The observation of g-mode candidates by the SoHO mission opens the possibility of probing the internal structure of the solar radiative zone ( RZ ) and the solar core more directly than possible via the use of the p-mode helioseismology data .
We study the effect of rotation and RZ magnetic fields on g-mode frequencies .
Using a self-consistent static MHD magnetic field model we show that a 1 % g-mode frequency shift with respect to the Solar Seismic Model ( SSeM ) prediction , currently hinted in the GOLF data , can be obtained for magnetic fields as low as 300 kG , for current measured modes of radial order n = -20 .
On the other hand , we also argue that a similar shift for the case of the low order g-mode candidate ( l = 2 , n = -3 ) frequencies can not result from rotation effects nor from central magnetic fields , unless these exceed 8 MG .