A Technique for Incorporating Large-scale Magnetic Fields Within Stellar Models: Implications for the Variability of the Solar Radius, Luminosity, and Pulsation Frequencies

Details A Technique for Incorporating Large-scale Magnetic Fields Within Stellar Models: Implications for the Variability of the Solar Radius, Luminosity, and Pulsation Frequencies A Technique for Incorporating Large-scale Magnetic Fields Within Stellar Models: Implications for the Variability of the Solar Radius, Luminosity, and Pulsation Frequencies

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.4408l&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #44.08; Bulletin of the American Astronomical Society, Vol. 26, p.1378

Astronomy and Astrophysics

Astronomy

Scientific paper

A set of physically consistent approximations are employed to include the effects of magnetic fields within the equations of stellar structure. A series of solar models are then constructed with large-scale (~0.1R_sun), intense (~10(6) gauss) magnetic fields. The results of such models are then compared to measurements of changes in the solar radius (from the Solar Disk Sextant Experiment) and changes in the solar p-mode frequencies in order to determine if such fields are associated with the solar cycle. This work was supported in part by an appointment to the Global Change Distinguished Postdoctoral Fellowships sponsored by the U.S. Department of Energy, Office of Health and Enviromental Research, and administered by the Oak Ridge Institute for Science and Education.

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