Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...466.1078r&link_type=abstract
Astrophysical Journal v.466, p.1078
Astronomy and Astrophysics
Astronomy
26
Sun: Interior, Sun: Magnetic Fields, Sun: Rotation
Scientific paper
A solar spin-down model is developed with the differential rotation in the convective envelope included. The model works with an internal magnetic field in the radiative core. The question is addressed whether the present profiles in radius and latitude of the angular velocity derived by helioseismology can be reproduced by following the spin-down over the solar lifetime. In spite of the high efficiency of the magnetic transport of the angular momentum, a positive answer is only possible if the viscosity is strongly amplified compared to its microscopic value.
The model is basically insensitive to the amplitude of the internal poloidal field when the field strength becomes larger than about 10-3 G. The magnetic field geometry is, however, an important factor. The helioseismology inversions are reproduced only with the poloidal field fully contained within the core. The dependence on the initial rotation rate is also small. After ˜1 Gyr, the stars with strongly different initial rotation rates settle on practically the same spin-down track.
Kitchatinov Leonid L.
Ruediger Guenther
No associations
LandOfFree
The Internal Solar Rotation in Its Spin-down History does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The Internal Solar Rotation in Its Spin-down History, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Internal Solar Rotation in Its Spin-down History will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1448864