Open AccessProbing the internal solar magnetic field through g modes
Author(s) -
Rashba T. I.,
Semikoz V. B.,
TurckChièze S.,
Valle J. W. F.
Publication year - 2007
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2007.11626.x
Subject(s) - physics , helioseismology , solar core , magnetic field , magnetohydrodynamics , oscillation (cell signaling) , radiative transfer , astrophysics , mode (computer interface) , computational physics , rotation (mathematics) , solar rotation , heliospheric current sheet , interplanetary magnetic field , solar physics , solar wind , optics , geometry , mathematics , quantum mechanics , solar neutrino , biology , nuclear physics , computer science , neutrino , genetics , operating system , neutrino oscillation
The observation of g‐mode candidates by the Solar and Heliospheric Observatory (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 magnetohydrodynamics magnetic field model, we show that a 1 per cent g‐mode frequency shift with respect to the Solar Seismic Model (SSEM) prediction, currently hinted in the Global Oscillation at Low Frequencies (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 cannot result from rotation effects nor from central magnetic fields, unless these exceed 8 MG.