An alternative explanation for the observed variation of solar p-modes with the solar cycle

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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.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.
dc.subject.lcsh Sun -- Internal structure
dc.subject.lcsh Solar magnetic fields
dc.subject.lcsh Solar oscillations
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)


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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.
 
Published Version: http://dx.doi.org/10.1086/309867
 
 

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