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Evolution of Alfvén wave-driven solar winds to red giants

Published online by Cambridge University Press:  01 September 2007

Takeru K. Suzuki
Takeru K. Suzuki*
Affiliation:
School of Arts and Sciences, University of Tokyo, Komaba, Meguro, Tokyo, Japan153-8902 email: stakeru@ea.c.u-tokyo.ac.jp
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Abstract

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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 Alfvén waves. The Alfvén 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 Alfvén 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.

Keywords

wavesMHDSun: photosphereSun: chromosphereSun: Coronasolar windstars: chromospheresstars: coronaestars: magnetic fieldsstars: mass lossstars: late-type
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S247: Waves & Oscillations in the Solar Atmosphere: Heating and Magneto-Seismology , September 2007 , pp. 201 - 207
Copyright
Copyright © International Astronomical Union 2008

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