论文标题
入门：如何从静液压表面发起超音速恒星风
Getting started: How a supersonic stellar wind is initiated from a hydrostatic surface
论文作者
论文摘要
恒星的大部分质量都以静水平衡结合，其中压力平衡了重力。但是，如果在某些近表面的层上，额外的外部力克服了重力，则可以过渡到超音速，流出的风，并带有声音点，在那里，向外力取消了重力，标志着液压气氛和空白流出之间的划分。这次演讲将通过这种出色的风流流出来回顾一般问题，以及这如何帮助设定风质量损失率。主要讨论与四个突出的稳态风中的流动开始形成了鲜明对比：（1）太阳的压力驱动冠状风和其他凉爽的恒星； （2）来自OB恒星的线驱动风； （3）来自Wolf-Rayet（WR）恒星的大量浓密风的两阶段启动模型； （4）高度进化的巨星慢速“溢出”质量损失。讨论的关注点简要回顾了爆发性的质量损失，特别关注Eta Carinae的巨型喷发。
Most of a star's mass is bound in a hydrostatic equilibrium in which pressure balances gravity. But if at some near-surface layer additional outward forces overcome gravity, this can transition to a supersonic, outflowing wind, with the sonic point, where the outward force cancels gravity, marking the division between hydrostatic atmosphere and wind outflow. This talk will review general issues with such transonic initiation of a stellar wind outflow, and how this helps set the wind mass loss rate. The main discussion contrasts the flow initiation in four prominent classes of steady-state winds: (1) the pressure-driven coronal wind of the sun and other cool stars; (2) line-driven winds from OB stars; (3) a two-stage initiation model for the much denser winds from Wolf-Rayet (WR) stars; and (4) the slow "overflow" mass loss from highly evolved giant stars. A follow on discussion briefly reviews eruptive mass loss, with particular focus on the giant eruption of eta Carinae.
