Radiative zone solar magnetic fields and g-modes
arXiv:astro-ph/0511708 · doi:10.1111/j.1365-2966.2006.10516.x
Abstract
We consider a generalized model of seismic-wave propagation that takes into account the effect of a central magnetic field in the Sun. We determine the g-mode spectrum in the perturbative magnetic field limit using a one-dimensional Magneto-Hydrodynamics (MHD) picture. We show that central magnetic fields of about 600-800 kG can displace the pure g-mode frequencies by about 1%, as hinted by the helioseismic interpretation of GOLF observations.
6 pages, 4 figures; final version to appear in MNRAS
References in corpus (5)
- First Results from KamLAND: Evidence for Reactor Anti-Neutrino Disappearance
- New Solar Seismic Models and the Neutrino Puzzle
- Large mixing angle oscillations as a probe of the deep solar interior
- Resonant origin for density fluctuations deep within the Sun: helioseismology and magneto-gravity waves
- Probing the internal magnetic field of slowly pulsating B-stars through g modes
Cited by in corpus (7)
- The quest for the solar g modes
- Effect of a fossil magnetic field on the structure of a young Sun
- Stability of Toroidal Magnetic Fields in Rotating Stellar Radiation Zones
- Probing the internal solar magnetic field through g-modes
- Magneto-Rotational Transport in the Early Sun
- Seismology of the Sun : Inference of Thermal, Dynamic and Magnetic Field Structures of the Interior
- Coriolis force corrections to g-mode spectrum in 1D MHD model