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Topology of convection beneath the solar surface
Abstract
It is shown that the topology of convection beneath the solar surface is dominated by effects of stratification. Convection in a strongly stratified medium has: (1) gentle expanding structureless warm upflows and (2) strong converging filamentary cool downdrafts. The horizontal flow topology is cellular, with a hierarchy of cell sizes. The small density scale height in the surface layers forces the formation of the solar granulation, which is a shallow surface phenomenon. Deeper layers support successively larger cells. The downflows of small cells close to the surface merge into filamentary downdrafts of larger cells at greater depths, and this process is likely to continue through most of the convection zone. Radiative cooling at the surface provides the entropy-deficient material which drives the circulation.
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Citations
Cited by
Simulations of Solar Granulation. I. General Properties
Stein, R. F., & Nordlund, A. (1998) · The Astrophysical Journal · doi:10.1086/305678 · Cited by 744
Self-citationClyne, J., Mininni, P., Norton, A., & Rast, M. (2007) · New Journal of Physics · doi:10.1088/1367-2630/9/8/301 · Cited by 286
TURBULENT CONVECTION IN STELLAR INTERIORS. III. MEAN-FIELD ANALYSIS AND STRATIFICATION EFFECTS
Viallet, M., Meakin, C., Arnett, D., & Mocák, M. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/769/1/1 · Cited by 106
Metadata
- Authors
- Stein, R. F., & Nordlund, A.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 1989-07
- Volume
- 342
- Pages
- L95
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2073847196
- Cited by
- 301
- References
- 0
- FWCI
- 21.96
- Type
- journal article
- Language
- en
- Open access
- closed
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- Stein, R. F., & Nordlund, A. (1989). Topology of convection beneath the solar surface. The Astrophysical Journal. https://doi.org/10.1086/185493
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