dc.creator |
Lydon, Thomas Joseph |
|
dc.creator |
Guenther, David B. |
|
dc.creator |
Sofia, S. |
|
dc.date.accessioned |
2013-11-01T15:42:30Z |
|
dc.date.available |
2013-11-01T15:42:30Z |
|
dc.date.issued |
1996-01-10 |
|
dc.identifier.issn |
2041-8205 |
|
dc.identifier.uri |
http://library2.smu.ca/xmlui/handle/01/25310 |
|
dc.description |
Publisher's version/PDF |
|
dc.description.abstract |
By mimicking the effects of a magnetic field on the interior structure of a solar model, observed changes in p-mode frequencies over the course of the solar cycle are explained in terms of a change in the intensity and distribution of a magnetic field near the top of the solar convection zone; previous attempts of explain these observations have concentrated on magnetic fields extending into the solar atmosphere. Specifically, the observed frequency changes for the 5 [less than or equal to] l [less than or equal to] 60 modes between 1986 and 1989 can be accounted for by a change in magnetic field strength of 400 G approximately 320 km below the solar surface; in a standard solar model, this depth corresponds to a temperature of 10,800 K and a pressure of 3.63 3 X 10[superscript 5] dyn cm[superscript -2]. These results are discussed in light of a measured change in the solar radius of 4 km between 1992 and 1994 by the Solar Disk Sextant Experiment. |
en_CA |
dc.description.provenance |
Submitted by Trish Grelot (trish.grelot@smu.ca) on 2013-11-01T15:42:30Z
No. of bitstreams: 1
guenther_d_b_article_1996.pdf: 139380 bytes, checksum: 3a0908fa796e992bd11474a89847c7e0 (MD5) |
en |
dc.description.provenance |
Made available in DSpace on 2013-11-01T15:42:30Z (GMT). No. of bitstreams: 1
guenther_d_b_article_1996.pdf: 139380 bytes, checksum: 3a0908fa796e992bd11474a89847c7e0 (MD5)
Previous issue date: 1996-01-10 |
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/10.1086/309867 |
|
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 magnetic fields |
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dc.subject.lcsh |
Solar oscillations |
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dc.title |
An alternative explanation for the observed variation of solar p-modes with the solar cycle |
en_CA |
dc.type |
Text |
en_CA |
dcterms.bibliographicCitation |
Astrophysical Journal Letters 456(2), L127-L130. (1996) |
|
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.