Accretion and wind dynamics in tidal disruption events

We 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...

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Bibliographic Details
Published in:Proceedings of the International Astronomical Union 2016-09, Vol.12 (S324), p.134-135
Main Authors: Mageshwaran, T., Mangalam, A.
Format: Article
Language:English
Subjects:
Accretion disks
Angular momentum
Astronomy
Band spectra
Computer simulation
Contributed Papers
Debris
Detritus
Disruption
Dynamics
Light curve
Physical properties
Spectral bands
Stellar winds
Tidal energy
Tidal power
Time dependence
Viscosity
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Summary:We 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.
ISSN:1743-9213
1743-9221
DOI:10.1017/S1743921317002228