2015/09/29 by V. Izmodenov, Vladislav Izmodenov, Dmitry Alexashov +1 · 165 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astronomy #Astrophysics #Atmospheric Ozone and Climate #Classical mechanics #Computational physics #Galaxy #Heliosphere #Interstellar medium #Ionosphere and magnetosphere dynamics #Kinetic energy #Magnetic field #Magnetohydrodynamics #Physics #Solar and Space Plasma Dynamics #Solar wind #astro-ph.SR #physics.space-ph
paper · pdf · doi:10.1088/0067-0049/220/2/32
published in The Astrophysical Journal Supplement Series 220(2), 32 (Institute of Physics) · The Astrophysical Journal Supplement Series, Special Issue, 2015
arxiv created 2015/09/29 · openalex publication_date 2015/10/20 · arxiv updated 2015/10/28 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
This paper provides a detailed description of the latest version of our model of the solar wind (SW) interaction with the local interstellar medium (LISM). This model has already been applied to the analysis of Ly α absorption spectra toward nearby stars and for analyses of Solar and Heliospheric Observatory /SWAN data. Katushkina et al. (this issue) used the model results to analyze IBEX -Lo data. At the same time, the details of this model have not yet been published. This is a three-dimensional (3D) kinetic-magnetohydrodynamical (MHD) model that takes into account SW and interstellar plasmas (including α particles in SW and helium ions in LISM), the solar and interstellar magnetic fields, and interstellar hydrogen atoms. The latitudinal dependence of SW and the actual flow direction of the interstellar gas with respect to the Sun are also taken into account in the model. It was very essential that our numerical code was developed in such a way that any numerical diffusion or reconnection across the heliopause were not allowed in the model. The heliospheric current sheet is a rotational discontinuity in the ideal MHD and can be treated kinematically. In the paper, we focus in particular on the effects of the heliospheric magnetic field and on the heliolatitudinal dependence of SW.