Accretion and Ejections in Magnetized Disks

Details Accretion and Ejections in Magnetized Disks Accretion and Ejections in Magnetized Disks

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004ap%26ss.292..377t&link_type=abstract

Astrophysics and Space Science, v. 292, Issue 1, p. 377-381 (2004).

Astronomy and Astrophysics

Astrophysics

Accretion, Disks, Jets, Mhd

Scientific paper

In this contribution I review the main challenges for theory and numerical simulation of accretion turbulence in disks. I then present briefly a solution we have elaborated in recent years to a part of these questions: we have found an MHD instability which occurs in the inner region of a disk in the configuration (poloidal field of the order of equipartition with the gas pressure) used for MHD jet models. This instability has the unique characteristic that it re-emits toward the corona a fraction of the energy and angular momentum it extracts from the disk. It is a good candidate to explain the low-frequency Quasi-Periodic Oscillation observed in X-ray binaries, and we believe that it might occur also in YSO.

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