An Extremely Slow Nova?
天体物理学
2009-11-06 v1
摘要
The binary companion to the peculiar F supergiant HD 172481 is shown to be a Mira variable with a pulsation period of 312 days. Its characteristics are within the normal range found for solitary Miras of that period, although its pulsation amplitude and mass-loss rate (M(dot) ~ 3 x 10^{-6} solar masses per year) are higher than average. Reasons are given for suspecting that the F supergiant, which has L ~ 10^4 solar luminosities, is a white dwarf burning hydrogen accreted from its companion.
引用
@article{arxiv.astro-ph/0102498,
title = {An Extremely Slow Nova?},
author = {Patricia Whitelock and Freddy Marang},
journal= {arXiv preprint arXiv:astro-ph/0102498},
year = {2009}
}
备注
4 pages, 1 figure, to be published in MNRAS