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Influence of a density increase on the evolution of the Kelvin-Helmholtz instability and vortices / U. V. Amerstorfer [et al.] // Phys. Plasmas. - 2010. - Vol. 17, Is. 7. - Ст. 72901, DOI 10.1063/1.3453705. - Cited References: 26. - This work was supported by the FWF under Project No. P21051-N16 and also by the RFBR under Grant No. 09-05-91000-ANF_a. . - ISSN 1070-664X

РУБ Physics, Fluids & Plasmas
Рубрики:
VENUS IONOPAUSE
   SIMULATION
   SCHEMES
   PLASMA
   FLOW
Кл.слова (ненормированные):
A-density -- Kelvin-Helmholtz instabilities -- Linear growth -- Loss rates -- Nonlinear numerical simulation -- Nonlinear phase -- Nonregular structures -- Plasma clouds -- Plasma layer -- Regular structure -- Spatial scale -- Turbulent phase -- Upper layer -- Boundary layers -- Helmholtz equation -- Ionosphere -- Plasma density -- Solar wind -- Magnetoplasma
Аннотация: Results of two-dimensional nonlinear numerical simulations of the magnetohydrodynamic Kelvin-Helmholtz instability are presented. A boundary layer of a certain width is assumed, which separates the plasma in the upper layer from the plasma in the lower layer. A special focus is given on the influence of a density increase toward the lower layer. The evolution of the Kelvin-Helmholtz instability can be divided into three different phases, namely, a linear growth phase at the beginning, followed by a nonlinear phase with regular structures of the vortices, and finally, a turbulent phase with nonregular structures. The spatial scales of the vortices are about five times the initial width of the boundary layer. The considered configuration is similar to the situation around unmagnetized planets, where the solar wind (upper plasma layer) streams past the ionosphere (lower plasma layer), and thus the plasma density increases toward the planet. The evolving vortices might detach around the terminator of the planet and eventually so-called plasma clouds might be formed, through which ionospheric material can be lost. For the special case of a Venus-like planet, loss rates are estimated, which are of the order of estimated loss rates from observations at Venus. (C) 2010 American Institute of Physics. [doi:10.1063/1.3453705]

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Держатели документа:
[Amerstorfer, U. V.
Biernat, H. K.] Austrian Acad Sci, Inst Space Res, A-8042 Graz, Austria
[Erkaev, N. V.] Siberian Fed Univ, Krasnoyarsk 660041, Russia
[Erkaev, N. V.] Inst Computat Modelling, Krasnoyarsk 660036, Russia
[Taubenschuss, U.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA
[Biernat, H. K.] Karl Franzens Univ Graz, Inst Phys, A-8010 Graz, Austria
ИВМ СО РАН
Space Research Institute, Austrian Academy of Sciences, 8042 Graz, Austria
Siberian Federal University, 660041 Krasnoyarsk, Russian Federation
Institute of Computational Modelling, 660036 Krasnoyarsk, Russian Federation
Department of Physics and Astronomy, University of Iowa, Iowa City, IA 52242-1479, United States
Institute of Physics, Karl-Franzens-University Graz, 8010 Graz, Austria

Доп.точки доступа:
Amerstorfer, U. V.; Erkaev, N. V.; Еркаев, Николай Васильевич; Taubenschuss, U.; Biernat, H. K.
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