Some results concerning the MHD boundary conditions at the base of the solar corona

Details Some results concerning the MHD boundary conditions at the base of the solar corona Some results concerning the MHD boundary conditions at the base of the solar corona

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004phdt.........7p&link_type=abstract

Thesis (PhD). NEW YORK UNIVERSITY, Source DAI-B 64/11, p. 5557, May 2004, 169 pages.

Physics

Scientific paper

Using the exact solutions of the linearized equations of ideal magnetohydrodynamics (MHD) in the solar photosphere and chromosphere, the radiation condition for downward propagating waves in the photosphere/chromosphere, and the jump conditions of ideal MHD across the transition region, boundary conditions are derived at the base of the solar corona which can be applied to the study of various coronal phenomena. These boundary conditions explicitly take into account the losses of wave energy from the corona to the photosphere. The background magnetic field in the photosphere/chromosphere is assumed to be strong as in the case of sunspots and active regions. In this case, the equations for the Alfvén waves in the photosphere/chromosphere de- couple from the equations for the fast and slow waves so the two classes of waves can be treated independently. Moreover, the solutions for each class of waves in the photosphere/chromosphere can be expressed in terms of known special functions. This enables the development of the boundary conditions. The boundary conditions for the Alfvén waves are applied to the study of resonances in coronal loops and an additional boundary condition is derived to treat the excitation by forced oscillations of the footpoints. This latter boundary condition is different from the “tied-line” boundary condition often used for driving footpoint motions because it simultaneously allows for losses to the photosphere.

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