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Stellar evolution



Main article: Black hole

If the mass of the stellar remnant is high enough, the neutron degeneracy pressure will be insufficient to prevent collapse below the Schwarzschild radius. The stellar remnant thus becomes a black hole. The mass at which this occurs is not known with certainty, but is currently estimated at between 2 and 3 solar masses.

Black holes are predicted by the theory of general relativity. According to classical general relativity, no matter or information can flow from the interior of a black hole to an outside observer, although quantum effects may allow deviations from this strict rule. The existence of black holes in the universe is well supported, both theoretically and by astronomical observation.

Since the core-collapse supernova mechanism itself is imperfectly understood, it is still not known whether it is possible for a star to collapse directly to a black hole without producing a visible supernova, or whether some supernovae initially form unstable neutron stars which then collapse into black holes; the exact relation between the initial mass of the star and the final remnant is also not completely certain. Resolution of these uncertainties requires the analysis of more supernovae and supernova remnants.

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References

  1. ^ "Why the Smallest Stars Stay Small." (November 1997). Sky & Telescope (22). 
  2. ^ Alan C. Edwards (1969). "The hydrodynamics of the helium flash". Monthly Notices of the Royal Astronomical Society 146: 445 - 472. 
  3. ^ I. Juliana Sackmann et al (1993). "Our Sun. III. Present and Future". The Astrophysical Journal 418: 457 - 468. 
  4. ^ D. Vanbeveren (1998). "Massive stars.". The Astronomy and Astrophysics Review 9: 63 - 152. 
  5. ^ Ken'ichi Nomoto (1987). "Evolution of 8-10 solar mass stars toward electron capture supernovae. II - Collapse of an O + Ne + Mg core". Astrophysical Journal 322 Part 1: 206 - 214. 
  6. ^ Claudio Ritossa et al (1999). "On the Evolution of Stars that Form Electron-degenerate Cores Processed by Carbon Burning. V. Shell Convection Sustained by Helium Burning, Transient Neon Burning, Dredge-out, URCA Cooling, and Other Properties of an 11 M_solar Population I Model Star". The Astrophysical Journal 515: 381 - 397. 
  7. ^ How do Massive Stars Explode?
  8. ^ Supernova Simulations Still Defy Explosions.
  9. ^ E. P. J. van den Heuvel (2004). "X-Ray Binaries and Their Descendants: Binary Radio Pulsars; Evidence for Three Classes of Neutron Stars?". Proceedings of the 5th INTEGRAL Workshop on the INTEGRAL Universe (ESA SP-552): 185 - 194. 
  10. ^ Pair Instability Supernovae and Hypernovae., Nicolay J. Hammer, (2003), accessed May 7, 2007.
  11. ^ Ken'ichi Nomoto (1984). "Evolution of 8-10 solar mass stars toward electron capture supernovae. I - Formation of electron-degenerate O + Ne + Mg cores". Astrophysical Journal 277 Part 1: 791 - 805. 
  12. ^ Ken'ichi Nomoto and Yoji Kondo (1991). "Conditions for accretion-induced collapse of white dwarfs". Astrophysical Journal 367 Part 2: L19 - L22. 

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