Overview of Solar Luminosity Variation Mechanisms

Details Overview of Solar Luminosity Variation Mechanisms Overview of Solar Luminosity Variation Mechanisms

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp31b01s&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SP31B-01 INVITED

Physics

1600 Global Change (New Category), 7524 Magnetic Fields, 7537 Solar And Stellar Variability, 7538 Solar Irradiance, 7544 Stellar Interiors And Dynamo Theory

Scientific paper

The theory of stellar structure can be used to put constraints on proposed mechanisms for the irradiance variations associated with the solar cycle. Changes in the emissivity of the solar surface turn out to be particularly effective. Such changes are produced by sunspots and the small scale magnetic field, either directly (spots being dark, for example) or indirectly through their effect on the convective flow in their immediate vicinity. They can account for most of the observed variation. Sources of variation deeper below the solar surface either have much smaller effects, or require ad-hoc new physics. Helioseismology may soon be able to distinguish between surface emissivity changes and interior sources, since their predicted effects on p-mode frequencies and travel times tend to have opposite sign.

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