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Intense plasma waves at and near the solar wind termination shock
Nature, 2008Plasma waves are a characteristic feature of shocks in plasmas, and are produced by non-thermal particle distributions that develop in the shock transition layer. The electric fields of these waves have a key role in dissipating energy in the shock and driving the particle distributions back towards thermal equilibrium.
D A, Gurnett, W S, Kurth
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Electron Plasma Oscillations Upstream of the Solar Wind Termination Shock
Science, 2005Electron plasma oscillations have been detected upstream of the solar wind termination shock by the plasma wave instrument on the Voyager 1 spacecraft. These waves were first observed on 11 February 2004, at a heliocentric radial distance of 91.0 astronomical units, and continued sporadically with a gradually increasing occurrence rate for nearly a ...
D A, Gurnett, W S, Kurth
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UV remote detection of the solar wind termination shock
Advances in Space Research, 1995Abstract The location of the solar wind termination shock is currently one of the most interesting questions in Space Physics, since it has now become possible to detect and locate its position using the four deep space probes, Pioneers 10 11 and Voyagers 1 2 .
P Gangopadhyay, D.L Judge
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Acceleration of Pick-up Ions at the Solar Wind Termination Shock
Astrophysics and Space Science, 2000It is generally accepted that pick-up ions act as a seed population for anomalous cosmic rays originating at the solar wind termination shock. We believe that the ion pre-acceleration process operating in the heliosphere up to the termination shock can be very important to inject the ions into the shock acceleration process.
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AIP Conference Proceedings, 2010
The Voyager‐2 observations at the recent crossing of the solar wind termination shock show that the downstream thermal protons still move with supersonic speed. Obviously it is due to their inefficient shock‐heating and that the surpathermal ions absorb most of the upstream kinetic solar wind energy.
Sergei V. Chalov +6 more
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The Voyager‐2 observations at the recent crossing of the solar wind termination shock show that the downstream thermal protons still move with supersonic speed. Obviously it is due to their inefficient shock‐heating and that the surpathermal ions absorb most of the upstream kinetic solar wind energy.
Sergei V. Chalov +6 more
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Cool heliosheath plasma and deceleration of the upstream solar wind at the termination shock
Nature, 2008The solar wind blows outward from the Sun and forms a bubble of solar material in the interstellar medium. The termination shock occurs where the solar wind changes from being supersonic (with respect to the surrounding interstellar medium) to being subsonic.
John D, Richardson +4 more
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Solar wind conditions in the outer heliosphere and the distance to the termination shock
Journal of Geophysical Research: Space Physics, 1993The Plasma Science experiment on the Voyager 2 spacecraft has measured to date the properties of solar wind protons from 1 to 40.4 AU. We use these observations to discuss the probable location and motion of the termination shock of the solar wind. A least squares fit of proton ram pressure to heliocentric distance R over this distance yields a ram ...
John W. Belcher +3 more
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Energetic particles near and beyond the solar-wind termination
AIP Conference Proceedings, 2006A global picture of the transport and acceleration of energetic particles in the heliosphere has evolved over the last few decades, which has successfully explained many features of the modulation of galactic cosmic rays and the transport of anomalous cosmic rays and their acceleration by the solar‐wind termination shock.
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The Longitudinal Distribution of Anomalous Hydrogen near the Solar Wind Termination Shock
Advances in Space Research, 1993Gasdynamic calculations show that the solar wind termination shock has a prolate shape. Consequently, the angle between the shock normal vector and the magnetic field lines varies with the variation of longitude. Near the ecliptic, the minimum speed for an upstream ion to be reflected by the shock, or for a downstream ion to overtake the shock ...
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Acceleration of galactic and Jovian electrons at the heliospheric solar wind termination shock
Advances in Space Research, 1997Abstract In 1973, with the aid of the Pioneer 10 spacecraft, it was discovered that the Jovian (Jupiter) magnetosphere at 5 AU is a relatively strong source of electrons with energies up to even ∼100 MeV. The most recent direct observational confirmation was in 1992 with the Ulysses spacecraft.
L.J. Haasbroek +2 more
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