Origin and structure of magnetic fields in cool stars (A16)

导电流体在湍流运动中产生的磁通量对于理解大雷诺数下的磁流体湍流具有重要意义。该项目尝试了一种跨学科的方法来解决恒星表面磁性的天体物理和湍流方面，一方面使用近表面恒星磁对流的辐射MHD模拟，另一方面通过获得从类太阳恒星到极低质量恒星的可靠的磁场定量观测。该项目由两部分组成：第一部分继续使用MURaM程序成功地模拟恒星磁场的预期特征，第二部分使用不同的方法观测低质量恒星中的磁场，包括国际BCool计划中的合作和对300颗恒星的分析，即Car-Menes计划的1万多个光谱。

The generation of magnetic flux in electrically conducting fluids in turbulent motion is of fundamental importance for understanding magnetohydrodynamic turbulence at large Reynolds numbers. This Project ventures an interdisciplinary approach to address the astrophysical and turbulence aspects of stellar surface magnetism by using radiative MHD simulations of nearsurface stellar magnetoconvection on the one hand, and by obtaining reliable quantitative observations of magnetic fields in stars from sun-like to very-low mass stars on the other. The project consists of two parts: the first continuing our successful simulations of expected signatures of stellar magnetic fields using the MURaM code, the second observing magnetic fields in low-mass stars using different approaches including collaborations in the international BCool project and analysis of 300 stars, i.e., more than ten thousand spectra from the CAR-MENES project.