Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/3932
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dc.contributor.authorSaini, T.D.-
dc.contributor.authorGulati, Mamta-
dc.contributor.authorSridhar, S.-
dc.date.accessioned2010-07-22T06:44:09Z-
dc.date.available2010-07-22T06:44:09Z-
dc.date.issued2009-01-15-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2009, Vol.400, p2090en
dc.identifier.issn1365-2966 (Online)-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/2289/3932-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractThin accretion discs around massive compact objects can support slow pressure modes of oscillations in the linear regime that have azimuthal wavenumber m= 1 . We consider finite, flat discs composed of barotropic fluid for various surface density profiles and demonstrate – through WKB analysis and numerical solution of the eigenvalue problem – that these modes are stable and have spatial scales comparable to the size of the disc. We show that the eigenvalue equation can be mapped to a Schrödinger-like equation. The analysis of this equation shows that all eigenmodes have discrete spectra. We find that all the models we have considered support negative frequency eigenmodes; however, the positive eigenfrequency modes are only present in power-law discs, albeit for physically uninteresting values of the power-law index β and barotropic index γ.en
dc.language.isoenen
dc.publisherWiley Interscience for the RASen
dc.relation.urihttp://adsabs.harvard.edu/abs/2009arXiv0901.4229Den
dc.relation.urihttp://arxiv.org/abs/0901.4229en
dc.relation.urihttp://dx.doi.org/10.1111/j.1365-2966.2009.15602.xen
dc.rights2009 Wiley Interscience for the RASen
dc.subjectaccretion discsen
dc.subjecthydrodynamicsen
dc.subjectwavesen
dc.subjectmethods analyticalen
dc.titleSlow pressure modes in thin accretion discsen
dc.typeArticleen
Appears in Collections:Research Papers (A&A)

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