Toward Understanding the Sun's Magnetic Fields and their Effects

Details Toward Understanding the Sun's Magnetic Fields and their Effects Toward Understanding the Sun's Magnetic Fields and their Effects

Apr 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..703..163t&link_type=abstract

PLASMAS IN THE LABORATORY AND IN THE UNIVERSE: New Insights and New Challenges. AIP Conference Proceedings, Volume 703, pp. 163

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Interplanetary Magnetic Fields, Magnetohydrodynamics And Plasmas

Scientific paper

Developments in instrumentation, numerical simulations, and theory are rapidly changing our view of solar magnetism. There are now observations that show magnetic field emerging on all convective scales. The emergence rate replaces the quiet Sun flux in less than 12 hours and even active region and sunspot fields are replaced in less than a month. There is evidence for local dynamo action suggesting that a bottom to a convection zone is not required for stellar magnetic activity. It is now recognized that 3D magnetic reconnection is fundamentally different from 2D. Time sequences of the one arc second (1'' = 726 km) spatial resolution TRACE images show that the temperature and density structure of the corona changes as fast as radiation and conduction allow. Because adjacent loops are observed in a range of temperatures that span at least 30,000 to 2,500,000 K, there is a inter mixture of temperatures regimes throughout the corona. Consequently, there is no line of sight through the corona that can be characterized by a single temperature and density. It would be surprising if other stars or other astrophysical systems with magnetic fields were simpler than the solar atmosphere.

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