Asteroseismology and dynamos in solar-like stars (A18)

在这个项目中，我们的目标是了解表面温度低于~6500K的冷恒星外层的湍流对流及其影响。为此，我们将研究恒星旋转，即所谓的表面效应，它被认为（至少部分地）起源于对流和波之间的各种相互作用，以及颗粒状，这是由近表面对流引起的表面图案。来自开普勒宇宙飞船的长光度时间序列数据将用于测量旋转分裂、颗粒化的特征时间尺度和幅度，并对多颗恒星进行结构反演和模型拟合。利用MURaM代码将观测结果与真实的对流模拟进行比较。

In this project, we aim to understand the turbulent convection and its effects in the outer layers of cool stars with surface temperatures below ~6500K. To this end, we will study stellar rotation, the so-called surface effect, which is thought to originate (at least partly) from various interactions between convection and waves, as well as granulation, which is the surface pattern caused by the near surface convection. Long photometric timeseries data from the Kepler spacecraft will be used to measure rotational splittings, characteristic time scales and amplitudes of granulation, and perform structure inversions and model fits on multiple stars. The observational results will be confronted with realistic convection simulations using the MURaM code.