Tidal Disruption Eddington Envelopes around Massive Black Holes
| dc.creator | Ulmer, Andrew | |
| dc.creator | Paczynski, Bohdan | |
| dc.creator | Goodman, Jeremy | |
| dc.date | 1997-11-18 | |
| dc.date.accessioned | 2026-07-07T02:25:09Z | |
| dc.date.available | 2026-07-07T02:25:09Z | |
| dc.description | 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. | |
| dc.description | 6 pages including 2 figures; latex; submitted to A&A | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9711199 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9711199 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/11820 | |
| dc.subject | Astrophysics | |
| dc.title | Tidal Disruption Eddington Envelopes around Massive Black Holes | |
| dc.type | text |