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Accretion and wind dynamics in tidal disruption events

  • T. Mageshwaran (a1) and A. Mangalam (a2)
Abstract
Abstract

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.

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This list contains references from the content that can be linked to their source. For a full set of references and notes please see the PDF or HTML where available.

Gezari et al. 2012, Nature, 485, 217

T. Mageshwaran & A. Mangalam 2015, ApJ, 814, 141

A. Mangalam 2001, A&A, 379, 1138

Martin J. Rees 1988, Nature, 333, 523

Linda E. Strubbe & Eliot. Quataert 2009, MNRAS, 400, 2070

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Proceedings of the International Astronomical Union
  • ISSN: 1743-9213
  • EISSN: 1743-9221
  • URL: /core/journals/proceedings-of-the-international-astronomical-union
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