Kinetic Physics of the Solar Corona and Solar Wind

By Eckart Marsch. 2006

674 citations recorded by the source corpus.

Kinetic plasma physics of the solar corona and solar wind are reviewed with emphasis on the theoretical understanding of the in situ measurements of solar wind particles and waves, as well as on the remote-sensing observations of the solar corona made by means of ultraviolet spectroscopy and imaging. In order to explain coronal and interplanetary heating, the micro-physics of the dissipation of various forms of mechanical, electric and magnetic energy at small scales (e.g., contained in plasma waves, turbulences or non-uniform flows) must be addressed. We therefore scrutinise the basic assumptions underlying the classical transport theory and the related collisional heating rates, and also describe alternatives associated with wave-particle interactions. We elucidate the kinetic aspects of heating the solar corona and interplanetary plasma through Landau- and cyclotron-resonant damping of plasma waves, and analyse in detail wave absorption and micro instabilities. Important aspects (virtues and limitations) of fluid models, either single- and multi-species or magnetohydrodynamic and multi-moment models, for coronal heating and solar wind acceleration are critically discussed. Also, kinetic model results which were recently obtained by numerically solving the Vlasov-Boltzmann equation in a coronal funnel and hole are presented. Promising areas and perspectives for future research are outlined finally.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/669759e091ba11a3be971cc50027f96c972e3bf8

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Citations in the corpus

The Heliospheric Magnetic Field (2013, background): “The solar wind exhibits a large array of different wave modes, many of which directly perturb the heliospheric magnetic field (see Tu and Marsch, 1995 and Marsch, 2006).”
Solar Orbiter (2012, background): “onance of ions or the turbulent cascade of energy to those frequencies should play an important role (Figure 9). For an extensive review of the kinetic physics of the solar corona and solar wind, see Marsch (2006). Theoretical attempts to develop self-consistent models of fast solar wind acceleratio”
Electron temperature anisotropy constraints in the solar wind (2008, background): “What is the origin of such distributions and more generally what are the physical processes that transport the energy in the solar wind? These questions are still a matter of considerable discussion [Marsch, 2006].”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, methodology): “llite observations. But using the solar wind as a turbulence laboratory is complicated by the fact that the solar wind is only weakly collisional, so a kinetic description is necessary [Marsch, 1991; Marsch, 2006]. A useful ﬁrst step in connecting theoretical ideas to observational data over the ran”
DEPENDENCE OF SOLAR-WIND POWER SPECTRA ON THE DIRECTION OF THE LOCAL MEAN MAGNETIC FIELD (2009, background): “Remarkably, a similar enhancement of proton density fluctuations in the solar wind near k‖ρi ∼ 1 has been reported by Neugebauer (1975, 1976). Hollweg (1999) has suggested these enhanced density fluctuations could be caused by the compressibility of KAWs in the case k⊥ ≫ k‖. However, if the enhancem”
INVARIANT KAPPA DISTRIBUTION IN SPACE PLASMAS OUT OF EQUILIBRIUM (2011, background): “…etc.) in the inner heliosphere, such as the solar wind (e.g., Chotoo et al. 2000; Mann et al. 2002; Zouganelis et al. 2004; Leubner & Vörös 2005; Marsch 2006; Yoon et al. 2006; Pierrard & Lazar 2010) and the planetary magnetospheres (e.g., Christon 1987; Mauk et al. 2004; Schippers et al.…”
Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “temperatures measured perpendicular and parallel to the background magnetic field (Marsch 2006).”
Space Weather: The Solar Perspective (2006, methodology): “I further recommend the recent reviews in Living Reviews in Solar Physics “Kinetic Physics of the Solar Corona and Solar Wind” by Marsch (2006) and “The Solar Wind as a Turbulence Laboratory” by Bruno and Carbone (2005) and the article by Marsch et al. (2003).”
The Solar Probe ANalyzer—Ions on the Parker Solar Probe (2021, background): “…et al. 1996; Steinberg et al. 1996; Kasper et al. 2006; Podesta & Gary 2011) are known to drive the VDFs unstable, subsequently leading to wave generation (Daughton & Gary 1998; Hu & Habbal 1999; Gary et al. 2000; Marsch 2006; Maneva et al. 2013; Verscharen & Chandran 2013; Verscharen et al. 2013).”
First In Situ Measurements of Electron Density and Temperature from Quasi-thermal Noise Spectroscopy with Parker Solar Probe/FIELDS (2019, background): “This assumes that if instabilities (Marsch 2006) and scattering by turbulent fluctuations at electronic scales change the velocity directions, they also negligibly change the kinetic energy per particle of this component of the distribution.”
A MODEL FOR THE SOURCES OF THE SLOW SOLAR WIND (2010, background): “The proton and ion temperatures measured in situ and in coronal holes by UVCS, for example, (e.g., Kohl et al. 2006) show the opposite trend in that the ion temperatures are substantially higher in the fast wind than in the slow (Marsch 2006).”
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).”
The magnetic field in the solar atmosphere (2014, methodology): “Here, we refer the interested reader to specialized reviews on the solar wind (Marsch, 2006; Ofman, 2010; Bruno and Carbone, 2013), space weather (Schwenn, 2006), and the heliospheric magnetic field (Owens and Forsyth,”
Radial evolution of nonthermal electron populations in the low‐latitude solar wind: Helios, Cluster, and Ulysses Observations (2009, neutral): “[30] Typically, three major regimes of solar wind flows are observed by the space missions [Marsch, 2006].”
The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, methodology): “…solely on the fractionation, referring the reader to the reviews of Reale (2014) for the properties of plasma in closed coronal loops, and to Marsch (2006), Cranmer (2009) and Ofman (2010) for the physics of the acceleration of the fractionated gas into the fast and slow speed solar wind.”