Physics – Plasma Physics
Scientific paper
Nov 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..dppfm1002b&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
Coronae of accretion disks from which jets emerge, and stellar corona share a lot in common. Both represent magnetically active environments anchored in turbulent rotators below. The geometry of jet mediating magnetic fields is analogous to that of stellar coronal holes. Where do the fields of these jets come from? In the sun, the sign reversals of the large scale coronal hole fields imply the field is produced in situ, not simply accreted from the original material from which the sun formed. We cannot measure such reversals in accretion disks, but the similarity between the two coronal environments and the difficulty of accreting large scale fields in thin disks suggest a role for in situ formation. I discuss the physics behind a two stage framework for understanding large scale field formation in coronae: (1) a helical dynamo in the rotator supplies the corona with bihelical structures of small net helicity (2) bihelical magnetic relaxation in the corona which grows global scale helical fields of a dominant sign.
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