Abstract
AbstractMagnetic activity of stars like the Sun evolves in time because of spin-down owing to angular momentum removal by a magnetized stellar wind. These magnetic fields are generated by an internal dynamo driven by convection and differential rotation. Spin-down therefore converges at an age of about 700 Myr for solar-mass stars to values uniquely determined by the stellar mass and age. Before that time, however, rotation periods and their evolution depend on the initial rotation period of a star after it has lost its protostellar/protoplanetary disk. This non-unique rotational evolution implies similar non-unique evolutions for stellar winds and for the stellar high-energy output. I present a summary of evolutionary trends for stellar rotation, stellar wind mass loss and stellar high-energy output based on observations and models.
Publisher
Springer Science and Business Media LLC
Subject
Space and Planetary Science,Astronomy and Astrophysics
Reference57 articles.
1. V.S. Airapetian, A.V. Usmanov, Astrophys. J. 817, L24 (2016)
2. V.S. Airapetian, A. Glocer, G. Gronoff et al., Nat. Geosci. 9, 452 (2016)
3. M. Audard, M. Güdel, J.J. Drake, V.L. Kashyap, Astrophys. J. 541, 396 (2000)
4. T.R. Ayres, J. Geophys. Res. 102, 1641 (1997)
5. L. Biermann, Z. Astrophys. 29, 274 (1951)
Cited by
12 articles.
订阅此论文施引文献
订阅此论文施引文献,注册后可以免费订阅5篇论文的施引文献,订阅后可以查看论文全部施引文献