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Solar wind, mass and momentum losses during the solar cycle

Published online by Cambridge University Press:  12 August 2011

R. Pinto ,
S. Brun ,
L. Jouve  and
R. Grappin
R. Pinto
Affiliation:
Service d'Astrophysique - CEA Saclay/DSM/Irfu, 91191 Gif-sur-Yvette Cedex, France email: rui.pinto@cea.fr
S. Brun
Affiliation:
Service d'Astrophysique - CEA Saclay/DSM/Irfu, 91191 Gif-sur-Yvette Cedex, France email: rui.pinto@cea.fr
L. Jouve
Affiliation:
DAMTP, Wilberforce Road, CB30WA Cambridge, UK
R. Grappin
Affiliation:
LUTH Obs. Paris-Meudon, France & LPP Ecole Polytechnique, Palaiseau, France
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Abstract

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We study the connections between the sun's convection zone evolution and the dynamics of the solar wind and corona. We input the magnetic fields generated by a 2.5D axisymmetric kinematic dynamo code (STELEM) into a 2.5D axisymmetric coronal MHD code (DIP). The computations were carried out for an 11 year cycle. We show that the solar wind's velocity and mass flux vary in latitude and in time in good agreement with the well known time-latitude assymptotic wind speed diagram. Overall sun's mass loss rate, momentum flux and magnetic breaking torque are maximal near the solar minimum.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S271: Astrophysical Dynamics: From Stars to Galaxies , June 2010 , pp. 395 - 396
Copyright
Copyright © International Astronomical Union 2011

References

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