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

页码：25 / 36

页数：12

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