论文标题
星星的活跃生活：旋转和XUV的完整描述F，G，K和M矮人
The active lives of stars: a complete description of rotation and XUV evolution of F, G, K, and M dwarfs
论文作者
论文摘要
目标。我们研究了F，G，G，K和M Dwarfs的旋转和高能量X射线，极端紫外线（EUV）和Ly-Alpha发射的演变，质量在0.1至1.2 MSUN之间，并提供了我们的进化代码，并提供了一套可用的进化轨道，以在Planetare Materne Itches研究中使用。 方法。我们开发了一个由年轻恒星簇中观察到的旋转分布约束的物理旋转模型。使用旋转，X射线，EUV和Ly-Alpha测量值，我们得出了高能发射对恒星参数的依赖性的经验关系。我们对X射线演化的描述是使用年轻簇中X射线分布的测量来验证的。 结果。恒星的X射线，EUV和Ly-Alpha的演化取决于其质量和初始旋转速率，初始旋转对下质量恒星的重要性不太重要。在所有年龄段的年龄上，太阳能巨星的X射线明显比较低的质量恒星和恒星比快速旋转器的活跃时间高于慢速旋转器的恒星更长。在所有进化阶段，由于其较长的进化时间尺度绕较低的质量恒星运行时，可居住区行星会获得更高的X射线和EUV通量。耀斑的速率遵循类似的进化趋势，较高的质量恒星的燃烧频率比所有年龄段的质量恒星都要高，尽管在绕下质量恒星绕的易居区的行星可能会受到耀斑的影响更大。 结论。我们的结果表明，单个衰减法律不足以描述恒星活动的演变，并强调了基于旋转演变的更全面描述的需求，包括短期变异性的影响。当绕较高的质量恒星运行时，距宿主恒星相似的轨道距离行星在其一生中获得了更多的X射线和EUV能量。 （抽象不完整）
Aims. We study the evolution of rotation and high energy X-ray, extreme ultraviolet (EUV), and Ly-alpha emission for F, G, K, and M dwarfs, with masses between 0.1 and 1.2 Msun, and provide our evolutionary code and a freely available set of evolutionary tracks for use in planetary atmosphere studies. Methods. We develop a physical rotational evolution model constrained by observed rotation distributions in young stellar clusters. Using rotation, X-ray, EUV, and Ly-alpha measurements, we derive empirical relations for the dependences of high energy emission on stellar parameters. Our description of X-ray evolution is validated using measurements of X-ray distributions in young clusters. Results. A star's X-ray, EUV, and Ly-alpha evolution is determined by its mass and initial rotation rate, with initial rotation being less important for lower mass stars. At all ages, solar mass stars are significantly more X-ray luminous than lower mass stars and stars that are born as rapid rotators remain highly active longer than those born as slow rotators. At all evolutionary stages, habitable zone planets receive higher X-ray and EUV fluxes when orbiting lower mass stars due to their longer evolutionary timescales. The rates of flares follow similar evolutionary trends with higher mass stars flaring more often than lower mass stars at all ages, though habitable zone planets are likely influenced by flares more when orbiting lower mass stars. Conclusions. Our results show that single decay-laws are insufficient to describe stellar activity evolution and highlight the need for a more comprehensive description based on the evolution of rotation, including also the effects of short-term variability. Planets at similar orbital distances from their host stars receive significantly more X-ray and EUV energy over their lifetimes when orbiting higher mass stars. (abstract incomplete)
