J. Galindo Trejo
Instituto de Astronomía, UNAM, Apdo. Postal 70-264, 04510 México, D. F., México (galindo@astroscu.unam.mx).
Received 2005 November 25
Accepted 2006 January 11
]]> RESUMEN
Analizamos la estabilidad MHD lineal de una protuberancia solar descrita por el modelo bidimensional de Osherovich (1989). Este modelo de equilibrio considera explícitamente la influencia de un campo magnético vertical externo de tal forma que la protuberancia puede encontrarse en la frontera entre dos regiones de polaridad magnética opuesta. Estudiamos su estabilidad frente a perturbaciones en el marco de la MHD ideal usando un método numérico basado en el Principio de Energía de Bernstein et al. (1958). En nuestro análisis se consideran casos específicos de parámetros físicos observados en protuberancias estacionarias. Por completez presentamos igualmente resultados para otros parámetros que podrían ser aplicables tal vez a estrellas del tipo solar.
ABSTRACT
We examine the linear MHD-stability of a solar quiescent prominence described by the two-dimensional model of Osherovich (1989). This equilibrium model takes into account explicitly the influence of an external vertical magnetic field so that the prominence can be situated on the boundary between two regions of opposite magnetic polarity. We analyze its stability against perturbations within ideal MHD using a numerical method based on the Energy Principle of Bernstein et al. (1958). In our study specific cases of physical parameters observed in quiescent prominence are considered. For completeness we present as well results for other parameters which may perhaps be applicable to solar-type stars.
Key Words: MHD: WAVES — SUN: OSCILLATIONS — SUN: PROMINENCES.
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