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Seismic Detection of Boundaries of Stellar Convective Regions

  • Mário J.P.F.G. Monteiro (a1), Jørgen Christensen-Dalsgaard (a2) and Michael J. Thompson (a3)

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The edge of a convective region inside a star gives rise to a characteristic periodic signal in the frequencies of its global p-modes (e.g. [1], [4]), such that the frequencies ω are then essentially a smooth function of the mode order n plus a periodic component . Here the amplitude is , with A 1 and A 2 being values that depend weakly on frequency ω: A 1 is always present in general, but A 2 will be non-zero only if there is overshoot; is essentially the acoustical depth τ (i.e. the sound travel time) of the edge of the convection zone measured from the surface of the star; and Φ0 is a constant related to the phase of the eigenfunctions. To facilitate the comparison between different stars, we consider the amplitude evaluated at a fiducial frequency by defining . For the Sun, we chose as the reference frequency . If we take this value and scale it for other stars (using just a standard homology scaling for frequencies), we find .

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References

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[1] Christensen-Dalsgaard, J., Monteiro, M.J.P.F.G., Thompson, M.J. (1995), MNRAS 276, 283
[2] Kippenhahn, R., Weigert, A. (1990), Stellar Structure and Evolution, Springer–Verlag
[3] Kjeldsen, H., Bedding, T.R. (1995), A&A 293, 87
[4] Monteiro, M.J.P.F.G., Christensen-Dalsgaard, J., Thompson, M.J. (1994), A&A 283, 247

Seismic Detection of Boundaries of Stellar Convective Regions

  • Mário J.P.F.G. Monteiro (a1), Jørgen Christensen-Dalsgaard (a2) and Michael J. Thompson (a3)

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