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OB Stars in the Tycho-2 and 2MASS Catalogues

机译:Tycho-2和2MASS目录中的OB星

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The Tycho-2 propermotions and five-band Tycho-2 and 2MASS photometry for approximately 2.5 million common stars have been used to select OB stars and to determine the extinction and photometric distance for each of them.We have selected 37 485 stars and calculated their reddenings based on their positions in the two-color VT–H, J–Ks diagrams relative to the zero-age main sequence and the theoretical reddening line for B5 stars. Tests confirm that the selected stars belong to the spectral types O–B with a small admixture of later types. We calculate the extinction coefficient R and its variations with Galactic longitude based on the positions of the selected stars in the two-color BT–VT , VT–Ks diagram. The interstellar extinction for each star is calculated as the product of the reddening found and the coefficient R. The extinction and its variations with Galactic longitude agree well with the extinction based on the model by Arenou et al. (1992). Calibration of the relation between the absolute magnitude and reduced propermotion VT AVT +5 +5logμ for Hipparcos stars has allowed us to calculate the absolute magnitudes and photometric distances for the selected stars. The distances found agree with those derived from the Hipparcos parallaxes within 500 pc. The distribution of the stars and the extinction variations with distance found show that the selected stars form an almost complete sample of stars with spectral types earlier than B5 within about 750 pc of the Sun. The sample includes many noticeably reddened stars in the first and second Galactic quadrants that are absent from the Hipparcos and Tycho Spectral Types Catalogues. This slightly changes the pattern of the distribution of OB stars compared to the classical pattern based on Hipparcos.
机译:我们使用Tycho-2固有运动和大约250万颗普通恒星的五波段Tycho-2和2MASS光度法来选择OB恒星,并确定它们的消光和光度距离,我们选择了37485颗恒星并计算出它们根据它们相对于零年龄主序列和B5星理论上的变红线在VT–H,J–Ks两色图中的位置进行变红。测试证实,选定的恒星属于光谱类型O–B,并带有少量的较晚类型的混合物。我们根据两色BT–VT,VT–Ks图中选定恒星的位置,计算消光系数R及其随银河系经度的变化。每颗恒星的星际消光是根据发现的变红与系数R的乘积计算的。该消光及其随银河系经度的变化与基于Arenou等人的模型的消光非常吻合。 (1992)。对Hipparcos恒星的绝对大小和减少的固有运动VT AVT +5 +5logμ之间的关系进行校准,使我们能够计算选定恒星的绝对大小和光度距离。发现的距离与从Hipparcos视差得出的500 pc之内的距离一致。恒星的分布和随着距离的消光变化表明,选定的恒星在大约750 pc的太阳中形成了光谱类型早于B5的几乎完整的恒星样本。该样本在第一和第二个银河象限中包含许多明显变红的恒星,而希普帕尔科斯和第谷光谱类型目录中却没有。与基于Hipparcos的经典模式相比,这稍微改变了OB星的分布模式。

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