Bonn 2020 – scientific programme
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EP: Fachverband Extraterrestrische Physik
EP 5: Sun and Heliosphere III
EP 5.2: Talk
Wednesday, April 1, 2020, 14:30–14:45, H-HS VIII
A numerical model of solar wind turbulence beyond the termination shock — •Jens Kleimann1, Sean Oughton2, and Horst Fichtner1 — 1Ruhr-Universität Bochum, 44780 Bochum, Germany — 2University of Waikato, Hamilton 3216, New Zealand
A pre-existing self-consistent model (Wiengarten et al. 2015, 2016) of incompressible MHD fluctuations and their transport in and interaction with the solar wind is extended into the inner heliosheath. This region has been explored in recent years by the two Voyager spacecraft that, particularly, provided evidence for compressive fluctuations. Dynamical equations for the Reynolds-averaged turbulence quantities, such as total fluctuation energy, cross-helicity and the associated lengthscales, are coupled to the large-scale single-fluid MHD equations and numerically integrated using the CRONOS code until a steady state is reached. This includes non-linear interactions with the background fields, as well as turbulence driving by pick-up ions and possibly other sources such as velocity shear. The resulting configurations are discussed and compared to those from other groups such as Usmanov et al. (2011, 2016).