Electrostatic analyzer design for solar wind proton measurements with high temporal, energy, and angular resolutions

2017 ◽  
Vol 122 (2) ◽  
pp. 1439-1450 ◽  
Author(s):  
Antoine Cara ◽  
Benoit Lavraud ◽  
Andrei Fedorov ◽  
Johan De Keyser ◽  
Rossana DeMarco ◽  
...  
Keyword(s):  
Solar Wind ◽  
Solar Wind Proton ◽  
Electrostatic Analyzer

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

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

scholarly journals Hybrid Simulations of Solar Wind Proton Precipitation to the Surface of Mercury

2020 ◽  
Vol 125 (4) ◽  
Author(s):  
S. Fatemi ◽  
A. R. Poppe ◽  
S. Barabash
Keyword(s):  
Solar Wind ◽  
Solar Wind Proton ◽  
Proton Precipitation ◽  
Hybrid Simulations

scholarly journals MIXING THE SOLAR WIND PROTON AND ELECTRON SCALES: EFFECTS OF ELECTRON TEMPERATURE ANISOTROPY ON THE OBLIQUE PROTON FIREHOSE INSTABILITY

2016 ◽  
Vol 832 (1) ◽  
pp. 64 ◽  
Author(s):  
Y. Maneva ◽  
M. Lazar ◽  
A. Viñas ◽  
S. Poedts
Keyword(s):  
Solar Wind ◽  
Electron Temperature ◽  
Temperature Anisotropy ◽  
Solar Wind Proton

Solar wind proton precipitation to the surface of Mercury

2020 ◽  
Author(s):  
Shahab Fatemi ◽  
Andrew R. Poppe ◽  
Stas Barabash
Keyword(s):  
Solar Wind ◽  
Dynamic Pressure ◽  
Solar Wind Plasma ◽  
Solar Wind Dynamic Pressure ◽  
Solar Wind Proton ◽  
Entire Surface ◽  
The North ◽  
Proton Precipitation ◽  
Neutral Sodium ◽  
The Imf

<p>We examine the effects of the interplanetary magnetic field (IMF) orientation and solar wind dynamic pressure on the solar wind proton precipitation to the surface of Mercury. We use the Amitis model, a three-dimensional GPU-based hybrid model of plasma (particle ions and fluid electrons), and explain a method we found necessary to accurately calculate plasma precipitation to the surface of Mercury through the highly dynamic Hermean magnetosphere. We use our model to explain ground-based telescope observations of Mercury's neutral sodium exosphere, and compare our simulation results with MESSENGER observations. For the typical solar wind dynamic pressure near the orbit of Mercury (i.e., ~7-8 nPa) our model shows a high solar wind proton flux precipitates through the magnetospheric cusps to the high latitudes on both hemispheres on the dayside with a higher precipitation rate to the southern hemisphere compared to the north, which is associated with the northward displacement of Mercury's intrinsic magnetic dipole. We show that this two peak pattern, which is also a common feature observed for neutral sodium exosphere, is controlled by the radial component (B<sub>x</sub>) of the IMF and not the B<sub>z</sub> component. Our model also suggests that the southward IMF and its associated magnetic reconnection do not play a major role in controlling plasma precipitation to the surface of Mercury through the magnetospheric cusps, in agreement with MESSENGER observations that show that, unlike the Earth, there is almost no dependence between the IMF angle and magnetic reconnection rate at Mercury. For the typical solar wind dynamic pressure, our model suggests that the solar wind proton precipitation through the cusps is longitudinally centered near noon with ~11<sup>o</sup> latitudinal extent in the north and ~21<sup>o</sup> latitudinal extent in the south, which is consistent with MESSENGER observations. We found an anti-correlation in the incidence area on the surface and the incidence particle rate between the northern and southern cusp precipitation such that the total area and the total rate through both of the cusps remain constant and independent of the IMF orientation. We also show that the solar wind proton incidence rate to the entire surface of Mercury is higher when the IMF has a northward component and nearly half of the incidence flux impacts the low latitudes on the nightside. During extreme solar events (e.g., Coronal Mass Ejections) a large area on the dayside surface of Mercury is exposed to the solar wind plasma, especially in the southern hemisphere. Our model suggests that over 70 nPa solar wind dynamic pressure is required for the entire surface of Mercury to be exposed to the solar wind plasma.</p>

Solar wind proton flux extremes and their association with pseudostreamers

2013 ◽  
Author(s):  
Liang Zhao ◽  
Sarah E. Gibson ◽  
Lennard A. Fisk
Keyword(s):  
Solar Wind ◽  
Proton Flux ◽  
Solar Wind Proton

scholarly journals Dependence of Solar Wind Proton Temperature on the Polarization Properties of Alfvénic Fluctuations at Ion-kinetic Scales

2021 ◽  
Vol 912 (2) ◽  
pp. 101
Author(s):  
L. D. Woodham ◽  
R. T. Wicks ◽  
D. Verscharen ◽  
J. M. TenBarge ◽  
G. G. Howes
Keyword(s):  
Solar Wind ◽  
Solar Wind Proton ◽  
Proton Temperature
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