Physics
Scientist
Institute of Geophysics and Planetary Physics, University of California, Riverside, CA 92521, USA; Institute for Problems in Mechanics, RAS, 101-1 Vernadskii Avenue, Moscow, 119526 Russian Federation für Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching bei München, Germany
IGPP, University of California, Riverside, CA 92521, USA of Geophysics and Planetary Physics, University of California, Riverside, CA 92521; Institute for Problems in Mechanics, Russian Academy of Sciences, 101-1 Vernadskii Ave., 119526 Moscow, Russia
Institute for Problems in Mechanics, Russian Academy of Sciences, pr. Vernadskogo 101, Moscow, 117526 Russia
Institute of Geophysics and Planetary Physics, University of California, 900 University Avenue, Riverside, CA 92521, USA; Institute for Problems in Mechanics, Russian Academy of Sciences, 101-1 Vernadskii Avenue, Moscow, 119526, Russian Federation of Geophysics and Planetary Physics, University of California, 900 University Avenue, Riverside, CA 92521, USA of Geophysics and Planetary Physics, University of California, Riverside, CA 92521; Institute for Problems in Mechanics, Russian Academy of Sciences, 101-1 Vernadskii Avenue, Moscow 117526, Russia
Institute of Geophysics and Planetary Physics, University of California, 900 University Avenue, Riverside, CA 92521, USA Academy of Sciences, Institute for Problems in Mechanics, Vernadskii Avenue 101-1, Moscow 117526, Russia, ; and Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85740 Garching bei München, Germany ula, of Geophysics and Planetary Physics, University of California, Riverside, CA 92521 for Problems in Mechanics, Russian Academy of Sciences 101-1 Vernadskii Avenue, Moscow 117526, Russia
A New, Three-dimensional, Adaptive Mesh Refinement Code for Modeling Flows of Partially Ionized Plasma
Accretion Flows: Aspects of Gas Dynamic Modeling
Adaptive Mesh Refinement on Curvilinear Grids
Consequences of the Heliopause Instability Caused by Charge Exchange
Global MHD--Boltzmann model of the outer heliosphere based on high-resolution shock-capturing methods, adaptive mesh refinement techniques, and Monte Carlo simulations
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