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Magnetic instability of filaments in different solar regions

Published online by Cambridge University Press:  12 September 2017

J. Palacios ,
A. Guerrero ,
C. Cid ,
E. Saiz  and
Y. Cerrato
J. Palacios
Affiliation:
Departamento de Física y Matemáticas, Universidad de Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: [email protected]
A. Guerrero
Affiliation:
Departamento de Física y Matemáticas, Universidad de Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: [email protected]
C. Cid
Affiliation:
Departamento de Física y Matemáticas, Universidad de Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: [email protected]
E. Saiz
Affiliation:
Departamento de Física y Matemáticas, Universidad de Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: [email protected]
Y. Cerrato
Affiliation:
Departamento de Física y Matemáticas, Universidad de Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: [email protected]
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Abstract

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Magnetic instability is a key consideration for filament eruptions and subsequent CMEs. In this contribution we are considering different magnetic conditions for active and non-active regions, such as coronal hole regions and quiet sun, and also active regions of a simple magnetic configuration. The aim is to assess magnetic instability through potential and non-potential field modelling and 3D evaluation of the magnetic decay index. Some eruptive examples from solar cycle 24 using HMI/SDO data are presented, complemented with observations of AIA/SDO.

Keywords

Sun: magnetic fieldsSun: atmosphere
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S327: Fine Structure and Dynamics of the Solar Atmosphere , October 2016 , pp. 71 - 76
Copyright
Copyright © International Astronomical Union 2017 

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