Accretion power and the origin of astrophysical jets

Details Accretion power and the origin of astrophysical jets Accretion power and the origin of astrophysical jets

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..dppcm1005p&link_type=abstract

American Physical Society, 46th Annual Meeting of the Division of Plasma Physics, 15-19 November, 2004, Savannah, GA. MEETING I

Physics

Plasma Physics

Scientific paper

Astrophysical jets are observed in a wide variety of systems ranging from stars in the act of formation to quasars. In most if not all of these systems, a central object such as a massive black hole or a young star accretes gas from a surrounding, Keplerian, gaseous disk. One of the most popular and best tested models for jet formation posits that jets are highly collimated, hydromagnetic winds that are flung out from the surfaces of accretion disks along open field lines that thread them. Basic theoretical calculations predict that these jets are powered by the gravitational potential energy that must be released as gas in the underlying disk slowly spirals in towards the central object. In addition, the magnetic torque exerted by such a wind can efficiently extract the angular momentum of gas within the disk, enabling the accretion process. Recent observations of jets from young stellar objects reveal that these flows rotate and can be traced back to an extended region of the underlying disk, and these provide stringent tests for the model. I shall review the basic elements of this picture and show that it provides a very promising universal model for jets. This is supported by sophisticated 3D numerical simulations.

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