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,...
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todo:paper_0004637X_v818_n2_p_Gomez2023-10-03T14:02:39Z SIMULATIONS of the KELVIN-HELMHOLTZ INSTABILITY DRIVEN by CORONAL MASS EJECTIONS in the TURBULENT CORONA Gómez, D.O. Deluca, E.E. Mininni, P.D. 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. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar 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 Gómez, D.O. Deluca, E.E. Mininni, P.D. 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.. |
| format |
JOUR |
| author |
Gómez, D.O. Deluca, E.E. Mininni, P.D. |
| author_facet |
Gómez, D.O. Deluca, E.E. Mininni, P.D. |
| author_sort |
Gómez, D.O. |
| 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 |
| url |
http://hdl.handle.net/20.500.12110/paper_0004637X_v818_n2_p_Gomez |
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AT gomezdo simulationsofthekelvinhelmholtzinstabilitydrivenbycoronalmassejectionsintheturbulentcorona AT delucaee simulationsofthekelvinhelmholtzinstabilitydrivenbycoronalmassejectionsintheturbulentcorona AT mininnipd simulationsofthekelvinhelmholtzinstabilitydrivenbycoronalmassejectionsintheturbulentcorona |
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1807316187619524608 |