Limits on magnetic fields that produce sunspots

Details Limits on magnetic fields that produce sunspots Limits on magnetic fields that produce sunspots

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993basi...21..371d&link_type=abstract

Astronomical Society of India, Bulletin (ISSN 0304-9523), vol. 21, no. 3-4, p. 371-372

Astronomy and Astrophysics

Astronomy

Solar Convection (Astronomy), Solar Magnetic Field, Solar Prominences, Stellar Models, Sunspots, Coriolis Effect, Helioseismology, Magnetic Field Configurations, Magnetic Flux

Scientific paper

The solar dynamo is believed to operate in a thin stable region at the bottom of the convection zone and the bipolar magnetic regions (BMRs) that we see on the surface are produced by magnetic flux tubes generated there. These flux tubes emerge as Omega shaped loops (Parker 1955, 1979) due to magnetic buoyancy, and the regions where they intersect the surface are called BMRs. These BMRs obey Joy's law (Hale et al. 1919; Wang & Sheeley 1989, 1991; Howard 1992), which states that the line joining the two poles of BMR makes an angle with the latitudinal line, called the tilt, which increases with increase in latitude and the p-spot (preceding region of the BMR which is Westward) is closer to the equator. We give a theoretical model for these tilts (D'Silva & Choudhuri 1993). We also show that if the BMRs produced by flux tubes emerging from the bottom of the convection zone have to exhibit the tilts measured by observations (Wang & Sheeley 1989, 1991; Howard 1992), then the field strength at the bottom of the convection zone has to lie between 60 and 160 kG. For fields stronger than 160 kG, magnetic buoyancy dominates over Coriolis force and the tilts produced are very small compared to the observed values. Whereas, for fields weaker than 60 kG, Coriolis force dominates over buoyancy and makes them emerge at very high latitudes, well above the typical sunspot latitudes.

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