Magnetohydrodynamic Shock Heating of the Solar Corona

Details Magnetohydrodynamic Shock Heating of the Solar Corona Magnetohydrodynamic Shock Heating of the Solar Corona

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..apr.k1027h&link_type=abstract

American Physical Society, April Meeting, 2004, May 1-4, 2004, Denver, Colorado April 2004, MEETING ID: APR04, abstract #K1.027

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Computation

Scientific paper

Our paper in the Astrophysical Journal, vol. 596, pp. 646-655 presented the results of our one dimensional computations which showed that strong Alfvén waves that propagate along magnetic field lines up into the solar corona can develop into MHD shocks and act as a significant mechanism for coronal heating and wind acceleration in regions of open magnetic field lines. We now present results of extended computations that allow stronger shocks. We also include gravitational stratification, and various types of polarizations. We use an adiabatic energy equation and an FCT algorithm.

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