Excitation of solar oscillation gravity modes by magnetic torque

Details Excitation of solar oscillation gravity modes by magnetic torque Excitation of solar oscillation gravity modes by magnetic torque

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...151...47d&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 151, no. 1, Oct. 1985, p. 47-51. CNR-supported research.

Astronomy and Astrophysics

Astrophysics

6

Gravity Waves, Helioseismology, Solar Magnetic Field, Solar Oscillations, Stellar Cores, Amplitudes, Magnetohydrodynamic Turbulence, Radial Velocity, Torque

Scientific paper

Observed radial velocity amplitudes are used to determine the energies of the identified solar gravity modes. The energies of some modes are of the same order of magnitude of the total energy of the convective motions in the solar envelope. Therefore the authors argue that this fact rules out the possibility of direct or indirect excitation of these modes of convection. After having reviewed some possibilities for a driving mechanism acting in the solar core, they suggest that the most plausible driving mechanism is the effect of the magnetic torque caused by the presence of a global magnetic field and mild turbulence in the core.

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