The effects of lunar surface plasma absorption and solar wind temperature anisotropies on the solar wind proton velocity space distributions in the low-altitude lunar plasma wake

2012 ◽  
Vol 117 (A10) ◽  
pp. n/a-n/a ◽  
Author(s):  
S. Fatemi ◽  
M. Holmström ◽  
Y. Futaana
Keyword(s):  
Solar Wind ◽  
Lunar Surface ◽  
Velocity Space ◽  
Surface Plasma ◽  
Solar Wind Proton ◽  
Low Altitude ◽  
Plasma Absorption

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

Solar wind proton reflection at the lunar surface: Low energy ion measurement by MAP-PACE onboard SELENE (KAGUYA)

2008 ◽  
Vol 35 (24) ◽  
Author(s):  
Y. Saito ◽  
S. Yokota ◽  
T. Tanaka ◽  
K. Asamura ◽  
M. N. Nishino ◽  
...  
Keyword(s):  
Solar Wind ◽  
Lunar Surface ◽  
Low Energy ◽  
Solar Wind Proton

scholarly journals Cusp-like plasma in high altitudes: a statistical study of the width and location of the cusp from Magion-4

2002 ◽  
Vol 20 (3) ◽  
pp. 311-320 ◽  
Author(s):  
J. Mĕrka ◽  
J. Šafránková ◽  
Z. Nĕmeček
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
High Altitudes ◽  
Data Set ◽  
Latitudinal Dependence ◽  
Merging Process ◽  
Low Altitude ◽  
Field Lines ◽  
The Magnetic Field ◽  
Dipole Tilt

Abstract. The width of the cusp region is an indicator of the strength of the merging process and the degree of opening of the magnetosphere. During three years, the Magion-4 satellite, as part of the Interball project, has collected a unique data set of cusp-like plasma observations in middle and high altitudes. For a comparison of high- and low-altitude cusp determination, we map our observations of cusp-like plasma along the magnetic field lines down to the Earth’s surface. We use the Tsyganenko and Stern 1996 model of the magnetospheric magnetic field for the mapping, taking actual solar wind and IMF parameters from the Wind observations. The footprint positions show substantial latitudinal dependence on the dipole tilt angle. We fit this dependence with a linear function and subtract this function from observed cusp position. This process allows us to study both statistical width and location of the inspected region as a function of the solar wind and IMF parameters. Our processing of the Magion-4 measurements shows that high-altitude regions occupied by the cusp-like plasma (cusp and cleft) are projected onto a much broader area (in magnetic local time as well as in a latitude) than that determined in low altitudes. The trends of the shift of the cusp position with changes in the IMF direction established by low-altitude observations have been confirmed.Key words. Magnetospheric physics (magnetopause, cusp and boundary layer; solar wind – magnetosphere interactions)

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

Permanent Lunar Surface Magnetism and Its Deflection of the Solar Wind

Science ◽  
1971 ◽  
Vol 172 (3984) ◽  
pp. 716-718 ◽  
Author(s):  
A. Barnes ◽  
P. Cassen ◽  
J. D. Mihalov ◽  
A. Eviatar
Keyword(s):  
Solar Wind ◽  
Lunar Surface ◽  
Surface Magnetism

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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