Convection and magnetic fields in stars

Details Convection and magnetic fields in stars Convection and magnetic fields in stars

Feb 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...243..945g&link_type=abstract

Astrophysical Journal, Part 1, vol. 243, Feb. 1, 1981, p. 945-953.

Other

175

Convection, Late Stars, Magnetic Flux, Magnetohydrodynamics, Stellar Atmospheres, Stellar Magnetic Fields, Boussinesq Approximation, Buoyancy, Chromosphere, M Stars, Solar Atmosphere, Solar Magnetic Field, Stellar Spectra, Sunspots, Turbulence

Scientific paper

Recent observations have demonstrated the unity of the study of stellar and solar magnetic fields. Results from numerical experiments on magnetoconvection are presented and used to discuss the concentration of magnetic flux into isolated ropes in the turbulent convective zones of the sun or other late-type stars. Arguments are given for siting the solar dynamo at the base of the convective zone. Magnetic buoyancy leads to the emergence of magnetic flux in active regions, but weaker flux ropes are shredded and dispersed throughout the convective zone. The observed maximum field strengths in late-type stars should be comparable with the field that balances the photospheric pressure.

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