Volume 392, Number 2, September III 2002
|Page(s)||469 - 472|
|Section||Cosmology (including clusters of galaxies)|
|Published online||30 August 2002|
Observational signatures of the magnetic connection between a black hole and a disk
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
Corresponding author: email@example.com
Accepted: 19 June 2002
We use a simple model to demonstrate the observational signatures of the magnetic connection between a black hole and a disk: (1) with the existence of the magnetic connection, more energy is dissipated in and radiated away from regions close to the center of the disk; (2) the magnetic connection can produce a very steep emissivity compared to the standard disk accretion; (3) the observational spectral signature of the magnetic connection can be robust. These signatures can be identified by the observations of Chandra and XMM-Newton. In fact, the steep emissivity index for the Seyfert 1 galaxies MCG–6-30-15 and Mrk-766 inferred from the recent XMM-Newton observations is very difficult to be explained with a standard accretion disk but can be easily explained with the magnetic connection between a black hole and a disk.
Key words: black hole physics / accretion disks / magnetic fields / galaxies: active / galaxies: Seyfert
© ESO, 2002
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.