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Conditions for the existence of Kelvin-Helmholtz instability in a CME

Published online by Cambridge University Press:  09 September 2016

Andrés Páez ,
Vera Jatenco-Pereira ,
Diego Falceta-Gonçcalves  and
Merav Opher
Andrés Páez
Affiliation:
Universidade de São Paulo, Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Rua do Matão 1226, São Paulo, SP, 05508-090, Brazil email: [email protected]
Vera Jatenco-Pereira
Affiliation:
Universidade de São Paulo, Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Rua do Matão 1226, São Paulo, SP, 05508-090, Brazil email: [email protected]
Diego Falceta-Gonçcalves
Affiliation:
Universidade de São Paulo, Escola de Artes, Ciências e Humanidades, Rua Arlindo Bettio 1000, São Paulo, SP, 03828-000, Brazil email: [email protected]
Merav Opher
Affiliation:
Astronomy Department, Boston University, Boston, MA 02215, USA email: [email protected]
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Abstract

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The presence of Kelvin-Helmholtz instability (KHI) in the sheaths of Coronal Mass Ejections (CMEs) has been proposed and observed by several authors in the literature. In the present work, we assume their existence and propose a method to constrain the local properties, like the CME magnetic field intensity for the development of KHI. We study a CME in the initiation phase interacting with the slow solar wind (Zone I) and with the fast solar wind (Zone II). Based on the theory of magnetic KHI proposed by Chandrasekhar (1961) we found the radial heliocentric interval for the KHI existence, in particular we constrain it with the CME magnetic field intensity. We conclude that KHI may exist in both CME Zones but it is perceived that Zone I is more appropriated for the KHI formation.

Keywords

SunCoronal mass ejectionKelvin-Helmholtz instability
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 218 - 220
Copyright
Copyright © International Astronomical Union 2016 

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