论文标题
超短期期联系人二进制：限制使用Gaia视差的主要参数
Ultra-short period contact binaries: restricting the parameters of the primary using Gaia parallax
论文作者
论文摘要
通过选择轨道周期低于0.22天截止的W UMA型变量，研究了可能的M型接触二进制。将GAIA视差与Gaia和2Mass光度法结合使用，以获得674个红色可变星的G和J波段绝对大小，该恒星在VSX数据库中被分类为接触二进制。主序列冷却矮人的绝对大小随光谱类型而变化很大，光谱类型被用来创建具有光谱类型M0-M3的原始系统的218个系统的选择。单独检查了46个系统的光效，具有最低的近红外亮度，以确认或拒绝UMA分类。将灭绝极限和振幅与计算出的绝对幅度结合在一起，以设置主要成分质量的上限。这是通过考虑到主要质量主要序列星的光度不少的来实现的。对于26个可能的接触二进制组，初级质量限制为小于0.5太阳能，而某些系统的主要限制为低至0.35太阳能块。这些罕见的系统是更详细的观察目标的有趣目标，因为它们位于接触二元分布的低质量端，并且它们的形成和进化尚不清楚。
Possible M-type contact binaries were investigated by selecting W UMa-type variables with orbital periods below the 0.22-day cutoff. Gaia parallaxes were combined with Gaia and 2MASS photometry to obtain G and J-band absolute magnitudes of 674 red variable stars catalogued as contact binaries in the VSX database. The absolute magnitude of main sequence cool dwarfs varies strongly with spectral type, which was used to create a selection of 218 systems with primaries potentially of spectral types M0-M3. Lightcurves of the 46 systems with lowest near-infrared luminosities were inspected individually to confirm or reject the W UMa classification where possible. The extinction limits and amplitudes were combined with the calculated absolute magnitudes in order to set upper limits for the masses of the primary components. This is achieved via the consideration that the luminosity of the primary is no less than that of a main sequence star of the same mass. For 26 possible contact binaries the mass of the primary was limited to less than 0.5 solar masses with some systems having upper limits for the primary as low as 0.35 solar masses. These rare systems are intriguing targets for more detailed observations since they are on the low-mass end of the contact binary distribution and their formation and evolution are still unclear.
