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Accretion and wind dynamics in tidal disruption events

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

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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Gezari et al. 2012, Nature, 485, 217
Mageshwaran T. & Mangalam A. 2015, ApJ, 814, 141
Mangalam A. 2001, A&A, 379, 1138
Mangalam A. 2003, Bulletin of the Astronomical Society of India, 31, 207
Rees Martin J. 1988, Nature, 333, 523
Saxton et al. 2014, A&A, 572
Strubbe Linda E. & Quataert Eliot. 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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