A seismic model of the solar convective envelope

dc.contributor.author	Shibahashi, H
dc.contributor.author	Hiremath, K. M
dc.contributor.author	Takata, M
dc.date.accessioned	2008-08-19T05:19:19Z
dc.date.available	2008-08-19T05:19:19Z
dc.date.issued	1998
dc.identifier.citation	International Astronomical Union Symposium, No. 185, pp. 81 - 84	en
dc.identifier.issn	0074 - 1809
dc.identifier.uri	http://hdl.handle.net/2248/3197
dc.description.abstract	We 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.extent	441182 bytes
dc.format.mimetype	application/pdf
dc.language.iso	en	en
dc.publisher	International Astronomical Union	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1998IAUS..185...81S	en
dc.subject	Hydrostatic Equilibrium	en
dc.subject	Helium Abundance	en
dc.title	A seismic model of the solar convective envelope	en
dc.type	Article	en