Solar coronal heating by magnetic cancellation - III. Thermodynamics

Details Solar coronal heating by magnetic cancellation - III. Thermodynamics Solar coronal heating by magnetic cancellation - III. Thermodynamics

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008mnras.384..972v&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 384, Issue 3, pp. 972-986.

Astronomy and Astrophysics

Astronomy

2

Mhd, Sun: Corona, Sun: Magnetic Fields

Scientific paper

We present two-dimensional numerical magnetohydrodynamics simulations of a coronal X-ray bright point (XBP) caused by a cancelling magnetic feature (CMF). Cancellation is driven by converging motions of two magnetic bipolar sources. These sources are initially disconnected from each other so that both, the CMF and the associated reconnection/heating event (i.e. the XBP), are modelled in a self-consistent way. In the initial state, there is no X-point but two separatrices are present. Hence, the reconnection/heating and the cancellation phases have not yet started. Our numerical experiments end shortly after the converging magnetic bipole has fully cancelled. By this time, reconnection in the inner domain has ceased and occurs only at the base. Solving the energy equation with various heating and cooling terms included, and considering different bottom boundary conditions, reveals that the unrealistically high temperatures produced by Ohmic heating are reduced to more moderate temperatures of 1.5-2 MK consistent with observations of XBPs, if thermal conduction is included and density and temperature are fixed at the base.

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