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Accretion and wind dynamics in tidal disruption events

Published online by Cambridge University Press:  23 June 2017

T. Mageshwaran  and
A. Mangalam
T. Mageshwaran
Affiliation:
Indian Institute of Astrophysics, Bangalore, India560034, email: mageshwaran@iiap.res.in
A. Mangalam
Affiliation:
Indian Institute of Astrophysics, Bangalore, India560034, email: mangalam@iiap.res.in
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Abstract

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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 Σd 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.

Keywords

Galaxy: nucleusblack hole physicsaccretionaccretion disks
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S324: New Frontiers in Black Hole Astrophysics , September 2016 , pp. 134 - 135
Copyright
Copyright © International Astronomical Union 2017 

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