How to infer the Sun's global magnetic field using the Hanle effect

Bibcode
2017MNRAS.465.4414V
DOI
10.1093/mnras/stw3044
Vieu, T.; Martínez González, M. J.; Pastor Yabar, A.; Asensio Ramos, A.
Referencia bibliográfica

Monthly Notices of the Royal Astronomical Society, Volume 465, Issue 4, p.4414-4422

Fecha de publicación:
3
2017
Revista
Monthly Notices of the Royal Astronomical Society
Número de autores
4
Número de autores del IAC
4
Número de citas
1
Número de citas referidas
1
Descripción
We present a different approach to determine the characteristics of the global magnetic field of the Sun based on the study of the Hanle signals. The Hanle effect of a stellar dipole produces a surface asymmetric pattern of linear polarization that depends on the strength and geometry of this global field. Moreover, if the dipole is misaligned with respect to the rotation, the Hanle signals are modulated following the rotational period. We explore the possibility to retrieve those characteristics by comparing the computed theoretical signatures with actual observations. We show that this is possible, in the case of the Sr I line of the Sun, provided that the polarimetric sensitivity is of the order or below 10-5-10-6. The inference can be done either using the maps of resolved signals, in particular the spread of values obtained along different directions on the stellar disc, or using the disc-integrated signals.
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
Campos magnéticos
Técnicas
Física Solar (FS)

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