### 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) |
---|---|

Pages (from-to) | 1919-1929 |

Number of pages | 11 |

Journal | Solar Physics |

Volume | 289 |

Issue number | 6 |

DOIs | |

State | Published - Jun 1 2014 |

### Fingerprint

### Keywords

- Helioseismology
- Magnetic fields
- Numerical methods
- Stellar models

### ASJC Scopus subject areas

- Astronomy and Astrophysics
- Space and Planetary Science

### Cite this

*Solar Physics*,

*289*(6), 1919-1929. https://doi.org/10.1007/s11207-013-0457-7

**Propagating Linear Waves in Convectively Unstable Stellar Models : A Perturbative Approach.** / Papini, E.; Gizon, Laurent; Birch, A. C.

Research output: Contribution to journal › Article

*Solar Physics*, vol. 289, no. 6, pp. 1919-1929. https://doi.org/10.1007/s11207-013-0457-7

}

TY - JOUR

T1 - Propagating Linear Waves in Convectively Unstable Stellar Models

T2 - A Perturbative Approach

AU - Papini, E.

AU - Gizon, Laurent

AU - Birch, A. C.

PY - 2014/6/1

Y1 - 2014/6/1

N2 - 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.

AB - 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.

KW - Helioseismology

KW - Magnetic fields

KW - Numerical methods

KW - Stellar models

UR - http://www.scopus.com/inward/record.url?scp=84893965989&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84893965989&partnerID=8YFLogxK

U2 - 10.1007/s11207-013-0457-7

DO - 10.1007/s11207-013-0457-7

M3 - Article

VL - 289

SP - 1919

EP - 1929

JO - Solar Physics

JF - Solar Physics

SN - 0038-0938

IS - 6

ER -