Supersonic solar wind ion flows downstream of the termination shock explained by a two-fluid shock model

DOI10.1051/0004-6361:200810679zbMath1156.85322OpenAlexW2015513230WikidataQ68674381 ScholiaQ68674381MaRDI QIDQ3614105

S. V. Chalov, Hans J. Fahr

Publication date: 16 March 2009

Published in: Astronomy & Astrophysics (Search for Journal in Brave)

Full work available at URL: https://doi.org/10.1051/0004-6361:200810679

zbMATH Keywords

shock wavessolar windhydrodynamics

Mathematics Subject Classification ID

Hydrodynamic and hydromagnetic problems in astronomy and astrophysics (85A30) Stability and instability of geophysical and astrophysical flows (76E20) Radiative transfer in astronomy and astrophysics (85A25)

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Gasdynamic models of physical phenomena occurring in the space. An overview ⋮ Phasespace transport of a quasi-neutral multi-fluid plasma over the solar wind MHD termination shock ⋮ Turbulent drag reduction by spanwise oscillations of a channel wall with porous layer ⋮ Enhanced drag-reduction over superhydrophobic surfaces with sinusoidal textures: a DNS study ⋮ The confrontation between general relativity and experiment

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