红巨星中长副周期变星的起源
发布时间：2019-07-04 17:23
【摘要】：长副周期变星是一类特殊的半规则变星,大量存在于银河系和大小麦哲伦云中,约占渐近巨星分支的25%～30%。该类变星有两个光变周期,短的主周期为30～200 d,由径向脉动的低阶模式导致;长的副周期长达400～1500 d。在长周期变星的周光关系中,长副周期变星处在D序列,平行于径向脉动的A、B和C序列,且与属于双星系统的E序列部分重叠。长副周期现象的起源一直是个谜,现存的解释模型有:径向脉动、非径向脉动、双星、磁活动、带有一个巨大黑子的转动红巨星、转动的椭球红巨星、κ机制等,但这些模型没有一种能完美地解释长副周期变星的起源。
文内图片：
图片说明：大麦哲伦云中长副周期变星的视向速度曲线[la}
[Abstract]:Long periodic variable stars are a special class of semi-regular variable stars, which exist in the Milky way and Magellanic clouds, accounting for about 25% and 30% of the branches of asymptotically superstars. This kind of variable star has two photoperiod, the short main period is 30 鈮，
本文编号：2510082
文内图片：
图片说明：大麦哲伦云中长副周期变星的视向速度曲线[la}
[Abstract]:Long periodic variable stars are a special class of semi-regular variable stars, which exist in the Milky way and Magellanic clouds, accounting for about 25% and 30% of the branches of asymptotically superstars. This kind of variable star has two photoperiod, the short main period is 30 鈮，
本文编号：2510082
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