منابع مشابه
Reconnection in Marginally Collisionless Accretion Disk Coronae
We point out that a conventional construction placed upon observations of accreting black holes, in which their nonthermal X-ray spectra are produced by inverse comptonization in a coronal plasma, suggests that the plasma is marginally collisionless. Recent developments in plasma physics indicate that fast reconnection takes place only in collisionless plasmas. As has recently been suggested fo...
متن کاملSimulations of Jet Production in Magnetized Accretion Disk Coronae
We describe the results of over 40 MHD simulations, performed on Caltech/JPL parallel supercomputers, of the coronae of magnetized accretion disks around compact objects. All produce some type of outflow from the disk. Our parameter study investigated the character of the outflow as a function of the strength of the initial poloidal magnetic field and its angle with respect to the disk rotation...
متن کاملTemporal properties of flares in accretion disk coronae
Using a non-linear Monte-Carlo code we investigate the radiative response of an accretion disk corona system to static homogeneous flares. We model a flare by a rapid (comparable to the light crossing time) energy dissipation in the corona or the disk. If the flares originate from the disk, the coronal response to the soft photon shots produces a strongly non-linear Comptonised radiation output...
متن کاملSemi-analytical radiative transfer in plane-parallel geometry: application to accretion disk coronae
A simplified frequency integrated radiative transfer equation is solved to study Compton scatterings in the corona of the disk by using numerical iterating method. We find that the vertical thickness of the corona cannot be used as the typical length to measure the optical depth of the corona. A semi-analytical approach is proposed to calculate the energy dissipations in the corona of the disk....
متن کاملAccretion disc coronae as magnetic reservoirs
Most astrophysical sources powered by accretion onto a black hole, either of stellar mass or supermassive, when observed with hard X-rays show signs of a hot Comptonizing component in the flow, the so-called corona, with observed temperatures and optical depths lying in a narrow range (0.1τ1 and 1×109KT 3×109 K). Here we argue that these facts constitute strong supporting evidence for a magneti...
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ژورنال
عنوان ژورنال: Highlights of Astronomy
سال: 1989
ISSN: 1539-2996
DOI: 10.1017/s1539299600008248