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Paper: Interstellar Magnetic Field in the Nearest Surroundings of the Sun
Volume: 484, Outstanding Problems in Heliophysics: From Coronal Heating to the Edge of the Heliosphere
Page: 182
Authors: Ratkiewicz, R.; Strumik, M.; Grygorczuk, J.; Ben-Jaffel, L.
Abstract: A large number of results of MHD models of the interaction between the solar wind (SW) and the local interstellar medium (LISM) is available nowadays. A central assumption in these studies is that the unperturbed interstellar magnetic field (ISMF), which is unknown, has a constant intensity and direction. Therefore the main purpose of the investigations made by several groups of researchers is to find the specific ISMF parameters. In modeling of the interaction of the SW with the LISM, the boundary conditions play an essential role. The state of the LISM near the Sun and the behavior of the solar wind determine the shape and structure of the heliosphere. Results of theoretical modeling of the heliosphere are verified against in situ measurements and remote observations of the heliosphere. However, up to now most comparison efforts do not agree on a unique solution for the ISMF strength and orientation. We discuss possible reasons of the ambiguity by outlining differences and similarities of MHD models published up to now.
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