scholarly journals Observational Evidence for Solar Wind Proton Heating by Ion‐Scale Turbulence

2020 ◽  
Vol 47 (18) ◽  
Author(s):  
G. Q. Zhao ◽  
Y. Lin ◽  
X. Y. Wang ◽  
D. J. Wu ◽  
H. Q. Feng ◽  
...  
Keyword(s):  
Solar Wind ◽  
Observational Evidence ◽  
Solar Wind Proton ◽  
Scale Turbulence

scholarly journals The Location of Magnetic Reconnection at Earth’s Magnetopause

2021 ◽  
Vol 217 (3) ◽  
Author(s):  
K. J. Trattner ◽  
S. M. Petrinec ◽  
S. A. Fuselier
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Magnetic Reconnection ◽  
Ion Beams ◽  
Review Article ◽  
Observational Evidence ◽  
Magnetic Shear ◽  
General Direction ◽  
Shear Model ◽  
Wide Range

AbstractOne of the major questions about magnetic reconnection is how specific solar wind and interplanetary magnetic field conditions influence where reconnection occurs at the Earth’s magnetopause. There are two reconnection scenarios discussed in the literature: a) anti-parallel reconnection and b) component reconnection. Early spacecraft observations were limited to the detection of accelerated ion beams in the magnetopause boundary layer to determine the general direction of the reconnection X-line location with respect to the spacecraft. An improved view of the reconnection location at the magnetopause evolved from ionospheric emissions observed by polar-orbiting imagers. These observations and the observations of accelerated ion beams revealed that both scenarios occur at the magnetopause. Improved methodology using the time-of-flight effect of precipitating ions in the cusp regions and the cutoff velocity of the precipitating and mirroring ion populations was used to pinpoint magnetopause reconnection locations for a wide range of solar wind conditions. The results from these methodologies have been used to construct an empirical reconnection X-line model known as the Maximum Magnetic Shear model. Since this model’s inception, several tests have confirmed its validity and have resulted in modifications to the model for certain solar wind conditions. This review article summarizes the observational evidence for the location of magnetic reconnection at the Earth’s magnetopause, emphasizing the properties and efficacy of the Maximum Magnetic Shear Model.

scholarly journals Nature of Subproton Scale Turbulence in the Solar Wind

2013 ◽  
Vol 110 (22) ◽  
Author(s):  
C. H. K. Chen ◽  
S. Boldyrev ◽  
Q. Xia ◽  
J. C. Perez
Keyword(s):  
Solar Wind ◽  
Scale Turbulence

scholarly journals ARTEMIS Observations of Solar Wind Proton Scattering off the Lunar Surface

2018 ◽  
Vol 123 (7) ◽  
pp. 5289-5299 ◽  
Author(s):  
C. Lue ◽  
J. S. Halekas ◽  
A. R. Poppe ◽  
J. P. McFadden
Keyword(s):  
Solar Wind ◽  
Lunar Surface ◽  
Proton Scattering ◽  
Solar Wind Proton

A Turbulent Heliosheath Driven by Rayleigh Taylor Instability

2021 ◽  
Author(s):  
Merav Opher ◽  
James Drake ◽  
Gary Zank ◽  
Gabor Toth ◽  
Erick Powell ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Large Scale ◽  
Neutral Atom ◽  
Solar Magnetic Field ◽  
Characteristic Time Scale ◽  
Rayleigh Taylor Instability ◽  
Scale Turbulence ◽  
Magnetohydrodynamic Simulations ◽  
Rt Instability

Abstract The heliosphere is the bubble formed by the solar wind as it interacts with the interstellar medium (ISM). Studies show that the solar magnetic field funnels the heliosheath solar wind (the shocked solar wind at the edge of the heliosphere) into two jet-like structures1-2. Magnetohydrodynamic simulations show that these heliospheric jets become unstable as they move down the heliotail1,3 and drive large-scale turbulence. However, the mechanism that produces of this turbulence had not been identified. Here we show that the driver of the turbulence is the Rayleigh-Taylor (RT) instability caused by the interaction of neutral H atoms streaming from the ISM with the ionized matter in the heliosheath (HS). The drag between the neutral and ionized matter acts as an effective gravity which causes a RT instability to develop along the axis of the HS magnetic field. A density gradient exists perpendicular to this axis due to the confinement of the solar wind by the solar magnetic field. The characteristic time scale of the instability depends on the neutral H density in the ISM and for typical values the growth rate is ~ 3 years. The instability destroys the coherence of the heliospheric jets and magnetic reconnection ensues, allowing ISM material to penetrate the heliospheric tail. Signatures of this instability should be observable in Energetic Neutral Atom (ENA) maps from future missions such as IMAP4. The turbulence driven by the instability is macroscopic and potentially has important implications for particle acceleration.

scholarly journals Interplanetary Response to Solar Long Time-Scale Phenomena

1980 ◽  
Vol 91 ◽  
pp. 105-125
Author(s):  
C. D'Uston ◽  
J. M. Bosqued
Keyword(s):  
Solar Wind ◽  
Time Scale ◽  
High Speed ◽  
Coronal Holes ◽  
Observational Evidence ◽  
Solar Wind Flow ◽  
Speed Solar Wind ◽  
Long Time ◽  
Outer Corona ◽  
High Speed Solar Wind

In this paper, we briefly review the experimental knowledge gained in the recent years on the interplanetary response to solar long-time scale phenomena such as the coronal magnetic structure and its evolution. Observational evidence that solar wind flow in the outer corona comes from the unipolar diverging magnetic regions of the photosphere is discussed along with relations to coronal holes. High-speed solar wind streams observed within the boundary of interplanetary magnetic sectors are associated with these structures. Their boundaries appear as very narrow velocity shears.

On the origin of solar wind proton thermal anisotropy

1973 ◽  
Vol 78 (28) ◽  
pp. 6451-6468 ◽  
Author(s):  
W. C. Feldman ◽  
J. R. Asbridge ◽  
S. J. Bame ◽  
M. D. Montgomery
Keyword(s):  
Solar Wind ◽  
Solar Wind Proton ◽  
Thermal Anisotropy

scholarly journals Reconstruction of Helio-Latitudinal Structure of the Solar Wind Proton Speed and Density

Solar Physics ◽  
2015 ◽  
Vol 290 (9) ◽  
pp. 2589-2615 ◽  
Author(s):  
Justyna M. Sokół ◽  
Paweł Swaczyna ◽  
Maciej Bzowski ◽  
Munetoshi Tokumaru
Keyword(s):  
Solar Wind ◽  
Solar Wind Proton
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