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arXiv 0807.4989astro-ph
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大熊座W型双星的新绝对星等刻度

New absolute magnitude calibrations for W Ursa Majoris type binaries

Z. Eker, S. Bilir, E. Yaz, O. Demircan, M. Helvaci

备注：
9 pages, 8 figures and 2 tables, accepted for publication in Astronomische Nachrichten
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摘要：

分析了依巴谷星表中的WUMa星的视差。选取了31颗具有最精确的视差（$σ_π/π<0.15$）的WUMa星，重新标定了WUMa星的周期-光度-颜色（PLC）关系。使用Lutz-Kelker（LK）偏置校正（最可能）的31个选择的W UMa的松弛、周期（$0.26< P(day)< 0.87$）和颜色（0.04< $(B-V)_{0}$ <1.28），修改并重新校准PLC关系。旧的（修订，但没有偏差校正）和新的（LK偏差校正）的关系之间的差异几乎可以忽略不计，在预测的距离W UMa恒星高达约100秒差距。但是，随着恒星距离的增加，它会增加并可能变得无法忍受。此外，利用2微米全天巡天数据的$(J-H)_{0}$和$(H-K_{s})_{0}$颜色，推导了适用于红外数据的PLC关系式。它可以与$-0.01<(J-H)_{0}<0.58$和$-0.10<(H-K_{s})_{0}<0.18$范围内的红外颜色一起使用。尽管{ \em 2 MASS}数据是单历元观测，不能保证在W UMa星的最大亮度时，但已建立的关系在预测W UMa星的LK校正距离时令人惊讶地一致和可靠。

英文摘要：

Parallaxes of W UMa stars in the Hipparcos catalogue have been analyzed. 31 W UMa stars, which have the most accurate parallaxes ($σ_π/π<0.15$) which are neither associated with a photometric tertiary nor with evidence of a visual companion, were selected for re-calibrating the Period--Luminosity--Color (PLC) relation of W UMa stars. Using the Lutz--Kelker (LK) bias corrected (most probable) parallaxes, periods ($0.26< P(day)< 0.87$), and colors (0.04<$(B-V)_{0}$<1.28) of the 31 selected W UMa, the PLC relation have been revised and re-calibrated. The difference between the old (revised but not bias corrected) and the new (LK bias corrected) relations are almost negligible in predicting the distances of W UMa stars up to about 100 parsecs. But, it increases and may become intolerable as distances of stars increase. Additionally, using $(J-H)_{0}$ and $(H-K_{s})_{0}$ colors from 2MASS (Two Micron All Sky Survey) data, a PLC relation working with infrared data was derived. It can be used with infrared colors in the range $-0.01<(J-H)_{0}<0.58$, and $-0.10<(H-K_{s})_{0}<0.18$. Despite {\em 2MASS} data are single epoch observations, which are not guaranteed at maximum brightness of the W UMa stars, the established relation has been found surprisingly consistent and reliable in predicting LK corrected distances of W UMa stars.

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