Self-consistent 2D MHD modeling of multi-streamer coronal structures

Details Self-consistent 2D MHD modeling of multi-streamer coronal structures Self-consistent 2D MHD modeling of multi-streamer coronal structures

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh21b..02o&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH21B-02

Physics

7509 Corona, 7524 Magnetic Fields, 7827 Kinetic And Mhd Theory, 7843 Numerical Simulation Studies

Scientific paper

Recently, a semi-empirical 2D MHD model of the solar corona was constructed by Sittler and Guhathakurta [1999]. The model uses an empirical electron density and empirical magnetic field during solar minimum as input to the conservation equations of mass, momentum, and energy to derive an empirical effective heat flux, or empirical heating function. This semi-empirical model is not a self-consistent calculation. We explore the possibility of developing a self-consistent model that uses the empirical heating function as a constraint for the calculations. This allows us to solve the energy equation without use of a polytrope which we know does not apply near the Sun. For our initial attempt we use the empirically derived magnetic field model obtained from observed streamer topologies and Ulysses boundary conditions to initialize our self-consistent 2D MHD model of the solar corona. We solve the thermally conductive energy equations with an empirical heating function, and obtain 3-streamer structure with self-consistent magnetic field, current-sheets, solar wind outflow, density, and temperature. We compare the results of the thermally conductive model to the polytropic model, and to the empirical model. We find that the self-consistent magnetic field structure is more realistic then the empirical model. We find that the thermally conductive streamers result in more diffuse current-sheets than in the polytropic model. We also find that the heating function reduces the heliocentric distance of the streamers' cusp, and produces more rapid acceleration of the solar wind in the thermally conductive model then in the polytropic model, consistent with observations. We investigate the effect of various forms of the heating function, and of an empirically derived heat flux on the solutions.

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