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Differential Rotation of the Sun from helioseismology and magnetic field study.

Published online by Cambridge University Press:  21 October 2010

Elena Gavryuseva  and
Susanne Höfner
Elena Gavryuseva
Affiliation:
Institute for Nuclear Research of the Academy of Sciences of Russia, Moscow, Russia email: [email protected]
Susanne Höfner
Affiliation:
Institute for Nuclear Research of the Academy of Sciences of Russia, Moscow, Russia email: [email protected]
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Abstract

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Differential rotational rate of the large scale magnetic field and its temporal dependence has been evidenced at different latitudes through activity cycles 21-23. Rotational rate of the magnetic field at the latitudes above 55 degrees doesn't getting slower. Torsional waves with 11-year period are clearly seen in the magnetic field rotation. Rotation is slower where and when the magnetic field is getting stronger.

The time of the magnetic field emergence to the photosphere was estimated.

It was revealed the existence of quasi-stable over 30 years exceptionally regular and symmetric in the both hemispherest longitudinal structure. This structure is originated from the tachocline zone rotating like a rigid body with the rotation rate corresponding to the rotation in the photosphere on the 55-60 degrees of the helio-latitudes.

Keywords

Sunmagnetic fieldrotationlongitudinal structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 355 - 356
Copyright
Copyright © International Astronomical Union 2010

References

Gavryuseva, E., Godoli, G. 2004, Physics and Chemistry of the Earth, v. 31, iss. 1–3, pp. 68–76.Google Scholar
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Gavryuseva, E. 2006, ibid, pp. 65–66CrossRefGoogle Scholar
Gavryuseva, E. 2007, AIPGoogle Scholar
Gavryuseva, E. 2007, AIPGoogle Scholar