Abstract
Linear time-domain simulations of acoustic oscillations are unstable in the stellar convection zone. To overcome this problem it is customary to compute the oscillations of a stabilized background stellar model. The stabilization affects the result, however. Here we propose to use a perturbative approach (running the simulation twice) to approximately recover the acoustic wave field while preserving seismic reciprocity. To test the method we considered a 1D standard solar model. We found that the mode frequencies of the (unstable) standard solar model are well approximated by the perturbative approach within 1 μHz for low-degree modes with frequencies near 3 mHz. We also show that the perturbative approach is appropriate for correcting rotational-frequency kernels. Finally, we comment that the method can be generalized to wave propagation in 3D magnetized stellar interiors because the magnetic fields have stabilizing effects on convection.
Original language | English (US) |
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Pages (from-to) | 1919-1929 |
Number of pages | 11 |
Journal | Solar Physics |
Volume | 289 |
Issue number | 6 |
DOIs | |
State | Published - Jun 2014 |
Keywords
- Helioseismology
- Magnetic fields
- Numerical methods
- Stellar models
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science