Magnetic Network Formation Due to Sub-arcsecond Flux Processing

Details Magnetic Network Formation Due to Sub-arcsecond Flux Processing Magnetic Network Formation Due to Sub-arcsecond Flux Processing

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.9213l&link_type=abstract

American Astronomical Society Meeting 210, #92.13; Bulletin of the American Astronomical Society, Vol. 39, p.210

Astronomy and Astrophysics

Astronomy

1

Scientific paper

Kinematic models of solar magnetic network formation typically employ the breakup of ephemeral regions by granular and supergranular flow. We show that the coalescence of sub-arcsecond-scale magnetic flux concentrations into features detectable with MDI is responsible for injecting as much flux into the magnetic network as the published emergence rate of ephemeral regions. We also show that the few fresh bipoles we do detect have no preferential alignment, and thus violate Joy's law at the arcsecond scale. These two items suggest that at least half of the flux that makes its way into the network has been processed at spatial scales below 1 arcsecond, indicative of a local dynamo.

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