Iron Line Profiles from Relativistic Thick Accretion Disk
| dc.creator | Wu, Sheng-Miao | |
| dc.creator | Wang, Ting-Gui | |
| dc.date | 2007-04-19 | |
| dc.date.accessioned | 2026-07-07T07:57:17Z | |
| dc.date.available | 2026-07-07T07:57:17Z | |
| dc.description | We present a new code for calculating the Fe Kalpha line profiles from relativistic accretion disks with finite thickness around a rotating black hole. The thin Keplerian accretion disk must become thicker and sub-Keplerian with increasing accretion rates. We here embark on, for the first time, a fully relativistic computation which is aimed at gaining an insight into the effects of geometrical thickness and the sub-Keplerian orbital velocity on the line profiles. This code is also well-suited to produce accretion disk images. | |
| dc.description | 2 pages, 1 figure, Conference proceedings to appear in "The Central Engine of Active Galactic Nuclei", ed. L. C. Ho and J.-M. Wang (San Francisco: ASP) | |
| dc.identifier | https://arxiv.org/abs/0704.2460 | |
| dc.identifier | http://arxiv.org/abs/0704.2460 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/127597 | |
| dc.subject | Astrophysics | |
| dc.title | Iron Line Profiles from Relativistic Thick Accretion Disk | |
| dc.type | text |