Physics of Mass Loss in Massive Stars

被引：2
作者：
Puls, Joachim [1 ]
Sundqvist, Jon O. [1 ]
Markova, Nevena [2 ]
机构：
[1] Univ Sternwarte, Scheinerstr 1, D-81679 Munich, Germany
[2] BAS, Inst Astron NAO, Smoljan 4700, Bulgaria
来源：
NEW WINDOWS ON MASSIVE STARS: ASTEROSEISMOLOGY, INTERFEROMETRY AND SPECTROPOLARIMETRY | 2014年 / 307卷
关键词：
stars: early-type; stars: mass loss; stars: winds; outflows; RADIATION-DRIVEN WINDS; HOT LUMINOUS STARS; HYDRODYNAMIC MODEL ATMOSPHERES; STELLAR WINDS; LOSS RATES; O-STARS; METALLICITY DEPENDENCE; LINE-PROFILES; WR STARS; SIMULATIONS;
D O I：
10.1017/S174392131400622X
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We review potential mass-loss mechanisms in the various evolutionary stages of massive stars, from the well-known line-driven winds of O-stars and BA-supergiants to the less-understood winds of Red Supergiants. We discuss optically thick winds from Wolf-Rayet stars and Very Massive Stars, and the hypothesis of porosity-moderated, continuum-driven mass loss from stars formally exceeding the Eddington limit, which might explain the giant outbursts from Luminous Blue Variables. We finish this review with a glance on the impact of rapid rotation, magnetic fields and small-scale inhomogeneities in line-driven winds.
引用
收藏
页码：25 / 36
页数：12
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