1. Animation of a Supernova Explosion
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This artist's animation shows the basics of a supernova explosion like the one that created Cas A. When a massive star runs out of fuel, it collapses onto itself and its remains are then expelled into the surrounding space. This expanding debris field is very hot and thus glows brightly in X-rays, which are detected by telescopes like Chandra. At the end of the animation, the view dissolves into an image of Cas A created from Chandra data.
[Runtime: 00:26]
(NASA/CXC/A.Hobart)
Related Chandra Images:
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This artist's animation shows the basics of a supernova explosion like the one that created Cas A. When a massive star runs out of fuel, it collapses onto itself and its remains are then expelled into the surrounding space. This expanding debris field is very hot and thus glows brightly in X-rays, which are detected by telescopes like Chandra. At the end of the animation, the view dissolves into an image of Cas A created from Chandra data.
[Runtime: 00:26]
(NASA/CXC/A.Hobart)
Related Chandra Images:
- Photo Album: Cassiopeia A
- Photo Album: Cassiopeia A
2. Brief Time-lapse Movie of Cassiopeia A
QuicktimeMPEG This brief movie of X-ray data from Chandra of Cas A was made by combining observations taken in January 2000, February 2002, February 2004, and December 2007. In these images, the lowest-energy X-rays Chandra detects are shown in red, intermediate energies in green, and the highest energies in blue. Scientists have used the movie to measure the expansion velocity of the leading edge of the explosion's outer blast wave (shown in blue). The researchers find that the velocity is 11 million miles per hour, which is significantly slower than expected for an explosion with the energy estimated to have been released in Cas A.
[Runtime: 00:20]
(NASA/CXC/SAO/D.Patnaude et al.)
Related Chandra Images:
QuicktimeMPEG This brief movie of X-ray data from Chandra of Cas A was made by combining observations taken in January 2000, February 2002, February 2004, and December 2007. In these images, the lowest-energy X-rays Chandra detects are shown in red, intermediate energies in green, and the highest energies in blue. Scientists have used the movie to measure the expansion velocity of the leading edge of the explosion's outer blast wave (shown in blue). The researchers find that the velocity is 11 million miles per hour, which is significantly slower than expected for an explosion with the energy estimated to have been released in Cas A.
[Runtime: 00:20]
(NASA/CXC/SAO/D.Patnaude et al.)
Related Chandra Images:
- Photo Album: Cassiopeia A
3. Movie of Chandra Images Evolving Over Time
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This movie has been created from a series of X-ray observations from Chandra of Cassiopeia A (Cas A) over eight years. It begins with a full-field view of Cas A, cycling through the movie several times. The camera then zooms into three different areas of Cas A where evolution of different features can been seen. This movie - the first of its kind for a supernova remnant - reveals new details about the supernova explosion and its remnant seen today.
[Runtime: 2:00]
(NASA/CXC/SAO/D.Patnaude et al.)
Related Chandra Images:
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This movie has been created from a series of X-ray observations from Chandra of Cassiopeia A (Cas A) over eight years. It begins with a full-field view of Cas A, cycling through the movie several times. The camera then zooms into three different areas of Cas A where evolution of different features can been seen. This movie - the first of its kind for a supernova remnant - reveals new details about the supernova explosion and its remnant seen today.
[Runtime: 2:00]
(NASA/CXC/SAO/D.Patnaude et al.)
Related Chandra Images:
- Photo Album: Cassiopeia A
4. Tour of G292.01+8
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By mapping the distribution of X-rays in different energy bands, astronomers can trace the distribution of chemical elements ejected in the supernova. The results imply that the explosion was not symmetrical. For example, silicon and sulfur, which are colored blue in this image, and magnesium, which is green, are seen strongly in the upper right. On the other hand, oxygen, which appears as yellow and orange, dominates the lower left. Studying the details of this X-ray image allows astronomers to better understand how some stars die and disperse important elements like oxygen into the next generation of stars and planets.
[Runtime: 1:11]
(X-ray: NASA/CXC/Penn State/S.Park et al.; Optical: Pal.Obs. DSS)
Related Chandra Images:
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- Audio (960.2 kb)
By mapping the distribution of X-rays in different energy bands, astronomers can trace the distribution of chemical elements ejected in the supernova. The results imply that the explosion was not symmetrical. For example, silicon and sulfur, which are colored blue in this image, and magnesium, which is green, are seen strongly in the upper right. On the other hand, oxygen, which appears as yellow and orange, dominates the lower left. Studying the details of this X-ray image allows astronomers to better understand how some stars die and disperse important elements like oxygen into the next generation of stars and planets.
[Runtime: 1:11]
(X-ray: NASA/CXC/Penn State/S.Park et al.; Optical: Pal.Obs. DSS)
Related Chandra Images:
- Photo Album: G292.0+1.8
5. Tour of SN1996cr
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[Runtime: 0.50]
(X-ray (NASA/CXC/Columbia/F.Bauer et al); Optical (NASA/STScI/UMD/A.Wilson et al.))
Related Chandra Images:
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- Audio (673.3 kb)
[Runtime: 0.50]
(X-ray (NASA/CXC/Columbia/F.Bauer et al); Optical (NASA/STScI/UMD/A.Wilson et al.))
Related Chandra Images:
- Photo Album: SN 1996cr
6. Tour of SN 1006
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[Runtime: 0.45]
(Credit: X-ray: NASA/CXC/Rutgers/G.Cassam-Chenaļ, J.Hughes et al.; Radio: NRAO/AUI/NSF/GBT/VLA/Dyer, Maddalena & Cornwell; Optical: Middlebury College/F.Winkler, NOAO/AURA/NSF/CTIO Schmidt & DSS)
Related Chandra Images:
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- Audio (613 kb)
[Runtime: 0.45]
(Credit: X-ray: NASA/CXC/Rutgers/G.Cassam-Chenaļ, J.Hughes et al.; Radio: NRAO/AUI/NSF/GBT/VLA/Dyer, Maddalena & Cornwell; Optical: Middlebury College/F.Winkler, NOAO/AURA/NSF/CTIO Schmidt & DSS)
Related Chandra Images:
- Photo Album: SN 1006
7. Tour of G1.9+0.3
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[Runtime: 0.46]
(Credit: X-ray (NASA/CXC/NCSU/S.Reynolds et al.); Radio (NSF/NRAO/VLA/Cambridge/D.Green et al.); Infrared (2MASS/UMass/IPAC-Caltech/NASA/NSF/CfA/E.Bressert))
Related Chandra Images:
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- Audio (617.7 kb)
[Runtime: 0.46]
(Credit: X-ray (NASA/CXC/NCSU/S.Reynolds et al.); Radio (NSF/NRAO/VLA/Cambridge/D.Green et al.); Infrared (2MASS/UMass/IPAC-Caltech/NASA/NSF/CfA/E.Bressert))
Related Chandra Images:
- Photo Album: G1.9+0.3
8. Animation of G1.9+0.3
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This animation begins with a view of the Milky Way from above the plane of the galaxy, where the Galactic center and bulge is unobscured by dust and gas. The viewer then travels towards the center of the Galaxy and zooms into the bright, crowded central bulge of the Milky Way, where a supernova explosion occurs. The ejecta from the explosion rushes outwards where it interacts with the gas surrounding the explosion, causing the formation of a supernova remnant which shines brightly in X-rays and radio waves. This is the scenario scientists envision occurred with G1.9+0.3
[Runtime: 0.23]
(NASA/CXC/A. Hobart)
Related Chandra Images:
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This animation begins with a view of the Milky Way from above the plane of the galaxy, where the Galactic center and bulge is unobscured by dust and gas. The viewer then travels towards the center of the Galaxy and zooms into the bright, crowded central bulge of the Milky Way, where a supernova explosion occurs. The ejecta from the explosion rushes outwards where it interacts with the gas surrounding the explosion, causing the formation of a supernova remnant which shines brightly in X-rays and radio waves. This is the scenario scientists envision occurred with G1.9+0.3
[Runtime: 0.23]
(NASA/CXC/A. Hobart)
Related Chandra Images:
- Photo Album: G1.9+0.3
9. Comparison of X-ray and Radio Images
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In order to determine the age of G1.9+0.3, astronomers needed to track how quickly it is expanding. By comparing a radio image from 1985 to a Chandra image taken in 2007, scientists see the ring of debris expand. The expansion rate was confirmed with another radio observation with the VLA in 2008. The difference in size between these images gives clear evidence for expansion, allowing the age of the remnant and the time since the original supernova explosion (about 140 years) to be estimated.
[Runtime: 0.35]
(X-ray (NASA/CXC/NCSU/S.Reynolds et al.); Radio (NSF/NRAO/VLA/ Cambridge/D.Green et al.)
Related Chandra Images:
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In order to determine the age of G1.9+0.3, astronomers needed to track how quickly it is expanding. By comparing a radio image from 1985 to a Chandra image taken in 2007, scientists see the ring of debris expand. The expansion rate was confirmed with another radio observation with the VLA in 2008. The difference in size between these images gives clear evidence for expansion, allowing the age of the remnant and the time since the original supernova explosion (about 140 years) to be estimated.
[Runtime: 0.35]
(X-ray (NASA/CXC/NCSU/S.Reynolds et al.); Radio (NSF/NRAO/VLA/ Cambridge/D.Green et al.)
Related Chandra Images:
- Photo Album: G1.9+0.3
10. Zoom into G1.9+0.3
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Beginning with a wide-field look at the center of the Milky Way from the Two Micron All Sky Survey, the view zooms into the Galactic Center before panning about a thousand light years away to where G1.9+0.3 is located. While most optical light is blocked by thick clouds of gas and dust in this part of the Galaxy, X-ray and radio radiation can penetrate them. A combination of data from Chandra and the VLA allowed for the discovery of a recent supernova explosion that would have appeared in the night sky during the late 19th century if it was unobscured.
[Runtime: 0.35]
(X-ray (NASA/CXC/NCSU/S.Reynolds et al.); Radio (NSF/NRAO/VLA/ Cambridge/ D.Green et al.); Infrared (2MASS/UMass/IPAC-Caltech/NASA/NSF/CfA/E.Bressert)
Related Chandra Images:
QuicktimeMPEG
Beginning with a wide-field look at the center of the Milky Way from the Two Micron All Sky Survey, the view zooms into the Galactic Center before panning about a thousand light years away to where G1.9+0.3 is located. While most optical light is blocked by thick clouds of gas and dust in this part of the Galaxy, X-ray and radio radiation can penetrate them. A combination of data from Chandra and the VLA allowed for the discovery of a recent supernova explosion that would have appeared in the night sky during the late 19th century if it was unobscured.
[Runtime: 0.35]
(X-ray (NASA/CXC/NCSU/S.Reynolds et al.); Radio (NSF/NRAO/VLA/ Cambridge/ D.Green et al.); Infrared (2MASS/UMass/IPAC-Caltech/NASA/NSF/CfA/E.Bressert)
Related Chandra Images:
- Photo Album: G1.9+0.3
Revised: April 17, 2013