Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.2630r&link_type=abstract
American Astronomical Society, HEAD meeting #10, #26.30
Astronomy and Astrophysics
Astrophysics
Scientific paper
Jets and outflows are observed around a wide variety of accreting objects and seem to be a near-ubiquitous feature of accretion disks. Large-scale magnetic fields are often thought necessary for jet formation, but a longstanding puzzle is that the turbulence which is responsible for inward disk accretion should be even more efficient at causing a large-scale magnetic field to diffuse outward; it just doesn't seem possible to build up a strong field in the inner disk through advection of a weak one from outside. Recently, however, we have proposed a simple mechanism whereby a large-scale magnetic field can be advected inward in the nonturbulent surface layer of a magnetorotationally unstable disk (as opposed to the main turbulent body, where it cannot advect in). Here, we will discuss this mechanism, its consequences for understanding jet formation and the structure of accretion disks, and numerical simulations that can and should be performed in order to test it.
D. M. Rothstein is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0602259.
Lovelace Richard V. E.
Rothstein David M.
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