紫外波段的剥离氦星
Stripped helium stars in UV
浏览论文内容
中文总结 AI 辅助
本文建模银河系剥离氦星群体，估计其数量受公共包层并合影响，紫外超量探测受伴星光谱主导限制，候选体可减至千以内。
中文摘要 AI 辅助
本文提出了银河系剥离氦星群体的模型，这些恒星是密近双星中质量约为5至24倍太阳质量的初始主星在洛希瓣溢出（RLOF）后的残余。这些恒星在光谱的紫外波段辐射，可能被计划中的“光谱-紫外”（Spektr-UV，即WSO-UV）太空望远镜上的探测器观测到。对于当前银河系恒星形成率2太阳质量每年，估计有效温度不低于25,000开尔文、质量在1至7倍太阳质量范围内的此类天体数量在14,700至28,500之间。质量在2至7倍太阳质量范围内的数量为3,200至5,500。影响该估计的主要演化因素是可能形成公共包层以及其中成分星的并合。通过紫外超量探测剥离氦星候选体受到阻碍，因为在双星复合光谱中，主序伴星的光谱占主导。这种观测选择效应可能将可通过测光潜在探测到的剥离氦星候选体数量减少至不超过1,000。
英文摘要
The model of Galactic population of stripped helium stars, the remnants of $5 \lesssim M/M_\odot \lesssim 24$ primary components of close binaries after RLOF is presented. These stars emit in the UV range of the spectrum and may be observed by detectors aboard planned "Spektr-UV" (WSO-UV) space telescope. For the current star formation rate in the Galaxy 2$\mathrm {M_\odot yr^{-1}}$, the estimate of the number of 1 to 7 $M_\odot$ objects with $T_{\rm eff} \gtrsim$25,000\,K ranges from 14700 to 28500. The number of 2 to 7 $M_\odot$ objects is 3200 to 5500. The main evolutionary factor influencing the estimate is possible formation of common envelopes and merger of components in them. Detection of candidate stripped helium stars by UV-excess is hampered by the dominance of main-sequence companions to stripped helium stars in the combined spectra of binaries. This effect of observational selection may reduce the number of candidate stripped helium stars potentially detectable by photometry to $\lesssim 1000$.
发表机构
- Institute of Astronomy of the RAS（俄罗斯科学院天文研究所）
- Sternberg Astronomical Institute, MSU（莫斯科国立大学斯滕伯格天文研究所）
- Moscow Institute of Physics and Technology（莫斯科物理技术学院）
机构由 AI 辅助整理，请以论文原文为准。
