Results 251 to 260 of about 505,915 (296)

Structure of the Earth's bow shock

Journal of Geophysical Research, 1972
Numerical simulations have provided detailed information of the microscopic processes that occur in a high Mach number oblique shock wave such as the bow shock. The gross feature of the ion dissipation is a strong interaction of the reflected ions with the whistler precursor, which can be explained by a nonlinear ion-ion counterstreaming instability ...
Biskamp, D., Welter, H.
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Ion Acceleration at the Earth’s Bow Shock

Space Science Reviews, 2012
The Earth’s bow shock is the most studied example of a collisionless shock in the solar system. It is also widely used to model or predict the behaviour at other astrophysical shock systems. Spacecraft observations, theoretical modelling and numerical simulations have led to a detailed understanding of the bow shock structure, the spatial organization ...
Eberhard Moebius, D Burgess, M Scholer
exaly   +3 more sources

Cluster at the Bow Shock: Status and Outlook

Space Science Reviews, 2005
International ...
Scholer, M., Thomsen, M.F., Burgess, D., Bale, S.D., Balikhin, M.A., Balogh, A., Horbury, T.S., Krasnoselskikh, V.V., Kucharek, H., Lucek, E.A., Lembège, Bertrand, Mobius, E., Schwartz, S.J., Walker, S.N.   +13 more
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Interaction of interplanetary shocks with the bow shock

Planetary and Space Science, 2007
Abstract Fast forward interplanetary (IP) shocks have been identified as a source of large geomagnetic disturbances. However, the shocks can evolve in the solar wind, they are modified by interaction with the bow shock and during their propagation through the magnetosheath.
J. Šafránková, Z. Němeček, L. Přech, A.A. Samsonov, A. Koval, K. Andréeová   +5 more
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On the Earth’s Bow Shock Motion and Speed

Space Science Reviews, 1975
The Earth’s bow shock has been shown to have often a speed rather high (50–150 km s−1) on the basis of different methods of investigation (Formisano et al.,1971; Greenstadt et al., 1972; Formisano et al., 1973; Guha et al.,1972). The causes of the shock motion and speed are not well understood, the resonant oscillator proposed by Smit (1968) being not ...
V. Formisano, G. Mastrantonio
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Pulsar Bow-Shocks

AIP Conference Proceedings, 2005
The study of pulsar bow‐shocks is one of the most promising ways towards the understanding of the interactions between neutron stars relativistic winds and their environment. These objects are best resolved as Hα nebulae but velocity‐driven features are seen also in the radio and X‐ray bands and represent interesting targets for future gamma‐rays ...
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Planetary Bow Shocks

2013
Our present knowledge of the properties of the various planetary bow shocks is briefly reviewed. We do not follow the astronomical ordering of the planets. We rather distinguish between magnetised and unmagnetised planets which groups Mercury and Earth with the outer giant planets of the solar system, Mars and Moon in a separate group lacking magnetic ...
André Balogh, Rudolf A. Treumann
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Bow Shock Formation in a Complex Plasma

Physical Review Letters, 2012
A bow shock is observed in a two-dimensional supersonic flow of charged microparticles in a complex plasma. A thin conducting needle is used to make a potential barrier as an obstacle for the particle flow in the complex plasma. The flow is generated and the flow velocity is controlled by changing a tilt angle of the device under the gravitational ...
Y, Saitou, Y, Nakamura, T, Kamimura, O, Ishihara   +3 more
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The Heliosphere’s Interstellar Interaction: No Bow Shock

Science, 2012
No Shock Ahead of the Sun The boundary of the heliosphere is the region where the solar wind interacts with interstellar space, and it marks the edge of our solar system. Based on observations from NASA's Interstellar Boundary Explorer, McComas et al. (p.
D J, McComas, D, Alexashov, M, Bzowski, H, Fahr, J, Heerikhuisen, V, Izmodenov, M A, Lee, E, Möbius, N, Pogorelov, N A, Schwadron, G P, Zank   +10 more
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Propagation of Interplanetary Shocks Across the Bow Shock

AIP Conference Proceedings, 2010
An important problem of the Space Weather Program is the interaction of interplanetary (IP) shocks with the Earth magnetosphere because their interaction often (but not always) leads to major geomagnetic storms. Since the huge interaction region can be covered by simultaneous spacecraft observations only sporadically, global MHD modeling can help in ...
Zdeněk Nem̌ecěk, Jana Šafránková, Lubomír Přech, Andriy Koval, Jan Merka, M. Maksimovic, K. Issautier, N. Meyer-Vernet, M. Moncuquet, F. Pantellini   +9 more
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