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The depth of the solar convection zone

Christensen-Dalsgaard, J., Gough, D. O., Thompson, M. J.·1991·The Astrophysical Journal

Abstract

The transition of the temperature gradient between being subadiabatic and adiabatic at the base of the solar convection zone gives rise to a clear signature in the sound speed. Helioseismic measurements of the sound speed therefore permit a determination of the location of the base of the convection zone. Two techniques were tested by applying them to artifical data, obtained by adding simulated noise to frequencies computed from two different solar models. The determinations appear to be relatively insensitive to uncertainties of the physics of the solar interior. From an analysis of observed frequencies of solar oscillation it is concluded that the depth of the solar convection zone is (0.287 + or - 0.003) solar radii.

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Metadata

Authors
Christensen-Dalsgaard, J., Gough, D. O., & Thompson, M. J.
Venue
The Astrophysical Journal
Published
1991-09
Volume
378
Pages
413
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
OpenAlex
W2091013083
Cited by
358
References
0
FWCI
15.73
Type
journal article
Language
en
Open access
closed

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CoChat. (2026). Citation check: The depth of the solar convection zone. https://app.cochat.ai/papers/10.1086/170441
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Christensen-Dalsgaard, J., Gough, D. O., & Thompson, M. J. (1991). The depth of the solar convection zone. The Astrophysical Journal. https://doi.org/10.1086/170441

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