Skip to main content
    • Aa
    • Aa

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.

Linked references
Hide All

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

Recommend this journal

Email your librarian or administrator to recommend adding this journal to your organisation's collection.

Proceedings of the International Astronomical Union
  • ISSN: 1743-9213
  • EISSN: 1743-9221
  • URL: /core/journals/proceedings-of-the-international-astronomical-union
Please enter your name
Please enter a valid email address
Who would you like to send this to? *



Full text views

Total number of HTML views: 0
Total number of PDF views: 10 *
Loading metrics...

Abstract views

Total abstract views: 26 *
Loading metrics...

* Views captured on Cambridge Core between 23rd June 2017 - 18th August 2017. This data will be updated every 24 hours.