Contribution of the Solar MagneticField on Gravitational Moments

Studies of the solar magnetic eld is one of the key method of explaining important phenomena found in the sun. in order to determine the contribution of the magnetic eld 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 eld, such as the eruptions of the ux tubes, are the source of the poloidal eld, 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 gures of the sun [2]. in this paper, this last theory was used, but adding the magnetic eld contribution. different estimates were obtained for the successive jn (n = 2, 4, 6, 8), in terms of different values of bcr (the critical eld), where the maximum value of the toroidal magnetic eld in the gl is 1:5 x bcr.