从恒星日冕到陀螺年代学：理论与观测探索
From Stellar Coronæ to Gyrochronology: a theoretical and observational exploration
摘要：
上下文恒星的自旋是一个复杂过程的结果，涉及旋转，发电机，风和磁性。对类太阳恒星的多波长观测揭示了它们的自转、X射线光度、质量损失和磁性之间可能存在的关系。这些对冷恒星的日冕和恒星风施加了很强的约束。目的。我们的目标是提供幂律处方的质量损失的恒星，他们的磁场，和他们的基础日冕的密度和温度，是兼容的观测约束自旋下降。方法.我们联系的磁场和质量损失率从风力矩制定与恒星旋转周期的分布在疏散星团和Skumanich法律。给定一个风模型和辐射损失的X射线光度的表达式，我们通过假设不同的物理参数将闭合环连接到冕洞来约束冕属性。结果我们发现，磁场和质量损失涉及到一个一对一的对应关系，从自旋下降的考虑。我们表明，一个磁场取决于Rossby数和恒星质量是需要保持一致的自旋下降模型。从我们的形式主义获得的磁场和质量损失率的估计与统计研究以及个人的观察是一致的，并给出了新的线索来约束磁场旋转关系。我们推导出的一组标度律可以广泛应用于从PMS到MS结束的冷恒星，并允许与迄今为止所有观测约束一致的恒星风建模。
英文摘要：
Context. Stellar spin-down is the result of a complex process involving rotation, dynamo, wind and magnetism. Multi-wavelength surveys of solar-like stars have revealed the likely existence of relationships between their rotation, X-ray luminosity, mass-losses and magnetism. Those impose strong constraints on the corona and wind of cool stars. Aims. We aim to provide power-law prescriptions of the mass-loss of stars, of their magnetic field, and of their base coronal density and temperature that are compatible with their observationally-constrained spin-down. Methods. We link the magnetic field and the mass-loss rate from a wind torque formulation in agreement with the distribution of stellar rotation periods in open clusters and the Skumanich law. Given a wind model and an expression of the X-ray luminosity from radiative losses, we constrain the coronal properties by assuming different physical scenarii linking closed loops to coronal holes. Results. We find that the magnetic field and the mass loss are involved in a one-to-one correspondence constrained from spin-down considerations. We show that a magnetic field depending on both the Rossby number and the stellar mass is required to keep a consistent spin-down model. The estimates of the magnetic field and the mass-loss rate obtained from our formalism are consistent with statistical studies as well as individual observations and give new leads to constrain the magnetic field-rotation relation. The set of scaling-laws we derived can be broadly applied to cool stars from the PMS to the end of the MS, and allow for a stellar wind modelling consistent with all the observational constraints available to date.
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