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Recent high resolution AIA/SDO images show evidence of the development of theKelvin-Helmholtz instability, as coronal mass ejections (CMEs) expand in theambient corona. A large-scale magnetic field mostly tangential to the interfaceis inferred, both on the CME and on the background sides. However, the magneticfield component along the shear flow is not strong enough to quench theinstability. There is also observational evidence that the ambient corona is ina turbulent regime, and therefore the criteria for the development of theinstability are a-priori expected to differ from the laminar case. To study theevolution of the Kelvin-Helmholtz instability with a turbulent background, weperform three-dimensional simulations of the incompressible magnetohydrodynamicequations. The instability is driven by a velocity profile tangential to theCME-corona interface, which we simulate through a hyperbolic tangent profile.The turbulent background is generated by the application of a stationarystirring force. We compute the instability growth-rate for different values ofthe turbulence intensity, and find that the role of turbulence is to attenuatethe growth. The fact that the Kelvin-Helmholtz instability is observed, sets anupper limit to the correlation length of the coronal background turbulence.

Simulations of the Kelvin-Helmholtz instability driven by coronal mass ejections in the turbulent corona