Coronal loop physical parameters from the analysis of multiple observed transverse oscillations

Bibcode
2013A&A...554A...7A
DOI
10.1051/0004-6361/201321428
Asensio-Ramos, A.; Arregui, I.
Referencia bibliográfica

Astronomy and Astrophysics, Volume 554, id.A7, 9 pp.

Fecha de publicación:
6
2013
Revista
Astronomy and Astrophysics
Número de autores
2
Número de autores del IAC
2
Número de citas
18
Número de citas referidas
18
Descripción
The analysis of quickly damped transverse oscillations of solar coronal loops using magneto-hydrodynamic seismology allows us to infer physical parameters that are difficult to measure otherwise. Under the assumption that such damped oscillations are due to the resonant conversion of global modes into Alfvén oscillations of the tube surface, we carry out a global seismological analysis of a large set of coronal loops. A Bayesian hierarchical method is used to obtain distributions for coronal loop physical parameters by means of a global analysis of a large number of observations. The resulting distributions summarize global information and constitute data-favoured information that can be used for the inversion of individual events. The results strongly suggest that internal Alfvén travel times along the loop are longer than 100 s and shorter than 540 s with 95% probability. Likewise, the density contrast between the loop interior and the surrounding is larger than 2.3 and below 6.9 with 95% probability.
Proyectos relacionados
Imagen del Proyecto
Magnestismo Solar y Estelar

Los campos magnéticos son uno de los ingredientes fundamentales en la formación de estrellas y su evolución. En el nacimiento de una estrella, los campos magnéticos llegan a frenar su rotación durante el colapso de la nube molecular, y en el fin de la vida de una estrella, el magnetismo puede ser clave en la forma en la que se pierden las capas

Tobías
Felipe García
En ejecución
Project Image
Magnetismo, Polarización y Transferencia Radiativa en Astrofísica

Los campos magnéticos están presentes en todos los plasmas astrofísicos y controlan la mayor parte de la variabilidad que se observa en el Universo a escalas temporales intermedias. Se encuentran en estrellas, a lo largo de todo el diagrama de Hertzsprung-Russell, en galaxias, e incluso quizás en el medio intergaláctico. La polarización de la luz

Tanausú del
Pino Alemán
En ejecución
Tipo
Con árbitro
Métodos
Física Solar (FS)

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