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Paper Information

Journal:   SCIENTIA IRANICA   FEBRUARY 2008 , Volume 15 , Number 1; Page(s) 144 To 149.
 
Paper: 

CONTRIBUTION OF THE SOLAR MAGNETIC FIELD ON GRAVITATIONAL MOMENTS

 
 
Author(s):  AJABSHIRIZADEH A.*, ROZELOT J.P., FAZEL Z.
 
* RESEARCH INSTITUTE FOR ASTRONOMY & ASTROPHYSICS OF MARAGHE, MARAGHE, I.R. IRAN
 
Abstract: 
Studies of the solar magnetic field are one of the key method of explaining important phenomena found in the Sun. In order to determine the contribution of the magnetic field on the solar outer shape, here, the dynamo model of the Babcock-Leighton type [1] is considered. This model explains that the surface eruptions of the toroidal magnetic field, such as the eruptions of the ux tubes, are the source of the poloidal field, whereas, generation of the toroidal field takes place in a thin, deep seated layer, called the Generating Layer (GL), at the bottom of the Solar Convection Zone (SCZ). To calculate the indicating quantity of the solar shape, i.e. the gravitational moments, Jn, several methods can be used: Stellar equations combined with a differential rotation model, inversion techniques applied to helioseismology and based on the Von Zeipel theorem, the theory of figures of the Sun [2]. In this paper, this last theory was used, but adding the magnetic field contribution. Different estimates were obtained for the successive Jn (n = 2, 4, 6, 8), in terms of different values of Bcr (the critical field), where the maximum value of the toroidal magnetic field in the GL is 1.5 × Bcr.
 
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