阿尔芬波驱动的太阳风到红巨星的演化
Evolution of Alfven wave-driven solar winds to red giants
摘要：
在这次演讲中，我们介绍了最近针对太阳风和恒星风加速进行的全球一维MHD模拟结果。我们施加横向光球运动对应的粒化，产生传出阿尔芬波。在密度分层大气中，阿尔芬波通过三波耦合和直接模式转换有效地消散为压缩波。我们指出，日冕加热和太阳风加速在开放的磁场区是自然的结果，在表面（光球）的磁场的足点波动。我们还讨论了由\Alfven波驱动的红巨星的风，侧重于与太阳风不同的方面。我们表明，红巨星风是高度结构化的间歇性磁化热泡嵌入在冷色球材料。
英文摘要：
In this talk we introduce our recent results of global 1D MHD simulations for the acceleration of solar and stellar winds. We impose transverse photospheric motions corresponding to the granulations, which generate outgoing Alfven waves. The Alfven waves effectively dissipate by 3-wave coupling and direct mode conversion to compressive waves in density-stratified atmosphere. We show that the coronal heating and the solar wind acceleration in the open magnetic field regions are natural consequence of the footpoint fluctuations of the magnetic fields at the surface (photosphere). We also discuss winds from red giant stars driven by \Alfven waves, focusing on different aspects from the solar wind. We show that red giants wind are highly structured with intermittent magnetized hot bubbles embedded in cool chromospheric material.
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