Seismic Detection of Boundaries of Stellar Convective Regions

Mário J.P.F.G. Monteiro; Jørgen Christensen-Dalsgaard; Michael J. Thompson

doi:10.1017/S0074180900238850

Seismic Detection of Boundaries of Stellar Convective Regions

Published online by Cambridge University Press: 08 February 2017

Mário J.P.F.G. Monteiro ,

Jørgen Christensen-Dalsgaard and

Michael J. Thompson

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Mário J.P.F.G. Monteiro: Affiliation:
DMA-FCUP and CAUP, Universidade do Porto, Portugal
Jørgen Christensen-Dalsgaard: Affiliation:
TAC and Inst. Fysik og Astronomi, Aarhus Universitet, Denmark
Michael J. Thompson: Affiliation:
Astronomy Unit, QMW, University of London, England

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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 A1 and A2 being values that depend weakly on frequency ω: A1 is always present in general, but A2 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 .