AAS 204th Meeting, June 2004
Session 4 Plasma Astrophysics of Coronae
Poster, Monday, May 31, 2004, 9:20am-6:30pm, Ballroom

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[4.06] How Helical Dynamos Sustain the Solar Cycle and Power Coronae and Ouflows from Astrophysical Disks

E. G. Blackman (University of Rochester)

Because the large scale solar coronal field reverses, it cannot be a remnant of the proto-sun and must be produced in situ. This requires an internal helical dynamo in combination with buoyant ejection and dynamical relaxation. The helical dynamo operates by segregating magnetic helicity and sending one sign to large scales and the opposite sign to small scales. I argue that both large and small scale magnetic helicity is ejected by the sun. The large scale ejection keeps the field from reaching the maximum value it could, and the ejection of small scale helicity allows the cycle to repeat on fast time scales. I also explain why the helical dynamo combined with magnetic relaxation is the likely mechanism that produces both coronal X-ray emission from accretion disks and the large scale fields that drive outflows.

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