Assembling the Ingredients for a Jet: How Do Large-Scale Magnetic Fields Get There?

Details Assembling the Ingredients for a Jet: How Do Large-Scale Magnetic Fields Get There? Assembling the Ingredients for a Jet: How Do Large-Scale Magnetic Fields Get There?

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.5021r&link_type=abstract

American Astronomical Society, AAS Meeting #211, #50.21; Bulletin of the American Astronomical Society, Vol. 39, p.815

Astronomy and Astrophysics

Astrophysics

Scientific paper

Jets and outflows are observed around a wide variety of accreting objects (e.g., X-ray binaries and active galactic nuclei) 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. Here, we report theoretical work which challenges this conventional wisdom and shows that the surface layer of the disk (which is magnetorotationally stable and therefore nonturbulent) can easily advect magnetic fields inward. These results have important implications for numerical simulations and for the character of magnetic fields expected in the inner region of an accretion disk.
D. M. Rothstein is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0602259.

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