錢德拉塞卡極限 

錢德拉塞卡極限Chandrasekhar Limit),以印度裔美籍天文物理學家蘇布拉馬尼揚·錢德拉塞卡命名,是無自轉恆星以電子簡併壓力阻擋重力塌縮所能承受的最大質量,這個值大約是1.44倍太陽質量 [1][2],計算的結果會依據原子核的結構和溫度而有些差異[3]。錢德拉塞卡[4], eq. (36),[5], eq. (58),[6], eq. (43) 给出

此處, μe是分子的每電子平均質量,是氫原子的質量,而是與莱恩-埃姆登方程有關的常數,在數值上,這個值大約是 (2/μe)2 · 2.85 · 1030 公斤,或是,此處的是標準的太陽質量 [7],而普朗克質量,是M的數量級極限MPl3/mH2

白矮星而言,電子簡併壓力是其抵抗重力的唯一力量,因此這個值也是白矮星的質量上限。主序星的質量若超過8倍的太陽質量,在演化結束前不能拋掉足夠的質量成為穩定的白矮星,因此會成為中子星或是黑洞 [8][9][10]

  1. ^ p. 55, How A Supernova Explodes, Hans A. Bethe and Gerald Brown, pp. 51–62 in Formation And Evolution of Black Holes in the Galaxy: Selected Papers with Commentary, Hans Albrecht Bethe, Gerald Edward Brown, and Chang-Hwan Lee, River Edge, NJ: World Scientific: 2003. ISBN 981238250X.
  2. ^ Mazzali, P. A.; K. Röpke, F. K.; Benetti, S.; Hillebrandt, W. A Common Explosion Mechanism for Type Ia Supernovae. Science. 2007, 315 (5813): 825–828. doi:10.1126/science.1136259. 
  3. ^ The Neutron Star and Black Hole Initial Mass Function页面存档备份,存于互联网档案馆), F. X. Timmes, S. E. Woosley, and Thomas A. Weaver, Astrophysical Journal 457 (February 1, 1996), pp. 834–843.
  4. ^ The Highly Collapsed Configurations of a Stellar Mass页面存档备份,存于互联网档案馆), S. Chandrasekhar, Monthly Notices of the Royal Astronomical Society 91 (1931), 456–466.
  5. ^ The Highly Collapsed Configurations of a Stellar Mass (second paper)页面存档备份,存于互联网档案馆), S. Chandrasekhar, Monthly Notices of the Royal Astronomical Society, 95 (1935), pp. 207--225.
  6. ^ On Stars, Their Evolution and Their Stability页面存档备份,存于互联网档案馆), Nobel Prize lecture, Subrahmanyan Chandrasekhar, December 8, 1983.
  7. ^ Standards for Astronomical Catalogues, Version 2.0页面存档备份,存于互联网档案馆), section 3.2.2, web page, accessed 12-I-2007.
  8. ^ White dwarfs in open clusters. VIII. NGC 2516: a test for the mass-radius and initial-final mass relations页面存档备份,存于互联网档案馆), D. Koester and D. Reimers, Astronomy and Astrophysics 313 (1996), pp. 810–814.
  9. ^ An Empirical Initial-Final Mass Relation from Hot, Massive White Dwarfs in NGC 2168 (M35)页面存档备份,存于互联网档案馆), Kurtis A. Williams, M. Bolte, and Detlev Koester, Astrophysical Journal 615, #1 (2004), pp. L49–L52; also arXiv astro-ph/0409447页面存档备份,存于互联网档案馆).
  10. ^ How Massive Single Stars End Their Life页面存档备份,存于互联网档案馆), A. Heger, C. L. Fryer, S. E. Woosley, N. Langer, and D. H. Hartmann, Astrophysical Journal 591, #1 (2003), pp. 288–300.



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