Energetics and Structure of Multispecies Solar Coronal Loops

Details Energetics and Structure of Multispecies Solar Coronal Loops Energetics and Structure of Multispecies Solar Coronal Loops

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998phdt........10l&link_type=abstract

Thesis (PHD). THE UNIVERSITY OF CHICAGO , Source DAI-B 59/07, p. 3495, Jan 1999, 43 pages.

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Helium

Scientific paper

The temperature and density profiles of multispecies quiescent solar coronal loops containing hydrogen, helium, and heavier species are investigated using a numerical model for steady-state force and energy balance. The model loop follows a semicircular magnetic field line anchored in the chromosphere and contains low-β plasma. The model allows for species-dependent heating. The electrons, protons, and helium ions are taken to be in thermal equilibrium and form the dominant plasma component. In nonisothermal regions (i.e., in the presence of steep transition-region temperature gradients), the outward thermal force induces an inward polarization electric field along the loop; in nearly isothermal (i.e., ∇ T small) coronal regions, the electric field is outward to counterbalance gravity. The pressure gradient is negative for the protons, though in many cases it is positive for heavier ions. The thermal force can induce local minor ion overdensities. Gravitational settling may deplete the heavy ion densities, especially in the longer loops, and can occur if the settling timescale is short compared with the loop lifetime and the turbulent mixing timescale. The calculated loop abundances vary with the loop parameters. For heavy ion temperatures of ~107-108 K, the collisional energy transfer rate per particle, and therefore the required heat input per particle, is ~10-8-10-9 ergs s-1.

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