Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.118..443s&link_type=abstract
(IAU, Asian-Pacific Regional Meeting, 3rd, Kyoto, Japan, Sept. 30-Oct. 5, 1984) Astrophysics and Space Science (ISSN 0004-640X),
Astronomy and Astrophysics
Astrophysics
6
Accretion Disks, Astrophysics, Magnetohydrodynamics, Plasma Jets, Radio Jets (Astronomy), Cosmic Plasma
Scientific paper
An MHD model for the formation of astrophysical jets is discussed, in which the directed flows are ejected along the rotaion axis of an accretion disk formed from a cloud having a large scale magnetic field parallel to the angular momentum axis of the disk. The acceleration of jets is due to the j x B force in the relaxing magnetic twist, which is produced by the rotation of the disk. The characteristic features of the jets, predicted by this mechanism and hopefully to be proven by observations, are the helical velocity and the hollow cylindrical shape of the jet, with a diameter of roughly the size of the region from which the accretion disk collected its mass. Justification for the asumption of the perpendicular orientation of the disk, or the parallelism of the jets, to the external magnetic field may be provided by the fact that the component of rotation whose axis is perpendicular to the field may have been damped in the earlier phase of the cloud contraction.
Shibata Kazunari
Uchida Yoshiharu
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