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Photospheric magnetic field of an eroded-by-solar-wind coronal mass ejection

Published online by Cambridge University Press:  12 September 2017

J. Palacios ,
C. Cid ,
E. Saiz  and
A. Guerrero
J. Palacios
Affiliation:
Departamento de Física y Matemáticas, Universidad de Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: judith.palacios@uah.es
C. Cid
Affiliation:
Departamento de Física y Matemáticas, Universidad de Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: judith.palacios@uah.es
E. Saiz
Affiliation:
Departamento de Física y Matemáticas, Universidad de Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: judith.palacios@uah.es
A. Guerrero
Affiliation:
Departamento de Física y Matemáticas, Universidad de Alcalá University Campus, Sciences Building, P.O. 28871, Alcalá de Henares, Spain email: judith.palacios@uah.es
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Abstract

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We have investigated the case of a coronal mass ejection that was eroded by the fast wind of a coronal hole in the interplanetary medium. When a solar ejection takes place close to a coronal hole, the flux rope magnetic topology of the coronal mass ejection (CME) may become misshapen at 1 AU as a result of the interaction. Detailed analysis of this event reveals erosion of the interplanetary coronal mass ejection (ICME) magnetic field. In this communication, we study the photospheric magnetic roots of the coronal hole and the coronal mass ejection area with HMI/SDO magnetograms to define their magnetic characteristics.

Keywords

Sun: coronal mass ejections (CMEs)Sun: magnetic fields(Sun:) solar wind(Sun:) solar-terrestrial relations

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