## Abstract

Numerical solutions of the general time-dependent gas-dynamical equations in linear adiabatic approximation are given for initial conditions imitating: (a) a central perturbation, (b) a boundary perturbation (in the convective envelope), and (c) a 'shrinking' of the Sun as a whole. For a variety of models of the Sun it is found that at the surface the radial component v_{r} of velocity is much greater than the tangential component v_{t}, and that the period T of stationary oscillations does not exceed 131^{m}. The appearance at the surface of a g mode with period 160^{m} is found to be improbable. With the initial conditions adopted, a propagating wave is produced which is reflected successively from the centre to the periphery and back, producing 5-min oscillations at the surface of the Sun. Expansion of this wave into separate modes leads to a power spectrum qualitatively similar to that observed.

Original language | English (US) |
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Pages (from-to) | 323-329 |

Number of pages | 7 |

Journal | Solar Physics |

Volume | 82 |

Issue number | 1-2 |

DOIs | |

State | Published - Jan 1983 |

Externally published | Yes |

## All Science Journal Classification (ASJC) codes

- Astronomy and Astrophysics
- Space and Planetary Science