Nonresonant Pitch‐Angle Scattering of Low‐Energy Electrons in the Solar Wind

2006 ◽  
Vol 642 (2) ◽  
pp. 1163-1172 ◽  
Author(s):  
B. R. Ragot
Keyword(s):  
Solar Wind ◽  
Pitch Angle ◽  
Low Energy ◽  
Angle Scattering ◽  
Low Energy Electrons

scholarly journals On the origin of low‐energy electrons in the inner magnetosphere: Fluxes and pitch‐angle distributions

2017 ◽  
Vol 122 (2) ◽  
pp. 1789-1802 ◽  
Author(s):  
M. H. Denton ◽  
G. D. Reeves ◽  
B. A. Larsen ◽  
R. H. W. Friedel ◽  
M. F. Thomsen ◽  
...  
Keyword(s):  
Pitch Angle ◽  
Low Energy ◽  
Inner Magnetosphere ◽  
Low Energy Electrons

Influence of time-variable solar wind on the response of Mercury’s magnetosphere

2021 ◽  
Author(s):  
Sae Aizawa ◽  
Nicolas André ◽  
Ronan Modolo ◽  
Elisabeth Werner ◽  
Jim Slavin ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Charged Particles ◽  
Time Variable ◽  
Low Energy ◽  
Field Of View ◽  
Plasma Measurement ◽  
Electrons And Ions ◽  
Low Energy Electrons ◽  
The Magnetic Field

<p><span lang="EN-GB">BepiColombo is going to conduct its first Mercury flyby in October 2021. During this flyby,  plasma measurement will be obtained and bring new insights on the Hermean magnetosphere and its interaction with the Sun despite the limited field of view of the instruments during the cruise phase. Unlike Mariner-10 ion measurements will be obtained, and unlike MESSENGER, low energy electrons and ions will be measured simultaneously. In this study, we have revisited Mariner 10 and MESSENGER observations with the help of the global hybrid model LatHyS in order to understand the influence of time-variable solar wind and to constraint the plasma environment. We are able to reproduce the magnetic field observations of Mariner 10 along its trajectory with in particular two distinct signatures consisting of a quiet and disturbed state of the magnetosphere. In addition, the plasma spectrogram is also collected in the model and this enables us to detail the properties of the charged particles observed during the flyby. We will discuss all these signatures both in term of an interaction with a time-variable solar wind and localized processes occurring in the magnetosphere. We will then present the virtual sampling of both the magnetic field and plasma spectrogram along BepiColombo’s first Mercury flyby trajectory and discuss the possible signatures to be observed at that time.</span></p>

Correction to: On the Power-Law Distribution of Pitch-Angle Scattering Times in Solar Wind Turbulence

Solar Physics ◽  
2019 ◽  
Vol 294 (6) ◽  
Author(s):  
Silvia Perri ◽  
Francesco Pucci ◽  
Francesco Malara ◽  
Gaetano Zimbardo
Keyword(s):  
Solar Wind ◽  
Power Law ◽  
Pitch Angle ◽  
Power Law Distribution ◽  
Solar Wind Turbulence ◽  
Angle Scattering ◽  
Wind Turbulence

scholarly journals On heating of solar wind protons by the breaking of large amplitude Alfvén waves

2018 ◽  
Author(s):  
Horia Comişel ◽  
Yasuhiro Nariyuki ◽  
Yasuhito Narita ◽  
Uwe Motschmann
Keyword(s):  
Solar Wind ◽  
Pitch Angle ◽  
Plasma Heating ◽  
Alfven Waves ◽  
Distribution Functions ◽  
Alfven Wave ◽  
Alfvén Waves ◽  
Parametric Decay ◽  
Angle Scattering ◽  
Velocity Distribution Functions

Abstract. By means of hybrid simulations, we present a study on plasma heating by the field-aligned parametric decay of a monochromatic left-handed polarized Alfven wave. Simultaneous multidimensional comparisons of the wave modes and proton kinetics suggest that parametric decay of Alfven waves and pitch angle scattering of solar wind protons are interrelated. Parametric decay mechanism yields counter-propagating Alfven waves that can shape and broaden via pitch angle scattering mechanism both the sunward and antisunward sides of the proton velocity distribution functions in agreement with in situ measurements of fast stream solar wind plasmas.

On the Power-Law Distribution of Pitch-Angle Scattering Times in Solar Wind Turbulence

Solar Physics ◽  
2019 ◽  
Vol 294 (3) ◽  
Author(s):  
Silvia Perri ◽  
Francesco Pucci ◽  
Francesco Malara ◽  
Gaetano Zimbardo
Keyword(s):  
Solar Wind ◽  
Power Law ◽  
Pitch Angle ◽  
Power Law Distribution ◽  
Solar Wind Turbulence ◽  
Angle Scattering ◽  
Wind Turbulence

scholarly journals Solar wind plasma interaction with solar probe plus spacecraft

2012 ◽  
Vol 30 (7) ◽  
pp. 1075-1092 ◽  
Author(s):  
S. Guillemant ◽  
V. Génot ◽  
J.-C. Matéo-Vélez ◽  
R. Ergun ◽  
P. Louarn
Keyword(s):  
Solar Wind ◽  
Numerical Models ◽  
Solar Wind Plasma ◽  
Sensitivity Study ◽  
Plasma Potential ◽  
Distribution Functions ◽  
Low Energy ◽  
High Yield ◽  
Solar Probe Plus ◽  
Low Energy Electrons

Abstract. 3-D PIC (Particle In Cell) simulations of spacecraft-plasma interactions in the solar wind context of the Solar Probe Plus mission are presented. The SPIS software is used to simulate a simplified probe in the near-Sun environment (at a distance of 0.044 AU or 9.5 RS from the Sun surface). We begin this study with a cross comparison of SPIS with another PIC code, aiming at providing the static potential structure surrounding a spacecraft in a high photoelectron environment. This paper presents then a sensitivity study using generic SPIS capabilities, investigating the role of some physical phenomena and numerical models. It confirms that in the near- sun environment, the Solar Probe Plus spacecraft would rather be negatively charged, despite the high yield of photoemission. This negative potential is explained through the dense sheath of photoelectrons and secondary electrons both emitted with low energies (2–3 eV). Due to this low energy of emission, these particles are not ejected at an infinite distance of the spacecraft and would rather surround it. As involved densities of photoelectrons can reach 106 cm−3 (compared to ambient ions and electrons densities of about 7 × 103 cm−3), those populations affect the surrounding plasma potential generating potential barriers for low energy electrons, leading to high recollection. This charging could interfere with the low energy (up to a few tens of eV) plasma sensors and particle detectors, by biasing the particle distribution functions measured by the instruments. Moreover, if the spacecraft charges to large negative potentials, the problem will be more severe as low energy electrons will not be seen at all. The importance of the modelling requirements in terms of precise prediction of spacecraft potential is also discussed.

Pitch angle diffusion of low-energy electrons by whistler mode waves

1993 ◽  
Vol 98 (A4) ◽  
pp. 5959-5967 ◽  
Author(s):  
A. D. Johnstone ◽  
D. M. Walton ◽  
R. Liu ◽  
D. A. Hardy
Keyword(s):  
Pitch Angle ◽  
Low Energy ◽  
Whistler Mode ◽  
Low Energy Electrons ◽  
Whistler Mode Waves

Modulation effects of a changing solar wind speed on low-energy electrons

2003 ◽  
Vol 32 (4) ◽  
pp. 675-680 ◽  
Author(s):  
S.E.S. Ferreira ◽  
M.S. Potgieter ◽  
D.M. Moeketsi
Keyword(s):  
Solar Wind ◽  
Wind Speed ◽  
Solar Wind Speed ◽  
Low Energy ◽  
Low Energy Electrons
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