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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/4099
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dc.contributor.authorPeraiah, A-
dc.date.accessioned2008-12-17T16:35:51Z-
dc.date.available2008-12-17T16:35:51Z-
dc.date.issued1982-09-
dc.identifier.citationJournal of Astrophysics and Astronomy, Vol. 3, pp. 297 - 302en
dc.identifier.issn0250- 6335-
dc.identifier.urihttp://hdl.handle.net/2248/4099-
dc.descriptionOpen Access-
dc.description.abstractAn attempt has been made to explain the Balmer progression in velocities seen in Pleione and other shell stars. Equations of conservation of mass and momentum are simultaneously solved with assumptions which simplify the calculations of the solution. We have considered the radiation pressure due to lines and continuum. It is found that the high-excitation lines are formed where the velocity gradients are high.en
dc.language.isoenen
dc.publisherIndian Academy of Sciencesen
dc.relation.urihttp://adsabs.harvard.edu/abs/1982JApA....3..297Pen
dc.relation.urihttp://www.springerlink.com/content/b500888wrv666304/en
dc.rights© Indian Academy of Sciencesen
dc.subjectGas Flowen
dc.subjectRadial Velocityen
dc.subjectStellar Envelopesen
dc.subjectVelocity Distributionen
dc.subjectAbsorption Spectraen
dc.subjectConservation Lawsen
dc.subjectHydrogenen
dc.subjectKinetic Energyen
dc.subjectRadiation Pressureen
dc.subjectShell Starsen
dc.subjectStellar Massen
dc.subjectStellar Temperatureen
dc.subjectStellar Modelsen
dc.subjectBalmer Progression-
dc.subjectVelocity Gradients-
dc.subjectShell Stars-
dc.titleOn the Balmer progression in the expanding shell of Pleioneen
dc.typeArticleen
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