TY - GEN

T1 - Pickup ions in the heliosphere

AU - Pogorelov, Nikolai

AU - Arge, Charles N.

AU - Gedalin, Michael

AU - Kim, Tae

AU - Renfroe, Kyle

AU - Roytershteyn, Vadim

AU - Zhang, Ming

PY - 2019

Y1 - 2019

N2 - Charge exchange between the solar wind (SW) protons and H atoms in the
local interstellar medium (LISM) gives birth to non-thermal, pickup ions
(PUIs). The distribution function of PUIs created this way quickly
becomes isotropic, but Maxwellian equilibrium is not reached. This
raises questions about the proper description of PUIs crossing
collisionless shocks, which are abundant in the space plasma. We discuss
numerical approaches to modeling the flow of the mixture of thermal and
non-thermal ions which constitute the SW. In particular, the
observational data sets suitable for the validation of numerical
simulations are discussed. We also compare solutions where PUIs are
treated as a separate component of plasma with those where the plasma is
assumed to be in Maxwellian equilibrium. Finally, we analyze the
boundary conditions on the distribution functions and bulk properties of
the SW flow and heliospheric magnetic field at collisionelss shocks,
e.g., the heliospheric termination shock. Numerical simulations are
compared with observations.
This work was supported, in part, by NASA Grant 80NSSC18K1649.

AB - Charge exchange between the solar wind (SW) protons and H atoms in the
local interstellar medium (LISM) gives birth to non-thermal, pickup ions
(PUIs). The distribution function of PUIs created this way quickly
becomes isotropic, but Maxwellian equilibrium is not reached. This
raises questions about the proper description of PUIs crossing
collisionless shocks, which are abundant in the space plasma. We discuss
numerical approaches to modeling the flow of the mixture of thermal and
non-thermal ions which constitute the SW. In particular, the
observational data sets suitable for the validation of numerical
simulations are discussed. We also compare solutions where PUIs are
treated as a separate component of plasma with those where the plasma is
assumed to be in Maxwellian equilibrium. Finally, we analyze the
boundary conditions on the distribution functions and bulk properties of
the SW flow and heliospheric magnetic field at collisionelss shocks,
e.g., the heliospheric termination shock. Numerical simulations are
compared with observations.
This work was supported, in part, by NASA Grant 80NSSC18K1649.

M3 - פרסום בספר כנס

BT - APS Division of Plasma Physics Meeting 2019

ER -