Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7141
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dc.contributor.authorMageshwaran, T-
dc.contributor.authorMangalam, A-
dc.date.accessioned2017-07-06T08:20:42Z-
dc.date.available2017-07-06T08:20:42Z-
dc.date.issued2017-06-
dc.identifier.citationProceedings of the International Astronomical Union, Vol. 324, pp. 134-135en_US
dc.identifier.isbn9781107169944-
dc.identifier.urihttp://hdl.handle.net/2248/7141-
dc.descriptionRestricted Accessen_US
dc.description.abstractWe have constructed self similar models of time dependent and non relativistic accretion disks in both sub and super-Eddington phase of TDEs with wind outflows for a general viscosity prescription which is a function of surface density of the disk Σ d and radius r. The physical parameters are black hole (BH) mass M •, specific orbital energy E and angular momentum J, star mass M ⋆ and radius R ⋆. We have considered an accretion disk where matter is lost due to accretion by black hole and out flowing wind (in case of super-Eddington) and added through fallback of the disrupted debris. We have simulated the light curve profiles in various spectral bands and fit them to the observations to determine the above mentioned physical parameters.en_US
dc.language.isoenen_US
dc.publisherInternational Astronomical Unionen_US
dc.relation.ispartofseriesProceedings IAU Symposium No. 324;-
dc.relation.urihttps://doi.org/10.1017/S1743921317002228-
dc.rights© International Astronomical Union-
dc.subjectGalaxy: nucleusen_US
dc.subjectBlack hole physicsen_US
dc.subjectAccretionen_US
dc.subjectAccretion disksen_US
dc.titleAccretion and wind dynamics in tidal disruption eventsen_US
dc.typeArticleen_US
Appears in Collections:IIAP Publications

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