1. Animation of Black Hole Formation in SN 1979C
QuicktimeMPEG This animation shows how a black hole may have formed in SN 1979C. The collapse of a massive star is shown, after it has exhausted its fuel. A flash of light from a shock breaking through the surface of the star is then shown, followed by a powerful supernova explosion. The view then zooms into the center of the explosion. Red, slow-moving material in a disk is shown falling onto the white neutron star that formed when the star collapsed. The rate of infall onto the neutron star increases until the star collapses into a black hole. Matter should continue to fall into the black hole and generate bright X-ray emission for many years.
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(NASA/CXC/A.Hobart)
Related Chandra Images:
QuicktimeMPEG This animation shows how a black hole may have formed in SN 1979C. The collapse of a massive star is shown, after it has exhausted its fuel. A flash of light from a shock breaking through the surface of the star is then shown, followed by a powerful supernova explosion. The view then zooms into the center of the explosion. Red, slow-moving material in a disk is shown falling onto the white neutron star that formed when the star collapsed. The rate of infall onto the neutron star increases until the star collapses into a black hole. Matter should continue to fall into the black hole and generate bright X-ray emission for many years.
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(NASA/CXC/A.Hobart)
Related Chandra Images:
- Photo Album: SN 1979C
2. Tour of G327.1-1.1
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(X-ray: NASA/CXC/SAO/T.Temim et al. and ESA/XMM-Newton Radio: SIFA/MOST and CSIRO/ATNF/ATCA; Infrared: UMass/IPAC-Caltech/NASA/NSF/2MASS)
Related Chandra Images:
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(X-ray: NASA/CXC/SAO/T.Temim et al. and ESA/XMM-Newton Radio: SIFA/MOST and CSIRO/ATNF/ATCA; Infrared: UMass/IPAC-Caltech/NASA/NSF/2MASS)
Related Chandra Images:
- Photo Album: G327.1-1.1
3. Tour of N49
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(X-ray: (NASA/CXC/Penn State/S.Park et al.); Optical: NASA/STScI/UIUC/Y.H.Chu & R.Williams et al)
Related Chandra Images:
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(X-ray: (NASA/CXC/Penn State/S.Park et al.); Optical: NASA/STScI/UIUC/Y.H.Chu & R.Williams et al)
Related Chandra Images:
- Photo Album: N49
4. Tour of G54.1+0.3
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(X-ray: NASA/CXC/SAO/T.Temim et al.; IR: NASA/JPL-Caltech)
Related Chandra Images:
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(X-ray: NASA/CXC/SAO/T.Temim et al.; IR: NASA/JPL-Caltech)
Related Chandra Images:
- Photo Album: G54.1+0.3
5. Animation of Merger Trigger for Supernova
QuicktimeMPEG This animation shows the main way that new Chandra results indicate Type Ia supernova are triggered in elliptical galaxies. Two white dwarf stars orbit each other and lose energy via gravitational radiation, eventually resulting in a merger between the two stars. Because the total mass of this merger exceeds the weight limit for a white dwarf, the merged star is unstable and explodes as a Type Ia supernova.
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View Stills
(NASA/CXC/A.Hobart)
Related Chandra Images:
QuicktimeMPEG This animation shows the main way that new Chandra results indicate Type Ia supernova are triggered in elliptical galaxies. Two white dwarf stars orbit each other and lose energy via gravitational radiation, eventually resulting in a merger between the two stars. Because the total mass of this merger exceeds the weight limit for a white dwarf, the merged star is unstable and explodes as a Type Ia supernova.
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(NASA/CXC/A.Hobart)
Related Chandra Images:
- Photo Album: M31
6. Images of Cosmic Cannonball
QuicktimeMPEG This sequence begins with a wide-field CTIO optical image which then combines with an X-ray image from the ROSAT observatory of Puppis A, the debris field created when a massive star exploded at the end of its life. The next image from Chandra shows the close-up view of the small, dense object, known as a "neutron star", left behind after the explosion. Chandra observations from 1999 and 2005 clearly show that the neutron star has moved over a period of five years. Astronomers calculate this neutron star is traveling at about 3 million miles per hour and is destined to exit the Galaxy million of years from now.
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(Chandra: NASA/CXC/Middlebury College/F.Winkler et al.; ROSAT: NASA/GSFC/S.Snowden et al.; Optical: NOAO/AURA/NSF/Middlebury College/F.Winkler et al.)
Related Chandra Images:
QuicktimeMPEG This sequence begins with a wide-field CTIO optical image which then combines with an X-ray image from the ROSAT observatory of Puppis A, the debris field created when a massive star exploded at the end of its life. The next image from Chandra shows the close-up view of the small, dense object, known as a "neutron star", left behind after the explosion. Chandra observations from 1999 and 2005 clearly show that the neutron star has moved over a period of five years. Astronomers calculate this neutron star is traveling at about 3 million miles per hour and is destined to exit the Galaxy million of years from now.
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(Chandra: NASA/CXC/Middlebury College/F.Winkler et al.; ROSAT: NASA/GSFC/S.Snowden et al.; Optical: NOAO/AURA/NSF/Middlebury College/F.Winkler et al.)
Related Chandra Images:
- Photo Album: RX J0822-4300 in Puppis A
7. Chandra Comparison of Type Ia Supernova Remnants
QuicktimeMPEG This sequence compares the Chandra image of Kepler's SNR with the Chandra images of 3 Type Ia supernova remnants located in the Milky Way. The X-ray emission for Kepler's remnant contains a bright central region similar to DEM L238, while the X-ray emission for Tycho's remnant and SN 1006 are generally much more uniform. These results suggest that the stars that exploded and caused the Kepler and DEM L238 supernova remnants were much younger than the stars that produced the Tycho and SN 1006 remnants.
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(X-ray: NASA/CXC/NCSU/S.Reynolds et al; Optical: DSS)
Related Chandra Images:
QuicktimeMPEG This sequence compares the Chandra image of Kepler's SNR with the Chandra images of 3 Type Ia supernova remnants located in the Milky Way. The X-ray emission for Kepler's remnant contains a bright central region similar to DEM L238, while the X-ray emission for Tycho's remnant and SN 1006 are generally much more uniform. These results suggest that the stars that exploded and caused the Kepler and DEM L238 supernova remnants were much younger than the stars that produced the Tycho and SN 1006 remnants.
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(X-ray: NASA/CXC/NCSU/S.Reynolds et al; Optical: DSS)
Related Chandra Images:
- Photo Album: Kepler's Supernova Remnant
8. Chandra's Kepler Image from Optical View
QuicktimeMPEG This sequence begins with an optical view of the region containing the Kepler supernova remnant. After zooming in, Chandra's X-ray image appears, showing the dramatic difference between what is seen in various wavelengths.
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(X-ray: NASA/CXC/NCSU/S.Reynolds et al; Optical: DSS)
Related Chandra Images:
QuicktimeMPEG This sequence begins with an optical view of the region containing the Kepler supernova remnant. After zooming in, Chandra's X-ray image appears, showing the dramatic difference between what is seen in various wavelengths.
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(X-ray: NASA/CXC/NCSU/S.Reynolds et al; Optical: DSS)
Related Chandra Images:
- Photo Album: Kepler's Supernova Remnant
9. Comparison of Type Ia Supernovas
QuicktimeMPEG This sequence compares the Chandra image of DEM L238 with the Chandra image of 3 Type Ia supernova remnants located in the Milky Way. The X-ray emission for Kepler's remnant contains a bright central region similar to DEM L238, while the X-ray emission for Tycho's remnant and SN 1006 are generally much more uniform. These results suggest that the stars that exploded and caused the DEM L238 and Kepler supernova remnants were much younger than the stars that produced the Tycho and SN 1006 remnants.
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(NASA/CXC)
Related Chandra Images:
QuicktimeMPEG This sequence compares the Chandra image of DEM L238 with the Chandra image of 3 Type Ia supernova remnants located in the Milky Way. The X-ray emission for Kepler's remnant contains a bright central region similar to DEM L238, while the X-ray emission for Tycho's remnant and SN 1006 are generally much more uniform. These results suggest that the stars that exploded and caused the DEM L238 and Kepler supernova remnants were much younger than the stars that produced the Tycho and SN 1006 remnants.
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(NASA/CXC)
Related Chandra Images:
- Photo Album: DEM L238 and DEM L249
10. Images of DEM L238 and DEM L249
QuicktimeMPEG The sequence shows an optical image and then a composite of Chandra X-ray data (blue) and optical data (white) of DEM L238 and DEM L249, two supernova remnants in the Large Magellanic Cloud. The view then shows how DEM L238 appears in the three bands of X-ray emission (low-energy X-rays in red, medium energies in green and high energies in blue). The central region of DEM L238 is green which indicates that it is rich in iron, identifying it as a Type Ia supernova that came from the explosion of a much younger star than expected.
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(X-ray: NASA/CXC/NCSU/K.Borkowski; Optical: NOAO/CTIO/MCELS)
Related Chandra Images:
QuicktimeMPEG The sequence shows an optical image and then a composite of Chandra X-ray data (blue) and optical data (white) of DEM L238 and DEM L249, two supernova remnants in the Large Magellanic Cloud. The view then shows how DEM L238 appears in the three bands of X-ray emission (low-energy X-rays in red, medium energies in green and high energies in blue). The central region of DEM L238 is green which indicates that it is rich in iron, identifying it as a Type Ia supernova that came from the explosion of a much younger star than expected.
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(X-ray: NASA/CXC/NCSU/K.Borkowski; Optical: NOAO/CTIO/MCELS)
Related Chandra Images:
- Photo Album: DEM L238 and DEM L249
Revised: April 17, 2013