Generation of the fast solar wind: A review with emphasis on the resonant cyclotron interaction

By J. V. Hollweg, P. Isenberg. 2002

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In Astronomy and Astrophysics

Citations in the corpus

EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “In a collisionless plasm , parallel-propagating Alfvén waves dissipate primarily bycyclotron resonance with positive ions (see Hollweg & Isenberg 2002).”
INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, background): “Farther from the Sun, the solar wind may be heated by high-frequency waves that are generated by either a turbulent cascade (Leamon et al. 1998; Hollweg & Isenberg 2002; Hamilton et al. 2008; Isenberg & Vasquez 2011) or by instabilities driven by the differential flow between the core of the proton…”
PERPENDICULAR ION HEATING BY LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE IN THE SOLAR WIND (2010, methodology): “…of high-frequency fast waves and Alfvén/ion-cyclotron waves could in principle explain the UVCS observations of ion heating (Li and Habbal 2001; Hollweg and Isenberg 2002; Markovskii et al. 2010), there is no direct observational evidence that waves with high frequencies and/or|k‖| & k⊥ are…”
Test Particle Energization by Current Sheets and Nonuniform Fields in Magnetohydrodynamic Turbulence (2004, methodology): “Kinetic dissipation mechanisms for coronal heating based on well-studied wave-particle energization models, such as ion cyclotron resonance (see Hollweg & Isenberg 2002 and references therein), or kinetic Alfvén waves models (Cranmer & van Ballegooijen 2003; Gary & Nishimura 2004) should also be…”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, background): “These ideas are highly complementary to theoretical models of wave dissipation via ion cyclotron resonance (e.g., Hollweg & Isenberg 2002; Cranmer 2000, 2001, 2002) that have been invoked to explain the observed preferential heating of heavy ions in the extended corona (Kohl et al. 1997, 1998,…”
On the Generation, Propagation, and Reflection of Alfvén Waves from the Solar Photosphere to the Distant Heliosphere (2004, background): “…into the solar wind, the classical transport theory of collisional damping begins to break down and collisionless wave-particle interactions should dominate the damping (e.g., Hollweg & Isenberg 2002; Marsch, Axford, & McKenzie 2003; Cranmer 2000, 2001, 2002, 2004; and many references therein).”
Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus (2015, background): “aHollweg (2008), Cranmer (2000), Hollweg and Isenberg (2002), Isenberg (2001a), Galinsky and Shevchenko (2000), Marsch and Tu (2001), Kasper et al.”
Slow Solar Wind: Observations and Modeling (2016, unknown): “Alternatively, for describing the heating terms one may invoke mechanisms based either on ion-cyclotron-resonance (see the review by Hollweg and Isenberg 2002) or on a perpendicular turbulent cascade (Chandran et al. 2011, and references therein).”