dc.creator |
Guenther, David B. |
|
dc.creator |
Chaboyer, Brian |
|
dc.creator |
Demarque, P. |
|
dc.creator |
Pinsonneault, M. H. |
|
dc.date.accessioned |
2015-03-24T14:31:16Z |
|
dc.date.available |
2015-03-24T14:31:16Z |
|
dc.date.issued |
1995-06-10 |
|
dc.identifier.issn |
0004-637X |
|
dc.identifier.uri |
http://library2.smu.ca/xmlui/handle/01/25997 |
|
dc.description |
Publisher's version/PDF |
en_CA |
dc.description.abstract |
We have studied the importance of the combined effects of rotation, diffusion, and convective overshoot on the p-mode oscillation spectrum and the neutrino flux of the standard solar model. To isolate the various physical affects included in the new rotation plus diffusion models we also constructed solar models to test the significance of diffusion and of overshoot by themselves. In previous studies, models that include helium diffusion during solar evolution were found to improve the predicted p-mode frequencies for some modes and worsen the agreement for others (Guenther et al. 1993). Here we verify this result for both the Bahcall & Loeb (1990) formulation of diffusion and the Proffitt & Michaud (1991) formulation of diffusion. We find that the effects of rotation on the Sun's structure in the outer layers perturbs the p-mode frequencies only slightly when compared to the more substantial effects due to diffusion. In the thin overshoot layer (taken here to be 0.1 H[subscript p]), we have compared the effect of overmixing in a radiative layer versus convective (adiabatic) penetration. Neither radiative overmixing nor adiabatic penetration has any significant effect on the p-modes, probably in part because the overshoot layer is constrained to be thin. The predicted neutrino flux in our diffusion plus rotation model is 7.12 SNU for Cl detectors, 127 SNU for Ga detectors, and 5.00 x 10[superscript 6] ergs cm[superscript -2] for the [superscript 8]B neutrinos; this is approximately half-way between the standard solar model without diffusion, and the standard solar model with diffusion alone. |
en_CA |
dc.description.provenance |
Submitted by Janine Mills (janine.mills@smu.ca) on 2015-03-24T14:31:16Z
No. of bitstreams: 1
Guenther_David_B_article_1995_a.pdf: 251552 bytes, checksum: fba27ccca26bd4f172316f940bc6e873 (MD5) |
en |
dc.description.provenance |
Made available in DSpace on 2015-03-24T14:31:16Z (GMT). No. of bitstreams: 1
Guenther_David_B_article_1995_a.pdf: 251552 bytes, checksum: fba27ccca26bd4f172316f940bc6e873 (MD5)
Previous issue date: 1995-06-10 |
en |
dc.language.iso |
en |
en_CA |
dc.publisher |
American Astronomical Society |
en_CA |
dc.relation.uri |
http://dx.doi.org/10.1086/175802 |
|
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 -- Internal structure |
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dc.subject.lcsh |
Solar oscillations |
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dc.subject.lcsh |
Sun -- Rotation |
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dc.title |
Rotation, diffusion, and overshoot in the Sun: effects on the oscillation frequencies and the neutrino flux |
en_CA |
dc.type |
Text |
en_CA |
dcterms.bibliographicCitation |
Astrophysical Journal 446, 435-444. (1995) |
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.