observatory: Chandra. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

2024 August 23

Supernova Remnant CTA 1
* Image Credit & Copyright: Thomas Lelu

Explanation:
There is a quiet pulsar at the heart of CTA 1. The supernova remnant was discovered as a source of emission at radio wavelengths by astronomers in 1960 and since identified as the result of the death explosion of a massive star. But no radio pulses were detected from the expected pulsar, the rotating neutron star remnant of the massive star's collapsed core. Seen about 10,000 years after the initial supernova explosion, the interstellar debris cloud is faint at optical wavelengths. CTA 1's visible wavelength emission from still expanding shock fronts is revealed in this deep telescopic image, a frame that spans about 2 degrees across a starfield in the northern constellation of Cepheus. While no pulsar has since been found at radio wavelengths, in 2008 the Fermi Gamma-ray Space Telescope detected pulsed emission from CTA 1, identifying the supernova remnant's rotating neutron star. The source has been recognized as the first in a growing class of pulsars that are quiet at radio wavelengths but pulse in high-energy gamma-rays.

https://apod.nasa.gov/apod/ap240823.html

#space #nebula #pulsar #astrophotography #photography #science #astronomy #physics #nature #NASA

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2024 August 23 Supernova Remnant CTA 1 * Image Credit & Copyright: Thomas Lelu Explanation: There is a quiet pulsar at the heart of CTA 1. The supernova remnant was discovered as a source of emission at radio wavelengths by astronomers in 1960 and since identified as the result of the death explosion of a massive star. But no radio pulses were detected from the expected pulsar, the rotating neutron star remnant of the massive star's collapsed core. Seen about 10,000 years after the initial supernova explosion, the interstellar debris cloud is faint at optical wavelengths. CTA 1's visible wavelength emission from still expanding shock fronts is revealed in this deep telescopic image, a frame that spans about 2 degrees across a starfield in the northern constellation of Cepheus. While no pulsar has since been found at radio wavelengths, in 2008 the Fermi Gamma-ray Space Telescope detected pulsed emission from CTA 1, identifying the supernova remnant's rotating neutron star. The source has been recognized as the first in a growing class of pulsars that are quiet at radio wavelengths but pulse in high-energy gamma-rays. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility Notices A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

2024 April 16

Filaments of the Vela Supernova Remnant
* Image Credit: CTIO, NOIRLab, DOE, NSF, AURA
https://noirlab.edu/public/programs/ctio/
https://noirlab.edu/
https://www.energy.gov/
https://www.nsf.gov/
https://www.aura-astronomy.org/
* Processing: T. A. Rector (U. Alaska Anchorage), M. Zamani & D. de Martin (’s NOIRLab)
http://aftar.uaa.alaska.edu/
https://www.uaa.alaska.edu/
https://mahdizamani.com/about
https://noirlab.edu/

Explanation:
The explosion is over, but the consequences continue. About eleven thousand years ago, a star in the constellation of Vela could be seen to explode, creating a strange point of light briefly visible to humans living near the beginning of recorded history. The outer layers of the star crashed into the interstellar medium, driving a shock wave that is still visible today. The featured image captures some of that filamentary and gigantic shock in visible light. As gas flies away from the detonated star, it decays and reacts with the interstellar medium, producing light in many different colors and energy bands. Remaining at the center of the Vela Supernova Remnant is a pulsar, a star as dense as nuclear matter that spins around more than ten times in a single second.

https://apod.nasa.gov/apod/ap240416.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA

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2024 April 16 Complex filaments of many colors cross the image in front of a starry background. Some regions have a diffuse red or orange glow. Filaments of the Vela Supernova Remnant * Image Credit: CTIO, NOIRLab, DOE, NSF, AURA * Processing: T. A. Rector (U. Alaska Anchorage), M. Zamani & D. de Martin (’s NOIRLab) Explanation: The explosion is over, but the consequences continue. About eleven thousand years ago, a star in the constellation of Vela could be seen to explode, creating a strange point of light briefly visible to humans living near the beginning of recorded history. The outer layers of the star crashed into the interstellar medium, driving a shock wave that is still visible today. The featured image captures some of that filamentary and gigantic shock in visible light. As gas flies away from the detonated star, it decays and reacts with the interstellar medium, producing light in many different colors and energy bands. Remaining at the center of the Vela Supernova Remnant is a pulsar, a star as dense as nuclear matter that spins around more than ten times in a single second. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

2025 August 31

NGC 7027: The Pillow Planetary Nebula
* Image Credit: NASA, ESA, Hubble
http://www.nasa.gov/
https://www.esa.int/
https://science.nasa.gov/mission/hubble/overview/about-hubble/
* Processing: Delio Tolivia Cadrecha
https://www.instagram.com/deliotolivia/

Explanation:
What created this unusual planetary nebula? Dubbed the Pillow Nebula and the Flying Carpet Nebula, NGC 7027 is one of the smallest, brightest, and most unusually shaped planetary nebulas known. Given its expansion rate, NGC 7027 first started expanding, as visible from Earth, about 600 years ago. For much of its history, the planetary nebula has been expelling shells, as seen in blue in the featured image by the Hubble Space Telescope. In modern times, though, for reasons unknown, it began ejecting gas and dust (seen in brown) in specific directions that created a new pattern that seems to have four corners. What lies at the nebula's center is unknown, with one hypothesis holding it to be a close binary star system where one star sheds gas onto an erratic disk orbiting the other star. NGC 7027, about 3,000 light years away, was first discovered in 1878 and can be seen with a standard backyard telescope toward the constellation of the Swan (Cygnus).

https://apod.nasa.gov/apod/ap250831.html

#space #nebula #astrophotography #photography #science #astronomy #physics #nature #NASA #ESA

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2025 August 31 A starfield surrounds a bright nebula. The nebula is somewhat rectangular like a pillow and is mostly white with brown filaments inside and blue shells surrounding. NGC 7027: The Pillow Planetary Nebula * Image Credit: NASA, ESA, Hubble; Processing: Delio Tolivia Cadrecha Explanation: What created this unusual planetary nebula? Dubbed the Pillow Nebula and the Flying Carpet Nebula, NGC 7027 is one of the smallest, brightest, and most unusually shaped planetary nebulas known. Given its expansion rate, NGC 7027 first started expanding, as visible from Earth, about 600 years ago. For much of its history, the planetary nebula has been expelling shells, as seen in blue in the featured image by the Hubble Space Telescope. In modern times, though, for reasons unknown, it began ejecting gas and dust (seen in brown) in specific directions that created a new pattern that seems to have four corners. What lies at the nebula's center is unknown, with one hypothesis holding it to be a close binary star system where one star sheds gas onto an erratic disk orbiting the other star. NGC 7027, about 3,000 light years away, was first discovered in 1878 and can be seen with a standard backyard telescope toward the constellation of the Swan (Cygnus). Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation

2025 November 5

Spiral Galaxy NGC 3370 from Hubble
* Image Credit: ESA/Hubble & NASA, A. Riess, K. Noll
https://esahubble.org/
https://www.nasa.gov/
https://physics-astronomy.jhu.edu/directory/adam-riess/
https://science.gsfc.nasa.gov/sci/bio/keith.s.noll

Explanation:
Is this what our own Milky Way Galaxy looks like from far away? Similar in size and grand design to our home Galaxy (although without the central bar), spiral galaxy NGC 3370 lies about 100 million light-years away toward the constellation of the Lion (Leo). Recorded here in exquisite detail by the Hubble Space Telescope, the big, beautiful face-on spiral is not only photogenic, but has proven sharp enough to study individual stars known as Cepheids. These pulsating stars have been used to accurately determine NGC 3370's distance. NGC 3370 was chosen for this study because in 1994 the spiral galaxy was also home to a well studied stellar explosion -- a Type Ia supernova. Combining the known distance to this standard candle supernova, based on the Cepheid measurements, with observations of supernovas at even greater distances has helped to reveal the size and expansion rate of the entire Universe itself.
https://esahubble.org/images/potw2542a/
https://en.wikipedia.org/wiki/NGC_3370
https://esahubble.org/videos/potw2542a/
https://cas.sdss.org/dr6/en/proj/basic/galaxies/spirals.asp
https://en.wikipedia.org/wiki/Cepheid_variable
http://www.ianridpath.com/startales/leo.html
https://www.pbs.org/wgbh/nova/universe/supernova1a_nf_01.html
https://www.starstryder.com/2007/10/03/type-1a-supernoave-a-non-standard-candle/
https://apod.nasa.gov/debate/debate96.html

https://apod.nasa.gov/apod/ap251105.html

#space #galaxy #astrophotography #photography #science #astronomy #nature #NASA #ESA #apod

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2025 November 5 A spiral galaxy covers the right part of the image. Brown dust and blue stars trace the spiral arms. On the left part of the image are several more red galaxies far in the distance. Spiral Galaxy NGC 3370 from Hubble * Image Credit: ESA/Hubble & NASA, A. Riess, K. Noll Explanation: Is this what our own Milky Way Galaxy looks like from far away? Similar in size and grand design to our home Galaxy (although without the central bar), spiral galaxy NGC 3370 lies about 100 million light-years away toward the constellation of the Lion (Leo). Recorded here in exquisite detail by the Hubble Space Telescope, the big, beautiful face-on spiral is not only photogenic, but has proven sharp enough to study individual stars known as Cepheids. These pulsating stars have been used to accurately determine NGC 3370's distance. NGC 3370 was chosen for this study because in 1994 the spiral galaxy was also home to a well studied stellar explosion -- a Type Ia supernova. Combining the known distance to this standard candle supernova, based on the Cepheid measurements, with observations of supernovas at even greater distances has helped to reveal the size and expansion rate of the entire Universe itself. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

TOPIC> Face On

Facing NGC 3344
* Image Credit: ESA/Hubble & NASA
http://www.esa.int/
https://www.spacetelescope.org/
httpshttps://apod.nasa.gov/apod/ap250624.html://www.nasa.gov/

Explanation:
From our vantage point in the Milky Way Galaxy, we see NGC 3344 face-on. Nearly 40,000 light-years across, the big, beautiful spiral galaxy is located just 20 million light-years away in the constellation of Leo Minor. This multi-color Hubble Space Telescope close-up of NGC 3344 includes remarkable details from near infrared to ultraviolet wavelengths. The frame extends some 15,000 light-years across the spiral's central regions. From the core outward, the galaxy's colors change from the yellowish light of old stars in the center to young blue star clusters and reddish star forming regions along the loose, fragmented spiral arms. Of course, the bright stars with a spiky appearance are in front of NGC 3344 and lie well within our own Milky Way.
https://esahubble.org/images/heic1803a/
https://apod.nasa.gov/apod/ap250513.html
https://science.nasa.gov/mission/hubble/overview/hubbles-35th-anniversary/

https://esahubble.org/images/heic1803a/

#space #galaxy #astrophotography #photography #science #nature #NASA

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2025 June 8 Grand spiral galaxy NGC 3344 is shown. Spiral arms with stars, star clusters, and nebula are visible. Facing NGC 3344 * Image Credit: ESA/Hubble & NASA Explanation: From our vantage point in the Milky Way Galaxy, we see NGC 3344 face-on. Nearly 40,000 light-years across, the big, beautiful spiral galaxy is located just 20 million light-years away in the constellation of Leo Minor. This multi-color Hubble Space Telescope close-up of NGC 3344 includes remarkable details from near infrared to ultraviolet wavelengths. The frame extends some 15,000 light-years across the spiral's central regions. From the core outward, the galaxy's colors change from the yellowish light of old stars in the center to young blue star clusters and reddish star forming regions along the loose, fragmented spiral arms. Of course, the bright stars with a spiky appearance are in front of NGC 3344 and lie well within our own Milky Way. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

2025 June 24

In the Center of Spiral Galaxy M61
* Image Credit: NASA, ESA, Hubble, ESO
https://www.eso.org/public/about-eso/
https://science.nasa.gov/mission/hubble/overview/about-hubble/
https://www.esa.int/
https://www.nasa.gov/;
* Processing & Copyright: Robert Gendler
http://www.robgendlerastropics.com/Biography2.html

Explanation:
Is there a spiral galaxy in the center of this spiral galaxy? Sort of. Image data from the Hubble Space Telescope, the European Southern Observatory, and smaller telescopes on planet Earth are combined in this detailed portrait of face-on spiral galaxy Messier 61 (M61) and its bright center. A mere 55 million light-years away in the Virgo Cluster of Galaxies, M61 is also known as NGC 4303. It's considered to be an example of a barred spiral galaxy similar to our own Milky Way. Like other spiral galaxies, M61 also features sweeping spiral arms, cosmic dust lanes, pinkish star forming regions, and young blue star clusters. Its core houses an active supermassive black hole surrounded by a bright nuclear spiral -- infalling star-forming gas that itself looks like a separate spiral galaxy.
https://esahubble.org/images/potw1324a/
http://www.robgendlerastropics.com/M61-HST-ESO-New.html
https://en.wikipedia.org/wiki/Messier_61

https://apod.nasa.gov/apod/ap100529.html
https://ui.adsabs.harvard.edu/abs/2000ApJ...528..677E/abstract

https://apod.nasa.gov/apod/ap250624.html

#space #galaxy #astrophotography #photography #science #astronomy #nature #NASA

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2025 June 24 A sprawling spiral galaxy is shown in great detail. This galaxy has blue spiral arms and a bright center that itself seems to look like a spiral galaxy. In the Center of Spiral Galaxy M61 * Image Credit: NASA, ESA, Hubble, ESO; Processing & Copyright: Robert Gendler Explanation: Is there a spiral galaxy in the center of this spiral galaxy? Sort of. Image data from the Hubble Space Telescope, the European Southern Observatory, and smaller telescopes on planet Earth are combined in this detailed portrait of face-on spiral galaxy Messier 61 (M61) and its bright center. A mere 55 million light-years away in the Virgo Cluster of Galaxies, M61 is also known as NGC 4303. It's considered to be an example of a barred spiral galaxy similar to our own Milky Way. Like other spiral galaxies, M61 also features sweeping spiral arms, cosmic dust lanes, pinkish star forming regions, and young blue star clusters. Its core houses an active supermassive black hole surrounded by a bright nuclear spiral -- infalling star-forming gas that itself looks like a separate spiral galaxy. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

2025 June 27

Messier 109
* Image Credit & Copyright: Robert Eder
https://app.astrobin.com/u/Robsi#gallery

Explanation:
Big beautiful barred spiral galaxy Messier 109 is the 109th entry in Charles Messier's famous catalog of bright Nebulae and Star Clusters. You can find it just below the Big Dipper's bowl in the northern constellation Ursa Major. In fact, bright dipper star Phecda, Gamma Ursa Majoris, produces the glare at the upper right corner of this telescopic frame. M109's prominent central bar gives the galaxy the appearance of the Greek letter "theta", θ, a common mathematical symbol representing an angle. M109 spans a very small angle in planet Earth's sky though, about 7 arcminutes or 0.12 degrees. But that small angle corresponds to an enormous 120,000 light-year diameter at the galaxy's estimated 60 million light-year distance. The brightest member of the now recognized Ursa Major galaxy cluster, M109 (aka NGC 3992) is joined by spiky foreground stars. Three small, fuzzy bluish galaxies also on the scene, identified (top to bottom) as UGC 6969, UGC 6940 and UGC 6923, are possibly satellite galaxies of the larger barred spiral galaxy Messier 109.
https://app.astrobin.com/u/Robsi?i=albk8c#gallery
https://science.nasa.gov/mission/hubble/science/explore-the-night-sky/hubble-messier-catalog/messier-109/

https://apod.nasa.gov/apod/ap110624.html
https://apod.nasa.gov/apod/ap121013.html

http://www.messier.seds.org/xtra/history/m-cat.html

https://chandra.harvard.edu/photo/scale_distance.html
https://chandra.harvard.edu/photo/scale.html
https://arxiv.org/abs/astro-ph/9608124

https://apod.nasa.gov/apod/ap250627.html

#space #galaxy #astrophotography #photography #science #nature #NASA

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2025 June 27 Messier 109 * Image Credit & Copyright: Robert Eder Explanation: Big beautiful barred spiral galaxy Messier 109 is the 109th entry in Charles Messier's famous catalog of bright Nebulae and Star Clusters. You can find it just below the Big Dipper's bowl in the northern constellation Ursa Major. In fact, bright dipper star Phecda, Gamma Ursa Majoris, produces the glare at the upper right corner of this telescopic frame. M109's prominent central bar gives the galaxy the appearance of the Greek letter "theta", θ, a common mathematical symbol representing an angle. M109 spans a very small angle in planet Earth's sky though, about 7 arcminutes or 0.12 degrees. But that small angle corresponds to an enormous 120,000 light-year diameter at the galaxy's estimated 60 million light-year distance. The brightest member of the now recognized Ursa Major galaxy cluster, M109 (aka NGC 3992) is joined by spiky foreground stars. Three small, fuzzy bluish galaxies also on the scene, identified (top to bottom) as UGC 6969, UGC 6940 and UGC 6923, are possibly satellite galaxies of the larger barred spiral galaxy Messier 109. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

2025 June 30

NGC 4651: The Umbrella Galaxy
* Image Credit: Rabeea Alkuwari & Anas Almajed
https://www.instagram.com/bolahdan/
https://www.instagram.com/anas_almajed/

Explanation:
It's raining stars. What appears to be a giant cosmic umbrella is now known to be a tidal stream of stars stripped from a small satellite galaxy. The main galaxy, spiral galaxy NGC 4651, is about the size of our Milky Way, while its stellar parasol appears to extend some 100 thousand light-years above this galaxy's bright disk. A small galaxy was likely torn apart by repeated encounters as it swept back and forth on eccentric orbits through NGC 4651. The remaining stars will surely fall back and become part of a combined larger galaxy over the next few million years. The featured deep image was captured in long exposures from Saudi Arabia. The Umbrella Galaxy lies about 50 million light-years distant toward the well-groomed northern constellation of Berenice's Hair (Coma Berenices).
https://www.instagram.com/anas_almajed/https://www.instagram.com/anas_almajed/
https://en.wikipedia.org/wiki/NGC_4651

https://en.wikipedia.org/wiki/Satellite_galaxy
https://en.wikipedia.org/wiki/Orbital_eccentricity#/media/File:Animation_of_Orbital_eccentricity.gif

https://apod.nasa.gov/apod/ap130514.html
https://apod.nasa.gov/apod/ap120604.html

https://apod.nasa.gov/apod/ap250630.html

#space #galaxy #astrophotography #photography #science #astronomy #nature #NASA

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2025 June 30 A spiral galaxy is shown with an unusual feature. Faint wisps of stars are seen both above and below the galaxy. A wisp above appears like an umbrella. NGC 4651: The Umbrella Galaxy * Image Credit: Rabeea Alkuwari & Anas Almajed Explanation: It's raining stars. What appears to be a giant cosmic umbrella is now known to be a tidal stream of stars stripped from a small satellite galaxy. The main galaxy, spiral galaxy NGC 4651, is about the size of our Milky Way, while its stellar parasol appears to extend some 100 thousand light-years above this galaxy's bright disk. A small galaxy was likely torn apart by repeated encounters as it swept back and forth on eccentric orbits through NGC 4651. The remaining stars will surely fall back and become part of a combined larger galaxy over the next few million years. The featured deep image was captured in long exposures from Saudi Arabia. The Umbrella Galaxy lies about 50 million light-years distant toward the well-groomed northern constellation of Berenice's Hair (Coma Berenices). Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

Short "Offtopic" Explanation

2013 May 14
Galaxy Collisions: Simulation vs Observations

* Images Credit: NASA, ESA
http://www.esa.int/
http://www.nasa.gov/;
* Visualization: Frank Summers (STScI)
http://www.stsci.edu/;
* Simulation: Chris Mihos (CWRU) & Lars Hernquist (Harvard)
https://astronomy.case.edu/ .

Explanation:
What happens when two galaxies collide? Although it may take over a billion years, such titanic clashes are quite common. Since galaxies are mostly empty space, no internal stars are likely to themselves collide. Rather the gravitation of each galaxy will distort or destroy the other galaxy, and the galaxies may eventually merge to form a single larger galaxy. Expansive gas and dust clouds collide and trigger waves of star formation that complete even during the interaction process. Pictured above is a computer simulation of two large spiral galaxies colliding, interspersed with real still images taken by the Hubble Space Telescope. Our own Milky Way Galaxy has absorbed several smaller galaxies during its existence and is even projected to merge with the larger neighboring Andromeda galaxy in a few billion years.

https://apod.nasa.gov/apod/ap130514.html

#space #galaxy #astrophotography #photography #science #astronomy #nature #NASA

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2013 May 14 Galaxy Collisions: Simulation vs Observations * Images Credit: NASA, ESA; * Visualization: Frank Summers (STScI); * Simulation: Chris Mihos (CWRU) & Lars Hernquist (Harvard). Explanation: What happens when two galaxies collide? Although it may take over a billion years, such titanic clashes are quite common. Since galaxies are mostly empty space, no internal stars are likely to themselves collide. Rather the gravitation of each galaxy will distort or destroy the other galaxy, and the galaxies may eventually merge to form a single larger galaxy. Expansive gas and dust clouds collide and trigger waves of star formation that complete even during the interaction process. Pictured above is a computer simulation of two large spiral galaxies colliding, interspersed with real still images taken by the Hubble Space Telescope. Our own Milky Way Galaxy has absorbed several smaller galaxies during its existence and is even projected to merge with the larger neighboring Andromeda galaxy in a few billion years. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Phillip Newman Specific rights apply. NASA Web Privacy Policy and Important Notices A service of: ASD at NASA / GSFC & Michigan Tech. U.

2025 July 4

NGC 6946 and NGC 6939
* Image Credit & Copyright: Alberto Pisabarro
https://www.loscoloresinvisibles.com/

Explanation:
Face-on spiral galaxy NGC 6946 and open star cluster NGC 6939 share this cosmic snapshot, composed with over 68 hours of image data captured with a small telescope on planet Earth. The field of view spans spans about 1 degree or 2 full moons on the sky toward the northern constellation Cepheus. Seen through faint interstellar dust couds near the plane of our Milky Way galaxy, the stars of open cluster NGC 6939 are 5,600 light-years in the distance, near bottom right in the frame. Face-on spiral galaxy NGC 6946 is at top left, but lies some 22 million light-years away. In the last 100 years, 10 supernovae have been discovered in NGC 6946, the latest one seen in 2017. By comparison, the average rate of supernovae in our Milky Way is about 1 every 100 years or so. Of course, NGC 6946 is also known as The Fireworks Galaxy.
https://www.loscoloresinvisibles.com/null
https://ui.adsabs.harvard.edu/abs/2022AJ....163..191K/abstract

Location:
http://www.hawastsoc.org/deepsky/cep/

Super Novae of NGC 6946:
https://rochesterastronomy.org/sn2017/sn2017eaw.html
https://skyandtelescope.org/astronomy-news/observing-news/possible-bright-supernova-discovered-in-fireworks-galaxy-ngc-6946/

nasa.gov/apod/ap250704.html

#space #galaxy #astrophotography #photography #science #nature #NASA

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2025 July 4 NGC 6946 and NGC 6939 * Image Credit & Copyright: Alberto Pisabarro Explanation: Face-on spiral galaxy NGC 6946 and open star cluster NGC 6939 share this cosmic snapshot, composed with over 68 hours of image data captured with a small telescope on planet Earth. The field of view spans spans about 1 degree or 2 full moons on the sky toward the northern constellation Cepheus. Seen through faint interstellar dust couds near the plane of our Milky Way galaxy, the stars of open cluster NGC 6939 are 5,600 light-years in the distance, near bottom right in the frame. Face-on spiral galaxy NGC 6946 is at top left, but lies some 22 million light-years away. In the last 100 years, 10 supernovae have been discovered in NGC 6946, the latest one seen in 2017. By comparison, the average rate of supernovae in our Milky Way is about 1 every 100 years or so. Of course, NGC 6946 is also known as The Fireworks Galaxy. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy, Accessibility, Notices; A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

NGC 6946: The ‘Fireworks Galaxy’

NGC 6946 is a medium-sized, face-on spiral galaxy about 22 million light years away from Earth. In the past century, eight supernovas have been observed to explode in the arms of this galaxy. Chandra observations (purple) have, in fact, revealed three of the oldest supernovas ever detected in X-rays, giving more credence to its nickname of the “Fireworks Galaxy.” This composite image also includes optical data from the Gemini Observatory in red, yellow, and cyan.

Image credit: X-ray: NASA/CXC/MSSL/R.Soria et al, Optical: AURA/Gemini OBs

#space #galaxy #astrophotography #photography #science #nature #NASA

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NGC 6946, or "the Fireworks Galaxy," is a medium-sized, face-on spiral galaxy about 22 million light years away from Earth.

A Mysterious Rash of Star Birth

"A Mysterious Rash of Star Birth In this crisp Gemini North image, pink bubbles of glowing hydrogen gas spread across the arms of the face-on spiral galaxy NGC 6946 like a rash. This amazing infusion of color is fueled by the ubiquitous birth of massive stars throughout NGC 6946; these hot young stars blast copious amounts of ultraviolet radiation into their natal shrouds of hydrogen gas, causing the clouds to glow red. For reasons unknown, NGC 6946 has a much higher rate of star formation than all of the other large galaxies in our local neighborhood. The prodigious output of stellar nurseries in this extragalactic neighbor — which lies about 20 million light years away in the direction of the constellation of Cepheus — eventually leads to accelerated numbers of supernovae explosions. NGC 6946’s supernovae have occurred in rapid-fire fashion for tens of millions of years. Over the past century, eight supernovae are known to have exploded in the arms of this stellar metropolis. NGC 6946 is, in fact, the most prolific known galaxy for supernovae during the past 100 years. These events have led to its popular nickname, the “Fireworks Galaxy.” If we could compress just a million years of NGC 6946’s history into a time-lapse movie, lasting but a few seconds, we would bear witness to a stream of nearly constant outbursts of light as new stars flare into view, while old ones expire in spectacular explosions." Technical Details: Acquisition Date(s): August 12, 2004 Telescope: Gemini North, Mauna Kea Hawai'i Instrument: GMOS (Gemini Multi-Object Spectrograph) Field of View: 5.80 x 5.58 arcminutes Orientation: Image is rotated CCW by 184 degrees from North = up, East = left
https://www.gemini.edu/news/press-releases/gemini0501

* Credits:
International Gemini Observatory/AURA/Manuel Paredes

https://www.gemini.edu/gallery/images/gemini0501a/

#space #galaxy #astrophotography #photography #science #nature #NASA

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"A Mysterious Rash of Star Birth In this crisp Gemini North image, pink bubbles of glowing hydrogen gas spread across the arms of the face-on spiral galaxy NGC 6946 like a rash. This amazing infusion of color is fueled by the ubiquitous birth of massive stars throughout NGC 6946; these hot young stars blast copious amounts of ultraviolet radiation into their natal shrouds of hydrogen gas, causing the clouds to glow red. For reasons unknown, NGC 6946 has a much higher rate of star formation than all of the other large galaxies in our local neighborhood. The prodigious output of stellar nurseries in this extragalactic neighbor — which lies about 20 million light years away in the direction of the constellation of Cepheus — eventually leads to accelerated numbers of supernovae explosions. NGC 6946’s supernovae have occurred in rapid-fire fashion for tens of millions of years. Over the past century, eight supernovae are known to have exploded in the arms of this stellar metropolis. NGC 6946 is, in fact, the most prolific known galaxy for supernovae during the past 100 years. These events have led to its popular nickname, the “Fireworks Galaxy.” If we could compress just a million years of NGC 6946’s history into a time-lapse movie, lasting but a few seconds, we would bear witness to a stream of nearly constant outbursts of light as new stars flare into view, while old ones expire in spectacular explosions." * Credits: International Gemini Observatory/AURA/Manuel Paredes

2025 April 26

Barred Spiral Galaxy NGC 5335
* Image Credit: NASA, ESA, STScI
https://www.nasa.gov/
https://www.stsci.edu/home
https://esahubble.org/

Explanation:
This stunning portrait of NGC 5335 was captured by the Hubble Space Telescope. Some 170,000 light-years across and over 200 million light-years away toward the constellation Virgo, the magnificent spiral galaxy is seen face-on in Hubble's view. Within the galactic disk, loose streamers of star forming regions lie along the galaxy's flocculent spiral arms. But the most striking feature of NGC 5335 is its prominent central bar. Seen in about 30 percent of galaxies, including our Milky Way, bar structures are understood to channel material inward toward the galactic center, fueling star formation. Of course, distant background galaxies are easy to spot, scattered around the sharp Hubble image. Launched in 1990, Hubble is now celebrating its 35th year exploring the cosmos from orbit around planet Earth.
https://science.nasa.gov/asset/hubble/ngc-5335/

https://apod.nasa.gov/apod/ap250426.html

#space #galaxy #astrophotography #photography #science #astronomy #nature #NASA

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2025 April 26 Barred Spiral Galaxy NGC 5335 * Image Credit: NASA, ESA, STScI Explanation: This stunning portrait of NGC 5335 was captured by the Hubble Space Telescope. Some 170,000 light-years across and over 200 million light-years away toward the constellation Virgo, the magnificent spiral galaxy is seen face-on in Hubble's view. Within the galactic disk, loose streamers of star forming regions lie along the galaxy's flocculent spiral arms. But the most striking feature of NGC 5335 is its prominent central bar. Seen in about 30 percent of galaxies, including our Milky Way, bar structures are understood to channel material inward toward the galactic center, fueling star formation. Of course, distant background galaxies are easy to spot, scattered around the sharp Hubble image. Launched in 1990, Hubble is now celebrating its 35th year exploring the cosmos from orbit around planet Earth. Authors & editors: Robert Nemiroff (MTU) & Jerry Bonnell (UMCP) NASA Official: Amber Straughn Specific rights apply. NASA Web Privacy Policy and Important Notices A service of: ASD at NASA / GSFC, NASA Science Activation & Michigan Tech. U.

January 10, 2005

Barred Spiral Galaxy NGC 1300 - NASA Science

One of the largest Hubble Space Telescope images ever made of a complete galaxy is being unveiled today at the American Astronomical Society meeting in San Diego, Calif.

The Hubble telescope captured a display of starlight, glowing gas, and silhouetted dark clouds of interstellar dust in this 4-foot-by-8-foot image of the barred spiral galaxy NGC 1300. NGC 1300 is considered to be prototypical of barred spiral galaxies. Barred spirals differ from normal spiral galaxies in that the arms of the galaxy do not spiral all the way into the center, but are connected to the two ends of a straight bar of stars containing the nucleus at its center.

At Hubble's resolution, a myriad of fine details, some of which have never before been seen, is seen throughout the galaxy's arms, disk, bulge, and nucleus. Blue and red supergiant stars, star clusters, and star-forming regions are well resolved across the spiral arms, and dust lanes trace out fine structures in the disk and bar. Numerous more distant galaxies are visible in the background, and are seen even through the densest regions of NGC 1300.

In the core of the larger spiral structure of NGC 1300, the nucleus shows its own extraordinary and distinct "grand-design" spiral structure that is about 3,300 light-years (1 kiloparsec) long. Only galaxies with large-scale bars appear to have these grand-design inner disks - a spiral within a spiral. Models suggest that the gas in a bar can be funneled inwards, and then spiral into the center through the grand-design disk, where it can potentially fuel a central black hole. NGC 1300 is not known to have an active nucleus, however, indicating either that there is no black hole, or that it is not accreting matter.

https://science.nasa.gov/asset/hubble/barred-spiral-galaxy-ngc-1300/

#space #galaxy #astrophotography #photography #science #astronomy #nature #NASA

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One of the largest Hubble Space Telescope images ever made of a complete galaxy is being unveiled today at the American Astronomical Society meeting in San Diego, Calif. The Hubble telescope captured a display of starlight, glowing gas, and silhouetted dark clouds of interstellar dust in this 4-foot-by-8-foot image of the barred spiral galaxy NGC 1300. NGC 1300 is considered to be prototypical of barred spiral galaxies. Barred spirals differ from normal spiral galaxies in that the arms of the galaxy do not spiral all the way into the center, but are connected to the two ends of a straight bar of stars containing the nucleus at its center. The image was constructed from exposures taken in September 2004 by the Advanced Camera for Surveys onboard Hubble in four filters. Starlight and dust are seen in blue, visible, and infrared light. Bright star clusters are highlighted in red by their associated emission from glowing hydrogen gas. Due to the galaxy's large size, two adjacent pointings of the telescope were necessary to cover the extent of the spiral arms. The galaxy lies roughly 69 million light-years away (21 megaparsecs) in the direction of the constellation Eridanus. Credit: The Hubble image was created from HST data from proposal 10342: K. Noll, H. Bond, C. Christian, L. Frattare, F. Hamilton, W. Januszewski, Z. Levay, and T. Royle (STScI), and P. Knezek (WIYN).

A zoom into the center of NGC 1300 that reveals the fine details captured by Hubble's Advanced Camera for Surveys across the spiral arms, and dust lanes in the disk and bar.

Credit:
NASA, ESA, and G. Bacon (STScI); Acknowledgment: NASA, ESA, A. Fujii, Digitized Sky Survey (DSS), STScI/AURA, Palomar/Caltech, and UKSTU/AAO, and the Hubble Heritage Team (STScI/AURA)

#space #galaxy #astrophotography #photography #science #astronomy #nature #NASA