Energy flow continuity in solar active regions

Details Energy flow continuity in solar active regions Energy flow continuity in solar active regions

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984siva.work..125s&link_type=abstract

In NASA, Washington Solar Irradiance Variations on Active Region Time Scales p 125-131 (SEE N84-27635 17-92)

Computer Science

2

Convective Flow, Flow Distribution, Solar Activity, Solar Atmosphere, Stellar Models, Sunspot Cycle, Sunspots, Computerized Simulation, Faculae, Solar Magnetic Field, Stellar Luminosity, Temperature Gradients

Scientific paper

The models for sunspots are combined into an active region model with consideration for the energy flow beneath active regions. An apparent average energy balance exists between the sunspot deficit and the facular excess, i.e., no 11 year variations in solar luminosity associated with the activity centers. This is seen as a consequence of the upper convection zone's inability to store these significant amounts of energy for periods greatly in excess of weeks. This view is supported by observed active region behavior and detailed numerical modelling. Increases in facular and spot brightness are nearly commensurate, with the faculae outlasting the spots on time scales of the order of weeks to a couple of months. Foukal finds the radiation (deficit from a sunspot blocking model) recovers slowly on a timescale of approximately 83 days.

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