脈動白矮星 

脈動白矮星是一種光度變化是由自身內部非徑向的引力波脈動造成的白矮星,已經知道的脈動白矮星包括DAV,或鯨魚座ZZ(這是大氣層以為主,光譜為DA型的白矮星)[1], pp. 891, 895DBV,或 武仙座V777(這是大氣層以為主,光譜為DB型的白矮星)[2], p. 3525、和室女座GW(這是大氣層以氦、為主,光譜為PG 1159型的白矮星。有些作者會將非PG 1159星的也包括在室女GW型內)。室女GW型可以再分為DOVPNNV[3], §1.1, 1.2;[4]。嚴格來說,它們還不是白矮星,因為在赫羅圖上還沒有抵達白矮星的位置,但可以算是前白矮星[3], § 1.1;[5]。大氣層以為主的次分類DQV星,也被建議屬於這一類[6]

由於有許多週期在數百秒至數千秒的變化模式疊加,使它們輸出的光度變化不會很大(1%-30%)。對這些變化的觀測提供了白矮星內部星震的證據[7]

  1. ^ Physics of white dwarf stars页面存档备份,存于互联网档案馆), D. Koester and G. Chanmugam, Reports on Progress in Physics 53 (1990), pp. 837–915.
  2. ^ White dwarfs, Gilles Fontaine and François Wesemael, in Encyclopedia of Astronomy and Astrophysics, ed. Paul Murdin, Bristol and Philadelphia: Institute of Physics Publishing and London, New York and Tokyo: Nature Publishing Group, 2001. ISBN 0333750888.
  3. ^ 3.0 3.1 Mapping the Instability Domains of GW Vir Stars in the Effective Temperature-Surface Gravity Diagram页面存档备份,存于互联网档案馆), Quirion, P.-O., Fontaine, G., Brassard, P., Astrophysical Journal Supplement Series 171 (2007), pp. 219–248.
  4. ^ §1, Detection of non-radial g-mode pulsations in the newly discovered PG 1159 star HE 1429-1209页面存档备份,存于互联网档案馆), T. Nagel and K. Werner, Astronomy and Astrophysics 426 (2004), pp. L45–L48.
  5. ^ 引证错误:没有为名为obrien的参考文献提供内容
  6. ^ SDSS J142625.71+575218.3: A Prototype for a New Class of Variable White Dwarf, M. H. Montgomery et al., Astrophysical Journal 678, #1 (May 2008), pp. L51–L54, Bibcode2008ApJ...678L..51M, doi:10.1086/588286.
  7. ^ Asteroseismology of white dwarf stars, D. E. Winget, Journal of Physics: Condensed Matter 10, #49 (December 14, 1998), pp. 11247–11261. DOI 10.1088/0953-8984/10/49/014.



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