SH027-05
Structure of the Heliosheath and Physical Processes in the Heliospheric Boundary Layer

Thursday, 10 December 2020: 17:36
Virtual
Nikolai V Pogorelov, University of Alabama in Huntsville, Department of Space Science, Huntsville, AL, United States, Federico Fraternale, University of Alabama in Huntsville, Center for Space Plasma and Aeronomic Research, Huntsville, AL, United States, Michael Gedalin, Ben-Gurion University of the Negev, Beer Sheva, Israel, Jacob Heerikhuisen, U of AL/Huntsville-CSPAR, Huntsville, AL, United States; University of Waikato, Hamilton, New Zealand, Tae K. Kim, Univ. of Alabama in Huntsville, CSPAR, Madison, AL, United States, Grzegorz Kowal, University of Sao Paulo, School of Arts, Sciences and Humanities, Sao Paulo, Brazil, Vadim Roytershteyn, Space Science Institute, Boulder, CO, United States and Ming Zhang, Florida Institute of Technology, Melbourne, FL, United States
Recorded Presentation
Abstract:
The solar wind (SW) interacts with the local interstellar medium (LISM) creating an outer heliosheath (OHS) in front of the heliopause. While the OHS can be considered as the LISM region affected by the presence of the heliosphere, the immediate vicinity of the heliopause is characterized by the presence of heliospheric boundary layer (HBL). In the HBL, the interstellar magnetic field (ISMF) drapes around the heliopause and defines the geometrical shape of the IBEX ribbon of enhanced energetic neutral atom (ENA) fluxes. The HBL structure is essentially determined by charge exchange between ions and neutral atoms. The topology of the heliopause and its orientation in space are also affected by charge exchange, which works to decrease the asymmetry of the heliosphere caused by the ISMF. The goal of this presentation is to describe major physical phenomena occurring near the heliopause and in the HBL: (1) ISMF draping the heliopause in stationary, non-stationary, and data-driven simulations; (2) plasma wave generation and radio emission from the HBL; (3) turbulent pre-shocks accompanied by changes in the Galactic cosmic ray (GCR) flux and its anisotropy; (4) global influence of the heliosphere on the surrounding LISM and its relation to observed anisotropies in the multi-TeV GCR flux, (4) instability of the heliopause and magnetic reconnection in its vicinity; and (5) the effect of pickup ions on the heliospheric interface. Simulation results are discussed in the context of observational data. The figure shows an "alien-view" of the heliosphere.
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