KelvinHelmholtz: Kelvin-Helmholtz Instability

Section author: Axel Huebl <a.huebl (at) hzdr.de>

Module author: Axel Huebl <a.huebl (at) hzdr.de>, E. Paulo Alves, Thomas Grismayer

This example simulates a shear-flow instability known as the Kelvin-Helmholtz Instability in a near-relativistic setup as studied in [Alves12], [Grismayer13], [Bussmann13]. The default setup uses a pre-ionized quasi-neutral hydrogen plasma. Modifiying the ion species’ mass to resample positrons instead is a test we perform regularly to control numerical heating and charge conservation.

References

Alves12

E.P. Alves, T. Grismayer, S.F. Martins, F. Fiuza, R.A. Fonseca, L.O. Silva. Large-scale magnetic field generation via the kinetic kelvin-helmholtz instability in unmagnetized scenarios, The Astrophysical Journal Letters (2012), https://dx.doi.org/10.1088/2041-8205/746/2/L14

Grismayer13

T. Grismayer, E.P. Alves, R.A. Fonseca, L.O. Silva. dc-magnetic-field generation in unmagnetized shear flows, Physical Reveview Letters (2013), https://doi.org/10.1103/PhysRevLett.111.015005

Bussmann13

M. Bussmann, H. Burau, T.E. Cowan, A. Debus, A. Huebl, G. Juckeland, T. Kluge, W.E. Nagel, R. Pausch, F. Schmitt, U. Schramm, J. Schuchart, R. Widera. Radiative Signatures of the Relativistic Kelvin-Helmholtz Instability, Proceedings of the International Conference on High Performance Computing, Networking, Storage and Analysis (2013), http://doi.acm.org/10.1145/2503210.2504564