File:Supernovas Portrait Gallery (1999-snrg - g21bluepurple2t).tiff
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![File:Supernovas Portrait Gallery (1999-snrg - g21bluepurple2t).tiff](https://upload.wikimedia.org/wikipedia/commons/thumb/a/aa/Supernovas_Portrait_Gallery_%281999-snrg_-_g21bluepurple2t%29.tiff/lossy-page1-722px-Supernovas_Portrait_Gallery_%281999-snrg_-_g21bluepurple2t%29.tiff.jpg?20240528093620)
Size of this JPG preview of this TIF file: 722 × 599 pixels. Other resolutions: 289 × 240 pixels | 578 × 480 pixels | 925 × 768 pixels | 1,234 × 1,024 pixels | 2,100 × 1,743 pixels.
Original file (2,100 × 1,743 pixels, file size: 1.31 MB, MIME type: image/tiff)
File information
Structured data
Captions
Captions
Chandra X-ray Image of G21.5-0.9
Summary
[edit]DescriptionSupernovas Portrait Gallery (1999-snrg - g21bluepurple2t).tiff |
English: The identification of G21.5-0.9 as the remnant of a supernova explosion is based on indirect evidence from radio and X-ray observations. At both radio and X-ray wavelengths, it appears as round patch in the sky. Detailed observations with radio telescopes confirm that the radio waves are produced by high energy electrons spiraling around magnetic field lines (synchrotron radiation). The X-rays are probably produced by the same process, but the electrons involved have energies many thousands times higher than those that produce the radio waves. The favored theory is that the high-energy electrons responsible for both the radio and X-ray emission are produced by a rapidly rotating, highly magnetized neutron star left behind when a massive star exploded some 40,000 years ago. |
Date | 20 September 1999 (upload date) |
Source | Supernovas Portrait Gallery |
Author | NASA/SAO |
Other versions |
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Category InfoField | Supernovas & Supernova Remnants, Neutron Stars/X-ray Binaries |
Color Code InfoField | Intensity |
Constellation InfoField | Scutum |
Coordinates (J2000) InfoField | RA 18h 33m 33.50s |
Distance Estimate InfoField | 20,000 light years |
Scale InfoField | 7.5 arcmin across. |
Instruments InfoField | ACIS |
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This media is a product of the Chandra X-ray Observatory Credit and attribution belongs to the Chandra X-ray Center, NASA/SAO/Penn State University/MIT |
Licensing
[edit]Public domainPublic domainfalsefalse |
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This file is in the public domain in the United States because it was solely created by NASA. NASA copyright policy states that "NASA material is not protected by copyright unless noted". (See Template:PD-USGov, NASA copyright policy page or JPL Image Use Policy.) | ![]() |
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Date/Time | Thumbnail | Dimensions | User | Comment | |
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current | 09:36, 28 May 2024 | ![]() | 2,100 × 1,743 (1.31 MB) | OptimusPrimeBot (talk | contribs) | #Spacemedia - Upload of https://chandra.si.edu/photo/1999/snrg/g21bluepurple2t.tif via Commons:Spacemedia |
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File usage on Commons
The following 7 pages use this file:
- File:Chandra X-ray Image of G21 5-0 9 with Scale Bar (1999-snrg-more-2).jpg
- File:Chandra X-ray Image of G21 5-0 9 with Scale Bar (1999-snrg-more-2).tiff
- File:E0102 - Chandra Supernovas Portrait Gallery (1999-snrg - e0102electricbluej).jpg
- File:E0102 - Chandra Supernovas Portrait Gallery (1999-snrg - e0102electricbluet).tiff
- File:Supernovas Portrait Gallery (1999-snrg - g21bluepurple2j).jpg
- File:Supernovas Portrait Gallery (1999-snrg - pulsarV2BBB).jpg
- File:Supernovas Portrait Gallery (1999-snrg - pulsarV2BBB).tiff
Metadata
This file contains additional information such as Exif metadata which may have been added by the digital camera, scanner, or software program used to create or digitize it. If the file has been modified from its original state, some details such as the timestamp may not fully reflect those of the original file. The timestamp is only as accurate as the clock in the camera, and it may be completely wrong.
Image title | G21.5-0.9 is about 16,000 light years from Earth. Chandra's image shows a bright nebula surrounded by a much larger diffuse cloud. Inside the inner nebula is a bright central source that is thought to be a rapidly rotating highly magnetized neutron star. A rotating neutron star acts like a powerful generator, creating intense electric voltages that accelerate electrons to speeds close to the speed of light. The total output of this generator is greater than a thousand suns. The fluffy appearance of the central nebula, which is about five light years across, is thought to be due to magnetic field lines that constrain the motions of the high-energy electrons. |
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Author | Chandra X-ray Observatory Center |
Width | 2,100 px |
Height | 1,743 px |
Bits per component |
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Compression scheme | LZW |
Pixel composition | RGB |
Orientation | Normal |
Number of components | 3 |
Number of rows per strip | 41 |
Horizontal resolution | 300 dpi |
Vertical resolution | 300 dpi |
Data arrangement | chunky format |
Software used | Adobe Photoshop CS4 Windows |
File change date and time | 10:00, 21 February 2013 |
Exif version | 2.21 |
Color space | sRGB |
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1,743 pixel
2,100 pixel
1,371,736 byte
2c7f47cdc16cc84be1cb908a48d17b66c1651b44
20 September 1999
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