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Superdiffusive Transport Upstream of the Solar Wind Termination Shock
AIP Conference Proceedings, 2010In this work the properties of transport of ions accelerated at the solar wind termination shock are studied. The approach used to investigate the propagation of those particles is probabilistic and is based on the analysis of particle time profiles upstream of the shock front.
Nicole Meyer-Vernet +2 more
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Magnetic Fields In The Termination Shock, Heliosheath And Solar Wind
AIP Conference Proceedings, 2008This paper will discuss recent magnetic field observations of the termination shock (TS), heliosheath (HSH), and supersonic solar wind (SW) made by Voyager 1 (V1) and Voyager 2 (V2). Voyager 2 crossed the TS at least 5 times at 83.7 AU and 27.5deg South heliographic latitude during 2007/242.14 to 244.80. The structure of the shock, observed on three of
Gary P Zank +2 more
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Is the solar wind termination shock a cosmic-ray mediated shock?
AIP Conference Proceedings, 2006Based on observations near Earth’s orbit with the CELIAS/STOF sensor on board SOHO and with the ACE magnetometer, and on the model of Zank et al. we calculate the evolution of transport parameters of energetic particles over heliocentric distance.
Kallenbach, R., Hilchenbach, M.
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Challenges to cosmic ray modeling: From beyond the solar wind termination shock
Advances in Space Research, 2008Abstract Voyager 1 crossed the solar wind termination shock on December 16, 2004 at a distance of 94 AU from the Sun, to become the first spacecraft to explore the termination shock region and to enter the heliosheath, the final heliospheric frontier. By the end of 2006, Voyager 1 will be at ∼101 AU, with Voyager 2 at ∼81 AU and still approaching the
M S Potgieter
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Effect of interstellar neutral hydrogen on the termination of the solar wind
Journal of Geophysical Research, 1970The effect of charge exchange and photoionization of neutral hydrogen penetrating the supersonic solar wind region from the interstellar medium is taken into account by constructing appropriate source terms for the equations of the flow. The equations are solved numerically for densities of 1, 5, and 10 cm−3 in the interstellar medium. It is shown that
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The termination of the solar wind
Icarus, 1971Abstract It has previously been suggested that the solar wind might terminate at distances of 5 AU to 20 AU from the Sun, and that the solar wind might be drastically slowed down by charge exchange and photoionization of interstellar hydrogen atoms which approach the Sun.
Thomas R. McDonough, Neil M. Brice
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An asymmetric solar wind termination shock
Nature, 2008Voyager 2 crossed the solar wind termination shock at 83.7 au in the southern hemisphere, approximately 10 au closer to the Sun than found by Voyager 1 in the north. This asymmetry could indicate an asymmetric pressure from an interstellar magnetic field, from transient-induced shock motion, or from the solar wind dynamic pressure.
Stone, Edward C. +5 more
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The solar wind shock termination
Advances in Space Research, 1986Abstract We analyse the possibility that the shock termination of the solar wind should occur at a heliocentric distance of 50 a.u. It is concluded that this is possible if the density of the interstellar medium near the Sun is of the order of 0.5 cm −3 , or the pressure of low energy cosmic rays (less than about 300 MeV/nucleon) is of the order of 6×
Axford, W., Ip, W.
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Magnetic fields at the solar wind termination shock
Nature, 2008A transition between the supersonic solar wind and the subsonic heliosheath was observed by Voyager 1, but the expected termination shock was not seen owing to a gap in the telemetry. Here we report observations of the magnetic field structure and dynamics of the termination shock, made by Voyager 2 on 31 August-1 September 2007 at a distance of 83.7 ...
L F, Burlaga +5 more
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Electrostatic Short-Scale Termination of Solar-Wind Turbulence
Physical Review Letters, 2009Recent hybrid Vlasov simulations [F. Valentini, Phys. Rev. Lett. 101, 025006 (2008)10.1103/PhysRevLett.101.025006] have shown that the short-scale termination of solar-wind turbulence is characterized by the occurrence of longitudinal electrostatic fluctuations.
VALENTINI, Francesco, VELTRI, Pierluigi
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