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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3197
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dc.contributor.authorShibahashi, H-
dc.contributor.authorHiremath, K. M-
dc.contributor.authorTakata, M-
dc.date.accessioned2008-08-19T05:19:19Z-
dc.date.available2008-08-19T05:19:19Z-
dc.date.issued1998-
dc.identifier.citationInternational Astronomical Union Symposium, No. 185, pp. 81 - 84en
dc.identifier.issn0074 - 1809-
dc.identifier.urihttp://hdl.handle.net/2248/3197-
dc.description.abstractWe deduce the density, pressure, and temperature profiles in the solar convective envelope by solving the basic equations for mass conservation and the hydrostatic equilibrium with the imposition of the helioseismologically determined sound-speed profile and equation of state. These profiles are required to match with the structure of the radiative core, which is also determined with the imposition of the sound speed profile. The depth of the convection zone and the helium abundance are obtained as a part of the solutions.en
dc.format.extent441182 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherInternational Astronomical Unionen
dc.relation.urihttp://adsabs.harvard.edu/abs/1998IAUS..185...81Sen
dc.subjectHydrostatic Equilibriumen
dc.subjectHelium Abundanceen
dc.titleA seismic model of the solar convective envelopeen
dc.typeArticleen
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