The Contribution by Thin Magnetic Flux Tubes to p-Mode Line Widths

Details The Contribution by Thin Magnetic Flux Tubes to p-Mode Line Widths The Contribution by Thin Magnetic Flux Tubes to p-Mode Line Widths

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...521..878c&link_type=abstract

The Astrophysical Journal, Volume 521, Issue 2, pp. 878-884.

Astronomy and Astrophysics

Astronomy

6

Magnetohydrodynamics: Mhd, Sun: Atmosphere, Sun: Magnetic Fields, Sun: Oscillations

Scientific paper

The contribution to p-mode line widths from the excitation of tube mode oscillations on an individual magnetic fibril is computed. An idealized model of the fibril within the photosphere is implemented, consisting of a vertical, thin magnetic flux tube embedded in a plane-parallel isentropic polytrope of index m. Bogdan et al. considered a similar model but imposed a stress-free boundary condition at the top of the photosphere, which acts to reflect any upward-propagating tube waves completely back down into the tube. The stress-free boundary condition neglects a possibly important physical process: the loss of energy to the upper solar atmosphere by the excitation of waves in the chromosphere and corona. Using simple models of the solar chromosphere and corona, we explore the consequences of applying various boundary conditions. The resultant upward energy fluxes are not large, but surprisingly the more realistic upper boundary conditions lead to a significant increase in kink mode flux out the bottom. Nevertheless, the sausage mode remains dominant in cases of interest and is essentially unaffected by the new boundary conditions. Consequently, the resultant total p-mode line width computed here can account for only a few percent of the observed line width.

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