亚矮星B双星PG 0101+039的潮汐同步
Tidal synchronization of the subdwarf B binary PG 0101+039
摘要：
潮汐锁定自转是一个经常应用的假设，它有助于测量密近双星中不可见的致密伴星的质量。同步时间的计算受到很大的不确定性的影响，特别是对于辐射包络要求观测约束的恒星。我们的目标是验证二进制PG 0101+039的潮汐锁定旋转，亚矮星B星+白矮星二进制从它的微小（0.025%）的光变化测量与MOST卫星（兰德尔等，2005年）。二进制参数来自质量函数，表观旋转和表面重力PG 0101+039假设规范质量为0.47钼和潮汐锁定旋转。然后合成光变曲线，发现与观察到的振幅很好地匹配。我们验证了光的变化是由于椭球变形和潮汐同步建立PG 0101+039。我们的结论是，这一假设应持有所有sdB双星的轨道周期小于半天。因此，质量可以从太微弱而无法测量微小光变化的系统中导出。
英文摘要：
Tidally locked rotation is a frequently applied assumption that helps to measure masses of invisible compact companions in close binaries. The calculations of synchronization times are affected by large uncertainties in particular for stars with radiative envelopes calling for observational constraints. We aim at verifying tidally locked rotation for the binary PG 0101+039, a subdwarf B star + white dwarf binary from its tiny (0.025 %) light variations measured with the MOST satellite (Randall et al. 2005). Binary parameters were derived from the mass function, apparent rotation and surface gravity of PG 0101+039 assuming a canonical mass of 0.47 Mo and tidally locked rotation. The light curve was then synthesised and was found to match the observed amplitude well. We verified that the light variations are due to ellipsoidal deformation and that tidal synchronization is established for PG 0101+039. We conclude that this assumption should hold for all sdB binaries with orbital periods of less than half a day. Hence the masses can be derived from systems too faint to measure tiny light variations.
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