Tidal Disruption Eddington Envelopes around Massive Black Holes
Abstract
Optically-thick envelopes may form following the tidal disruption of a star by a massive black hole. Such envelopes would reprocess hard radiation from accretion close to the black hole into the UV and optical bands producing AGN-luminosity flares with duration ~1 year. We show that due to relativistic effects, the envelopes are convective. If convection is efficient, then the structure of the envelopes is similar to that described in previous work; however, the photospheric radius is shown to be very sensitive to the luminosity at the envelope base, suggesting that either the envelope collapses or the envelope expands to a maximum radius at which point a wind may set in. For an envelope without winds, we find a maximum photospheric radius of ~10^16 cm (i.e. minimum effective temperature ~6,000 K). The evolution of the envelopes is described based on simple energy arguments.
Cite
@article{arxiv.astro-ph/9711199,
title = {Tidal Disruption Eddington Envelopes around Massive Black Holes},
author = {Andrew Ulmer and Bohdan Paczynski and Jeremy Goodman},
journal= {arXiv preprint arXiv:astro-ph/9711199},
year = {2007}
}
Comments
6 pages including 2 figures; latex; submitted to A&A