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Probing the internal solar magnetic field through g-modes

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Probing the internal solar magnetic field through g-modes

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dc.contributor.author Rashba, Timur I.
dc.contributor.author Semikoz, Victor B.
dc.contributor.author Turck-Chièze, Sylvaine
dc.contributor.author Furtado Valle, José Wagner
dc.date.accessioned 2015-09-30T10:08:29Z
dc.date.available 2015-09-30T10:08:29Z
dc.date.issued 2007
dc.identifier.citation Rashba, Timur I. Semikoz, Victor B. Turck-Chièze, Sylvaine Furtado Valle, José Wagner 2007 Probing the internal solar magnetic field through g-modes Monthly Notices of the Royal Astronomical Society 377 1 453 458
dc.identifier.uri http://hdl.handle.net/10550/47478
dc.description.abstract 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.
dc.language.iso eng
dc.relation.ispartof Monthly Notices of the Royal Astronomical Society, 2007, vol. 377, num. 1, p. 453-458
dc.subject Física
dc.title Probing the internal solar magnetic field through g-modes
dc.type journal article es_ES
dc.date.updated 2015-09-30T10:08:29Z
dc.identifier.doi 10.1111/j.1365-2966.2007.11626.x
dc.identifier.idgrec 043137
dc.rights.accessRights open access es_ES

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