Stark Broadening of Carbon and Oxygen Lines in Hot DQ White Dwarf Stars: Recent Results and Applications

Baltic astronomy

article

P. Dufour¹  N. Ben Nessib²  S. Sahal-Bréchot³  M. S. Dimitrijević⁴ 

[1] D´epartement de Physique, Universit´e de Montr´eal;INSAT (National Institute of Applied Sciences and Technology), University of Carthage;Observatoire de Paris, LERMA, CNRS, UMR;Astronomical Observatory

关键词: stars;    white dwarfs;    fundamental parameters;    Stark broadening;   

DOI  :  10.1515/astro-2017-0329

来源: Institute of Theoretical Physics and Astronomy

【 摘 要 】

White dwarf stars are traditionally found to have surface compositions made primarily of hydrogen or helium. However, a new family has recently been uncovered, the so-called hot DQ white dwarfs, which have surface compositions dominated by carbon and oxygen with little or no trace of hydrogen and helium (Dufour et al. 2007, 2008, 2010). Deriving precise atmospheric parameters for these objects (such as the effective temperature and the surface gravity) requires detailed modeling of spectral line profiles. Stark broadening parameters are of crucial importance in that context. We present preliminary results from our new generation of model atmospheres including the latest Stark broadening calculations for C II lines and discuss the implications as well as future work that remains to be done.

【 授权许可】

Unknown