摘要
ζAur双星系统是一类特殊双星系统 ,由一颗晚型红巨星和一颗早型热星组成。红巨星有强大的星风物质损失 ,并在双星系统外部形成一向外膨胀的气壳 ;热星在星风气壳内作轨道运动。由于热星的紫外辐射可以激发星风物质而发光 ,星风物质的向外运动和双星的轨道运动使得ζAur型双星系统的光谱产生特殊周期性变化的PCyg谱线。近十多年来发展起来的、利用运动大气理论计算ζAur型双星系统的PCyg谱线形成 ,以确定这类双星系统中红巨星的星风物质损失率的方法是目前测定物质损失率方法中较为精确的方法。
The ζ Aur-type binary system consists of a hot early type star and a late type red giant or rad supergiant with strong stellar wind,which forms an expanding gas shell surrounding the binary system.The outward motion of the shell and the orbital motion of the hot component in the shell produce the P Cygni type lines with periodic and peculiarly variable profiles in the spectra of the ζ Aur-type binary systems.The methods based on moving atmosphere theories are developed in more than this decade year.It is more accurate than other methods to determine the mass loss rates due to stellar wind.
出处
《云南天文台台刊》
CSCD
2000年第1期1-9,共9页
Publications of the Yunnan Observatoty
