Constraints on the Solar Internal Magnetic Field from a Buoyancy Driven Solar Dynamo |
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| Authors: | Dibyendu Nandy |
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| Institution: | (1) Department of Physics, Indian Institute of Science, Bangalore, 560012, India |
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| Abstract: | We report here results from a dynamo model developed on the lines of the Babcock-Leighton idea that the poloidal field is
generated at the surface of the Sun from the decay of active regions. In this model magnetic buoyancy is handled with a realistic
recipe – wherein toroidal flux is made to erupt from the overshoot layer wherever it exceeds a specified critical field B
c (105 G). The erupted toroidal field is then acted upon by the α-effect near the surface to give rise to the poloidal field. In
this paper we study the effect of buoyancy on the dynamo generated magnetic fields. Specifically, we show that the mechanism
of buoyant eruption and the subsequent depletion of the toroidal field inside the overshoot layer, is capable of constraining
the magnitude and distribution of the magnetic field there. We also believe that a critical study of this mechanism may give
us new information regarding the solar interior and end with an example, where we propose a method for estimating an upper
limit of the difusivity within the overshoot layer.
This revised version was published online in July 2006 with corrections to the Cover Date. |
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| Keywords: | Sun Dynamo Magnetic Buoyancy Overshoot Tachocline |
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