Radial evolution of the electron distribution functions in the fast solar wind between 0.3 and 1.5 AU

By M. Maksimović, I. Zouganelis, J. Chaufray, K. Issautier, E. Scime, J. Littleton, Eckart Marsch, David John McComas, C. Salem, R. Lin and 1 more. 2005

259 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/d33a4f3b137f67dc29279665e206bcfd3f3a1132

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Citations in the corpus

A review of solar type III radio bursts (2014, background): “Observations of the background solar wind electrons have shown that a kappa distribution can better model the solar wind (Maksimovic et al., 2005; Le Chat et al., 2010).”
First In Situ Measurements of Electron Density and Temperature from Quasi-thermal Noise Spectroscopy with Parker Solar Probe/FIELDS (2019, background): “The latter value and the radial profile are similar to those found by Helios (Pilipp et al. 1990; Maksimovic et al. 2005), despite the general decrease in solar activity until the Helios epoch and the expected overall decrease in coronal temperature (Schwadron et al. 2014).”
The Heliospheric Magnetic Field (2013, background): “This signature may only be present for newly added heliospheric loops, as the apex of a loop will continue to move anti-sunward meaning the loop length will increase such that the CSE signature is lost by pitchangle scattering (Hammond et al., 1996; Maksimovic et al., 2005; Owens et al., 2008b).”
Electron temperature anisotropy constraints in the solar wind (2008, unknown): “Maksimovic, E. Marsch, A. N. Fazakerley, and E. E. Scime (2008), Electron temperature”
Introduction to special section on Origins and Properties of Kappa Distributions: Statistical Background and Properties of Kappa Distributions in Space Plasmas (2015, background): “…to describe numerous space plasma populations in (i) the inner heliosphere, including solar wind [e.g., Collier et al., 1996; Mann et al., 2002; Maksimovic et al., 2005; Marsch, 2006; Zouganelis, 2008; Štverák et al., 2009; Livadiotis and McComas, 2010a, 2011a, 2013d; Yoon, 2014], solar corona…”
Radial evolution of nonthermal electron populations in the low‐latitude solar wind: Helios, Cluster, and Ulysses Observations (2009, unknown): “This subject was already examined and published by many other authors, we refer the reader, for example, to Marsch et al. [1989], Issautier et al.”
ASTROPHYSICAL GYROKINETICS: KINETIC AND FLUID TURBULENT CASCADES IN MAGNETIZED WEAKLY COLLISIONAL PLASMAS (2007, background): “Besides the anisotropies, the particle distribution functions in the solar wind (especially the electron one) exhibit nonMaxwellian suprathermal tails (see Maksimovic et al. 2005; Marsch 2006, and references therein).”
Kinetic Physics of the Solar Corona and Solar Wind (2006, background): “The lower frame of Figure 1 after Maksimovic et al. (2005) indicates that the strahl is declining with radial distance from the Sun, whereas the halo is relatively increasing, perhaps by scattering of strahl electrons.”
The Solar Probe Plus Mission: Humanity’s First Visit to Our Star (2016, background): “The eVDFs permanently exhibit three different components: a thermal core and a supra-thermal halo, which are present at all pitch angles, and a sharply magnetic field aligned “strahl” which is usually propagating antisunward (Rosenbauer et al. 1977; Maksimovic et al. 2005).”