當在吸積時,質量的損失和電離化過程處於平衡狀態,系統被認為是寧靜的。此時,系統持續以大致平穩地速率釋放能量[2]。這可以通過恆星的光譜能量分布(spectral energy distribution,SED)來觀察,該分部將保持相對恆定。 of the star which will be remain relatively constant.這可以通過恆星的[光譜能量分布](SED)來觀察,該分佈將保持相對恒定。
^Samus, N. N.; Durlevich, O. V.; et al. VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013). VizieR On-line Data Catalog: B/gcvs. Originally Published in: 2009yCat....102025S. 2009, 1. Bibcode:2009yCat....102025S.
^ 2.02.1Skopal, Augustin. How to understand the light curves of symbiotic stars. Journal of the American Association of Variable Star Observers. 8 May 2008, 36 (1): 9. Bibcode:2008JAVSO..36....9S. arXiv:0805.1222.
^Tomokazu Kogure; Kam-Ching Leung. The Astrophysics of Emission-Line Stars. Springer Science & Business Media. 5 May 2010: 5– [2020-05-18]. ISBN 978-0-387-68995-1. (原始内容于2020-08-19).
^Mikołajewska, Joanna. Orbital and stellar parameters of symbiotic stars. ASP Conference Series. 2002, 303: 9. Bibcode:2003ASPC..303....9M. arXiv:astro-ph/0210489.
^ 5.05.1Skopal, A. Disentangling the composite continuum of symbiotic binaries. I. S-type systems. Astronomy and Astrophysics. 2005, 440 (3): 995. Bibcode:2005A&A...440..995S. arXiv:astro-ph/0507272. doi:10.1051/0004-6361:20034262.
^Sokoloski, J. L. Symbiotic Stars as Laboratories for the Study of Accretion and Jets: A Call for Optical Monitoring. Journal of the American Association of Variable Star Observers. June 20, 2003, 31 (2): 89–102. Bibcode:2003JAVSO..31...89S. arXiv:astro-ph/0403004.
外部連結编辑
List of symbiotic stars (页面存档备份,存于互联网档案馆) discovered by IPHAS