### Abstract

Perturbation theory is used to calculate the frequency shift of acoustic modes of a homogeneous turbulent fluid and the frequency shifts of solar modes due to turbulent convection. For sound waves in a random flow, the fractional frequency shift is +(11/30)M^{2} in the long-wavelength limit, and the shift at short wavelengths is -2/3 M^{2}, where M is the average Mach number of the flow. In our model of solar convection, the low-degree f-mode shift is positive and unobservably small, whereas the fractional frequency shift at high degrees (l ≫ 500) is -M^{2}, where M is the Mach number of convection near the solar surface.

Original language | English (US) |
---|---|

Pages (from-to) | 458-464 |

Number of pages | 7 |

Journal | Astrophysical Journal |

Volume | 498 |

Issue number | 1 PART I |

DOIs | |

State | Published - 1998 |

### Fingerprint

### Keywords

- Sun: interior
- Sun: oscillations
- Turbulence

### ASJC Scopus subject areas

- Space and Planetary Science

### Cite this

*Astrophysical Journal*,

*498*(1 PART I), 458-464. https://doi.org/10.1086/305522

**Sound speed in a random flow and turbulent shifts of the solar eigenfrequencies.** / Gruzinov, Andrei V.

Research output: Contribution to journal › Article

*Astrophysical Journal*, vol. 498, no. 1 PART I, pp. 458-464. https://doi.org/10.1086/305522

}

TY - JOUR

T1 - Sound speed in a random flow and turbulent shifts of the solar eigenfrequencies

AU - Gruzinov, Andrei V.

PY - 1998

Y1 - 1998

N2 - Perturbation theory is used to calculate the frequency shift of acoustic modes of a homogeneous turbulent fluid and the frequency shifts of solar modes due to turbulent convection. For sound waves in a random flow, the fractional frequency shift is +(11/30)M2 in the long-wavelength limit, and the shift at short wavelengths is -2/3 M2, where M is the average Mach number of the flow. In our model of solar convection, the low-degree f-mode shift is positive and unobservably small, whereas the fractional frequency shift at high degrees (l ≫ 500) is -M2, where M is the Mach number of convection near the solar surface.

AB - Perturbation theory is used to calculate the frequency shift of acoustic modes of a homogeneous turbulent fluid and the frequency shifts of solar modes due to turbulent convection. For sound waves in a random flow, the fractional frequency shift is +(11/30)M2 in the long-wavelength limit, and the shift at short wavelengths is -2/3 M2, where M is the average Mach number of the flow. In our model of solar convection, the low-degree f-mode shift is positive and unobservably small, whereas the fractional frequency shift at high degrees (l ≫ 500) is -M2, where M is the Mach number of convection near the solar surface.

KW - Sun: interior

KW - Sun: oscillations

KW - Turbulence

UR - http://www.scopus.com/inward/record.url?scp=22044438124&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=22044438124&partnerID=8YFLogxK

U2 - 10.1086/305522

DO - 10.1086/305522

M3 - Article

VL - 498

SP - 458

EP - 464

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1 PART I

ER -