dc.creator |
Guenther, David B. |
|
dc.creator |
Li, L. H. |
|
dc.creator |
Robinson, F. J. |
|
dc.creator |
Demarque, P. |
|
dc.creator |
Sofia, S. |
|
dc.date.accessioned |
2015-04-02T14:33:38Z |
|
dc.date.available |
2015-04-02T14:33:38Z |
|
dc.date.issued |
2002-03-10 |
|
dc.identifier.issn |
0004-637X |
|
dc.identifier.uri |
http://library2.smu.ca/xmlui/handle/01/26023 |
|
dc.description |
Publisher's version/PDF |
en_CA |
dc.description.abstract |
The general consensus is that in order to reproduce the observed solar p-mode oscillation frequencies, turbulence should be included in solar models. However, until now there has not been any well-tested efficient method to incorporate turbulence into solar modeling. We present here two methods to include turbulence in solar modeling within the framework of the mixing length theory, using the turbulent velocity obtained from numerical simulations of the highly superadiabatic layer (SAL) of the Sun at three stages of its evolution. The first approach is to include the turbulent pressure alone, and the second is to include both the turbulent pressure and the turbulent kinetic energy. The latter is achieved by introducing two variables : the turbulent kinetic energy per unit mass and the effective ratio of specific heats owing to the turbulent perturbation. These are treated as additions to the standard thermodynamic coordinates (e.g., pressure and temperature). We investigate the effects of both treatments of turbulence on the structure variables, the adiabatic sound speed, the structure of the highly superadiabatic layer, and the p-mode frequencies. We find that the second method reproduces the SAL structure obtained in three-dimensional simulations and produces a p-mode frequency correction an order of magnitude better than the first method. |
en_CA |
dc.description.provenance |
Submitted by Janine Mills (janine.mills@smu.ca) on 2015-04-02T14:33:38Z
No. of bitstreams: 1
Guenther_David_B_article_2002_a.pdf: 305457 bytes, checksum: a6d137673c875baa5d49cf115d02a8d3 (MD5) |
en |
dc.description.provenance |
Made available in DSpace on 2015-04-02T14:33:38Z (GMT). No. of bitstreams: 1
Guenther_David_B_article_2002_a.pdf: 305457 bytes, checksum: a6d137673c875baa5d49cf115d02a8d3 (MD5)
Previous issue date: 2002-03-10 |
en |
dc.language.iso |
en |
en_CA |
dc.publisher |
American Astronomical Society |
en_CA |
dc.publisher |
IOP Publishing |
|
dc.relation.uri |
http://dx.doi.org/10.1086/338352 |
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dc.rights |
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user. |
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dc.subject.lcsh |
Sun -- Evolution |
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dc.subject.lcsh |
Helioseismology |
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dc.subject.lcsh |
Sun -- Internal structure |
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dc.subject.lcsh |
Turbulence |
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dc.title |
Inclusion of turbulence in solar modeling |
en_CA |
dc.type |
Text |
en_CA |
dcterms.bibliographicCitation |
Astrophysical Journal 567(2), 1192-1201. (2002) |
en_CA |
Copyright statement:
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.