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THE MAGNETIC FIELD IN THE HELIOSHEATH
1992The interplanetary magnetic field (IMF) behaves in a reasonably well-understood manner between the Sun and the heliospheric termination shock. At the shock, the azimuthal field is amplified by a factor of four (for a strong shock) and undergoes secular amplification in the heliosheath until the flow is fully turned into the downstream direction and has
S.T. Suess, S. Nerney
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Crossing the Termination Shock into the Heliosheath: Magnetic Fields
Science, 2005Magnetic fields measured by Voyager 1 show that the spacecraft crossed or was crossed by the termination shock on about 16 December 2004 at 94.0 astronomical units. An estimate of the compression ratio of the magnetic field strength B (± standard error of the mean) across the shock is B 2
L F, Burlaga +6 more
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Voyager 1 in the Foreshock, Termination Shock, and Heliosheath
Science, 2005Voyager 1 (V1) began measuring precursor energetic ions and electrons from the heliospheric termination shock (TS) in July 2002. During the ensuing 2.5 years, average particle intensities rose as V1 penetrated deeper into the energetic particle foreshock of the TS.
R B, Decker +7 more
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Plasma and magnetic fields in the heliosheath
AIP Conference Proceedings, 2013This paper reviews recent results from the Voyager spacecraft in the heliosheath. The speed observed at Voyager 2 (V2) has been constant across the heliosheath, but the flow is turning significantly toward the heliotail. The V2 density and temperature decreased in 2008 and stayed low until 2011 when the density increased by a factor of 2 and the ...
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No meridional plasma flow in the heliosheath transition region
Nature, 2012Over a two-year period, Voyager 1 observed a gradual slowing-down of radial plasma flow in the heliosheath to near-zero velocity after April 2010 at a distance of 113.5 astronomical units from the Sun (1 astronomical unit equals 1.5 × 10(8) kilometres).
Robert B, Decker +3 more
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Observations of the Termination Shock and Heliosheath
2010Voyagers 1 and 2 have both crossed the solar wind termination shock and are now in the heliosheath, the region of shocked solar wind plasma before the heliopause. This paper reviews observations of the termination foreshock, the termination shock (TS), and the heliosheath.
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A comparison of magnetosheaths, ICME sheaths, and the heliosheath
AIP Conference Proceedings, 2007Sheaths are regions of compressed, heated, decelerated, and deflected flow behind a shock. We compare three types of sheath observed in the heliosphere, planetary magnetosheaths, ICME sheaths, and the heliosheath. Features common to these sheaths are plasma depletion layers, mirror mode waves, hot proton components, and asymmetries.
John D. Richardson, Ying Liu
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Anomalous cosmic rays in the heliosheath
AIP Conference Proceedings, 2012Contrary to some expectations, ACR spectra did not unfold to smooth power laws when the two Voyager spacecraft crossed the termination shock in December 2004 and August 2007, respectively. ACR fluxes continued to increase as Voyagers advanced deeper into the Heliosheath.
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The Heliosheath: The Ultimate Solar System Frontier
Astronomical Review, 2012AbstractThe recent measurements in-situby the Voyager spacecrafts, combined with the all-sky images of the heliospheric boundaries by the Interstellar Boundary Explorer (IBEX) mission have transformed radically our knowledge of the boundaries of the heliosphere. Concepts that lasted decades are being revisited due to their puzzling measurements.
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