arXiv 0811.35572008-11-21astro-ph

Herbig Ae/Be型和Vega型星的参数

Parameters of Herbig Ae/Be and Vega-type stars

Benjamin Montesinos, Carlos Eiroa, Alcione Mora, Bruno Merin

备注：: 18 pages, 11 figures
DOI：: 10.1051/0004-6361:200810623

摘要：

这项工作提出了27个年轻的早期型恒星的有效温度，重力，金属丰度，质量，光度和年龄的测定，其中大多数的年龄范围在1-10百万年，和三个疑似热的同伴后T金牛星属于Lindroos二进制样本。这些物体中的大多数在其光谱能量分布中显示出IR过量，这表明存在盘。这项工作与恒星物理学、盘物理学和行星系统形成等领域有关。光谱能量分布和中分辨率光谱被用来估计有效温度。比较的轮廓的巴耳末线与合成的配置文件提供了恒星重力的值。高分辨率光学观测和合成光谱用于估计金属丰度[M/H]。一旦知道了每颗恒星的这三个参数，演化轨迹和等时线就可以提供质量、光度、年龄和距离（在某些情况下是上限）的估计。该方法是原始的意义上说，它是距离无关的，即恒星参数的估计不需要，因为它发生在其他作品，知识的距离对象。详细讨论了一些个别对象，特别是VV Ser，RR Tau，49 Cet和后金牛座T的三个可疑的热同伴，提出。本文还表明，在恒星参数的计算中，系统星+盘的形态和行为所带来的困难。

英文摘要：

This work presents the determination of the effective temperature, gravity, metallicity, mass, luminosity and age of 27 young early-type stars, most of them in the age range 1-10 Myr, and three -suspected- hot companions of post-T Tauri stars belonging to the Lindroos binary sample. Most of these objects show IR excesses in their spectral energy distributions, which are indicative of the presence of disks. The work is relevant in the fields of stellar physics, physics of disks and formation of planetary systems. Spectral energy distributions and mid-resolution spectra were used to estimate the effective temperature. The comparison of the profiles of the Balmer lines with synthetic profiles provides the value of the stellar gravity. High-resolution optical observations and synthetic spectra are used to estimate the metallicity, [M/H]. Once these three parameters are known for each star, evolutionary tracks and isochrones provide estimations of the mass, luminosity, age and distance (or upper limits in some cases). The method is original in the sense that it is distance-independent, i.e. the estimation of the stellar parameters does not require, as it happens in other works, the knowledge of the distance to the object. A detailed discussion on some individual objects, in particular VV Ser, RR Tau, 49 Cet and the three suspected hot companions of post-T Tauris, is presented. The paper also shows the difficulty posed by the morphology and behaviour of the system star+disk in the computation of the stellar parameters.

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英文摘要：

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