Sion Edward M, Godon Patrick
Department of Astrophysics & Space Science, Villanova University, 800 Lancaster Ave., Villanova, PA 19085, USA.
Acta Polytech CTU Proc. 2015;2(1):35-40. doi: 10.14311/APP.2015.02.0035.
In this review, we summarize what is currently known about the surface temperatures of accreting white dwarfs in non-magnetic and magnetic cataclysmic variables (CVs) based upon synthetic spectral analyses of far ultraviolet data. We focus only on white dwarf surface temperatures, since in the area of chemical abundances, rotation rates, WD masses and accretion rates, relatively little has changed since our last review, pending the results of a large HST GO program involving 48 CVs of different CV types. The surface temperature of the white dwarf in SS Cygni is re-examined in the light of its revised distance. We also discuss new HST spectra of the recurrent nova T Pyxidis as it transitioned into quiescence following its April 2011 nova outburst.
在本综述中，我们基于对远紫外数据的合成光谱分析，总结了目前关于非磁性和磁性激变变星（CVs）中吸积白矮星表面温度的已知信息。我们仅关注白矮星表面温度，因为在化学丰度、自转速率、白矮星质量和吸积率方面，自我们上次综述以来变化相对较小，等待一项涉及48颗不同CV类型的大型哈勃太空望远镜（HST）常规观测计划的结果。根据SS Cygni修正后的距离，重新审视了它的白矮星表面温度。我们还讨论了再发新星T Pyxidis在2011年4月新星爆发后进入宁静期时的新哈勃太空望远镜光谱。
