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: firstname.lastname@example.org
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
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