Results 51 to 60 of about 728 (195)
Energetic Neutral Atoms from the Heliosheath as an Additional Population of Neutral Hydrogen in the Inner Heliosphere [PDF]
, 2019 Interstellar neutral hydrogen (ISN H) gas penetrates freely the heliopause. Inside the inner heliosheath, the chargeexchange interaction of this gas with the shocked solar wind and pickup ions creates energetic neutral atoms (ENAs).
Bzowski, M., Galli, André
core +2 more sources
Dispersive Fast Magnetosonic Waves and Shock‐Driven Compressible Turbulence in the Inner Heliosheath [PDF]
, 2020 The solar wind in the inner heliosheath beyond the termination shock (TS) is a nonequilibrium collisionless plasma consisting of thermal solar wind ions, suprathermal pickup ions, and electrons.
Opher, Merav +7 more
core +1 more source
On the generation of compressible mirror-mode fluctuations in the inner heliosheath [PDF]
, 2020 Measurements made with the Voyager 1 spacecraft indicate that significant levels of compressive fluctuations exist in the inner heliosheath. Some studies have already been performed with respect to the mirror-mode instability in the downstream region ...
Fichtner, Horst +5 more
core +1 more source
PLASMA IN THE HELIOSHEATH: 3.5 YEARS OF OBSERVATIONS [PDF]
The Astrophysical Journal, 2011 Voyager 2 (V2) has observed heliosheath (HSH) plasma since 2007 August. We describe how the plasma has evolved across the HSH. We show that the low solar wind dynamic pressure leads to an inward movement of the termination shock (TS) of about 10 AU to a minimum position of 73 AU in 2010.
Wang, C., Richardson, John D.
openaire +3 more sources
Magnetic Decreases (MDs) and mirror modes: two different plasma β changing mechanisms [PDF]
Nonlinear Processes in Geophysics, 2010 We discuss two different physical processes that create localized high β plasma regions. One is nonlinear wave-steepening, generating magnetic decreases (MDs) by a ponderomotive force.
E. Echer +4 more
doaj +1 more source
Mapping the magnetic mayhem in the heliosheath [PDF]
Eos, Transactions American Geophysical Union, 2011 When Voyager 1 passed into the heliosheath in 2004, it became the first human‐made object to explore the remote edge of the Sun's magnetic influence. The heliosheath, between 1.5 and 15 billion kilometers thick and starting roughly 14 billion kilometers from the Sun, is where the outgoing flows of solar wind start to be pushed back by interstellar ...
openaire +1 more source
HSTOF ENA observations and energetic ion distributions in the heliosheath
, 2012 Context. Launched in 1996, HSTOF on board SOHO was the first instrument to detect the energetic neutral atoms (ENA) from the heliosheath.
Hsieh, K. +5 more
core +1 more source
Large-scale Field-aligned Flows in the Heliosheath
The Astrophysical JournalWe use a state-of-the-art 3D MHD simulation to show that large-scale thermal pressure gradients in the heliosheath drive suprathermal particles (pickup ions with 1–5 keV) to stream along magnetic field lines faster than the cold bulk solar wind.
Merav Opher +9 more
doaj +1 more source
Lyα Absorption from Heliosheath Neutrals [PDF]
The Astrophysical Journal, 2007 We assess the information that HST observations of stellar Lyα lines can provide on the heliosheath, the region of the heliosphere between the termination shock and heliopause. To search for evidence of heliosheath absorption, we conduct a systematic inspection of stellar Lyα lines reconstructed after correcting for ISM absorption (and heliospheric ...
Brian E. Wood +3 more
openaire +1 more source
The problem with the non-idealness of the MHD heliosheath [PDF]
Astrophysics and Space Sciences Transactions, 2006 When describing the plasma - field behaviour in the heliospheric interface the difficulty arises that classical MHD concepts are not fully applicable to this complicated multifluid interaction scenario. The classical MHD concept of ideally frozen-in magnetic fields is only strictly valid, if the magnetized medium is fully ionized.
Baranov, V. B., Fahr, H.-J.
openaire +3 more sources