SIMULATIONS of the KELVIN-HELMHOLTZ INSTABILITY DRIVEN by CORONAL MASS EJECTIONS in the TURBULENT CORONA

Recent high-resolution Atmospheric Imaging Assembly/Solar Dynamics Observatory images show evidence of the development of the Kelvin-Helmholtz (KH) instability, as coronal mass ejections (CMEs) expand in the ambient corona. A large-scale magnetic field mostly tangential to the interface is inferred,...

Descripción completa

Guardado en:
Detalles Bibliográficos
Autores principales: Gomez, Daniel Osvaldo, Mininni, Pablo Daniel
Publicado: 2016
Materias:
instabilities
magnetohydrodynamics
Sun: coronal mass ejections
turbulence
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v818_n2_p_Gomez
http://hdl.handle.net/20.500.12110/paper_0004637X_v818_n2_p_Gomez
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v818_n2_p_Gomez
record_format dspace
spelling paper:paper_0004637X_v818_n2_p_Gomez2023-06-08T14:29:16Z SIMULATIONS of the KELVIN-HELMHOLTZ INSTABILITY DRIVEN by CORONAL MASS EJECTIONS in the TURBULENT CORONA Gomez, Daniel Osvaldo Mininni, Pablo Daniel instabilities magnetohydrodynamics Sun: coronal mass ejections turbulence Recent high-resolution Atmospheric Imaging Assembly/Solar Dynamics Observatory images show evidence of the development of the Kelvin-Helmholtz (KH) instability, as coronal mass ejections (CMEs) expand in the ambient corona. A large-scale magnetic field mostly tangential to the interface is inferred, both on the CME and on the background sides. However, the magnetic field component along the shear flow is not strong enough to quench the instability. There is also observational evidence that the ambient corona is in a turbulent regime, and therefore the criteria for the development of the instability are a priori expected to differ from the laminar case. To study the evolution of the KH instability with a turbulent background, we perform three-dimensional simulations of the incompressible magnetohydrodynamic equations. The instability is driven by a velocity profile tangential to the CME-corona interface, which we simulate through a hyperbolic tangent profile. The turbulent background is generated by the application of a stationary stirring force. We compute the instability growth rate for different values of the turbulence intensity, and find that the role of turbulence is to attenuate the growth. The fact that KH instability is observed sets an upper limit on the correlation length of the coronal background turbulence. © 2016. The American Astronomical Society. All rights reserved.. Fil:Gómez, D.O. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Mininni, P.D. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2016 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v818_n2_p_Gomez http://hdl.handle.net/20.500.12110/paper_0004637X_v818_n2_p_Gomez
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic instabilities
magnetohydrodynamics
Sun: coronal mass ejections
turbulence
spellingShingle instabilities
magnetohydrodynamics
Sun: coronal mass ejections
turbulence
Gomez, Daniel Osvaldo
Mininni, Pablo Daniel
SIMULATIONS of the KELVIN-HELMHOLTZ INSTABILITY DRIVEN by CORONAL MASS EJECTIONS in the TURBULENT CORONA
topic_facet instabilities
magnetohydrodynamics
Sun: coronal mass ejections
turbulence
description Recent high-resolution Atmospheric Imaging Assembly/Solar Dynamics Observatory images show evidence of the development of the Kelvin-Helmholtz (KH) instability, as coronal mass ejections (CMEs) expand in the ambient corona. A large-scale magnetic field mostly tangential to the interface is inferred, both on the CME and on the background sides. However, the magnetic field component along the shear flow is not strong enough to quench the instability. There is also observational evidence that the ambient corona is in a turbulent regime, and therefore the criteria for the development of the instability are a priori expected to differ from the laminar case. To study the evolution of the KH instability with a turbulent background, we perform three-dimensional simulations of the incompressible magnetohydrodynamic equations. The instability is driven by a velocity profile tangential to the CME-corona interface, which we simulate through a hyperbolic tangent profile. The turbulent background is generated by the application of a stationary stirring force. We compute the instability growth rate for different values of the turbulence intensity, and find that the role of turbulence is to attenuate the growth. The fact that KH instability is observed sets an upper limit on the correlation length of the coronal background turbulence. © 2016. The American Astronomical Society. All rights reserved..
author Gomez, Daniel Osvaldo
Mininni, Pablo Daniel
author_facet Gomez, Daniel Osvaldo
Mininni, Pablo Daniel
author_sort Gomez, Daniel Osvaldo
title SIMULATIONS of the KELVIN-HELMHOLTZ INSTABILITY DRIVEN by CORONAL MASS EJECTIONS in the TURBULENT CORONA
title_short SIMULATIONS of the KELVIN-HELMHOLTZ INSTABILITY DRIVEN by CORONAL MASS EJECTIONS in the TURBULENT CORONA
title_full SIMULATIONS of the KELVIN-HELMHOLTZ INSTABILITY DRIVEN by CORONAL MASS EJECTIONS in the TURBULENT CORONA
title_fullStr SIMULATIONS of the KELVIN-HELMHOLTZ INSTABILITY DRIVEN by CORONAL MASS EJECTIONS in the TURBULENT CORONA
title_full_unstemmed SIMULATIONS of the KELVIN-HELMHOLTZ INSTABILITY DRIVEN by CORONAL MASS EJECTIONS in the TURBULENT CORONA
title_sort simulations of the kelvin-helmholtz instability driven by coronal mass ejections in the turbulent corona
publishDate 2016
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v818_n2_p_Gomez
http://hdl.handle.net/20.500.12110/paper_0004637X_v818_n2_p_Gomez
work_keys_str_mv AT gomezdanielosvaldo simulationsofthekelvinhelmholtzinstabilitydrivenbycoronalmassejectionsintheturbulentcorona
AT mininnipablodaniel simulationsofthekelvinhelmholtzinstabilitydrivenbycoronalmassejectionsintheturbulentcorona
_version_ 1768546376595013632

Ejemplares similares