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

被引：0

作者：

Paez, Andres ^{[1
]}

Jatenco-Pereira, Vera ^{[1
]}

Falceta-Goncalves, Diego ^{[2
]}

Opher, Merav ^{[3
]}

机构：

[1] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226, BR-05508090 Sao Paulo, SP, Brazil

[2] Univ Sao Paulo, Escola Artes Ciencias & Humanidades, Rua Arlindo Bettio 1000, BR-03828000 Sao Paulo, SP, Brazil

[3] Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA

来源：

SOLAR AND STELLAR FLARES AND THEIR EFFECTS ON PLANETS | 2016年 / 11卷 / S320期

关键词：

Sun; Coronal mass ejection; Kelvin-Helmholtz instability; SOLAR-WIND VELOCITY;

D O I：

10.1017/S1743921316008656

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页码：218 / 220

页数：3

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