类太阳活动恒星表面黑子结构的多普勒成像（I）：技术

回顾了恒星表面结构多谱勒成像研究工作的发展历史,重点评述了该项技术在类太阳活动恒星研究领域的应用。介绍了该项技术在国际上的发展现状,给出了恒星表面黑子结构形态的多普勒成像技术的基本原理,讨论了该项技术对观测仪器、观测过程和观测对象的要求,并对未来这一领域的研究工作进行了展望。     

Rotation Profiles of Solar-like Stars with Magnetic Fields

We investigate the rotation profile of solar-like stars with magnetic fields. A diffu-sion coefficient of magnetic angular momentum transport is deduced. Rotating stellar models with different mass incorporating the coefficient are computed to give the rotation profiles. The total angular momentum of a solar model with only hydrodynamic instabilities is about 13 times larger than that of the Sun at the age of the Sun, and this model can not reproduce quasi-solid rotation in the radiative region. However, the solar model with magnetic fields not only can reproduce an almost uniform rotation in the radiative region, but also a total angular momentum that is consistent with the helioseismic result at the 3 σ level at the age of the Sun. The rotation of solar-like stars with magnetic fields is almost uniform in the radiative region, but for models of 1.2-1.5 M⊙, there is an obvious transition region between the convective core and the radiative region, where angular velocity has a sharp radial gradient, which is different from the rotation profile of the Sun and of massive stars with magnetic fields. The change of angular velocity in the transition region increases with increasing age and mass.