 | |
| Event type | Type II supernova  |
|---|---|
| Type II[1] | |
| Date | 1979 |
| Constellation | Coma Berenices |
| Right ascension | 12h 22m 58.58s |
| Declination | +15° 47′ 52.7″ |
| Epoch | J2000.0 |
| Galactic coordinates | G271.2454 +76.8848 |
| Distance | 50 Mly |
| Remnant | ? |
| Host | M100 |
| Progenitor | ? |
| Progenitor type | ? |
| Colour (B-V) | ? |
| Peak apparent magnitude | +12.23 |
| Other designations | SN 1979C, AAVSO 1217+16 |
SN 1979C was a supernova about 50 million light-years away in Messier 100, a spiral galaxy in the constellation Coma Berenices. The Type II supernova was discovered April 19, 1979 by Gus Johnson, a school teacher and amateur astronomer.[2] This type of supernova is known as a core collapse and is the result of the internal collapse and violent explosion of a large star. A star must have at least 9 times the mass of the Sun in order to undergo this type of collapse.[3] The star that resulted in this supernova was estimated to be in the range of 20 solar masses.[1]
On November 15, 2010 NASA announced that evidence of a black hole had been detected as a remnant of the supernova explosion. Scientists led by Dr. Dan Patnaude from the Center for Astrophysics | Harvard & Smithsonian in Cambridge, MA evaluated data gathered between 1995 and 2007 from several space based observatories. NASA's Chandra X-ray Observatory, the Swift Gamma-Ray Burst Mission, as well as the European Space Agency's XMM-Newton, and Germany's ROSAT all participated in the examination.[4]
The researchers observed a steady source of X-rays and determined that it was likely that this was material being fed into the object either from the supernova or a binary companion. However, an alternative explanation would be that the X-ray emissions could be from the pulsar wind nebula from a rapidly spinning pulsar, similar to the one in the center of the Crab Nebula.[4] These two ideas account for several types of known X-ray sources. In the case of black holes the material that falls into the black hole emits the X-rays and not the black hole itself. Gas is heated by the fall into the strong gravitational field.
SN 1979C has also been studied in the radio frequency spectrum. A light curve study was performed between 1985 and 1990 using the Very Large Array radio telescope in New Mexico.[5]
See also
References
- ^ a b Nancy Atkinson (November 15, 2010). "Has a Recent, Nearby Supernova Become a Baby Black Hole?". Universe Today. Retrieved 2010-11-18.
- ^ Peter Edmonds (November 16, 2010). "The Man Who Discovered SN 1979C and Beat the Machines". Harvard & Smithsonian. Retrieved 2010-11-21.
- ^ Gilmore, Gerry (2004). "The Short Spectacular Life of a Superstar". Science. 304 (5697): 1915–1916. doi:10.1126/science.1100370. PMID 15218132. S2CID 116987470. Retrieved 2007-05-01.
- ^ a b Trent Perrotto; Janet Anderson; Megan Watzke (Nov 15, 2010). "NASA'S Chandra Finds Youngest Nearby Black Hole". NASA. Archived from the original on 2016-03-03. Retrieved 2010-11-15.
- ^ Weiler, K. W.; van Dyk, S. D.; Discenna, J. L.; Panagia, N.; Sramek, R. A. (1991). "The 10 year radio light curves for SN 1979C". Astrophysical Journal. 380: 161–166. Bibcode:1991ApJ...380..161W. doi:10.1086/170571.
External links
- Light curves and spectra Archived 2021-05-22 at the Wayback Machine on the Open Supernova Catalog
- SN 1979C in M100
- A Tour of SN 1979C (narration of podcast by Dr. Dan Patnaude)
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This page was last edited on 26 November 2023, at 06:19