Ion Cyclotron Wave Dissipation in the Solar Corona: The Summed Effect of More than 2000 Ion Species

By S. Cranmer. 2000

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In Astronomy and Astrophysics

Citations in the corpus

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).”
Alfvénic Turbulence in the Extended Solar Corona: Kinetic Effects and Proton Heating (2003, background): “…of ion cyclotron waves as a potentially important mechanism in the acceleration region of the high-speed wind (e.g., McKenzie et al. 1995; Tu & Marsch 1997, 2001; Hollweg 1999b; Li et al. 1999; Galinsky & Shevchenko 2000; Cranmer 2000, 2001, 2002; Hollweg & Isenberg 2002; Vocks & Marsch 2002).”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, methodology): “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,…”
Making the Corona and the Fast Solar Wind: A Self-consistent Simulation for the Low-Frequency Alfvén Waves from the Photosphere to 0.3 AU (2005, background): “Although the latter process might be responsible for generation of the highfrequency (up to 104Hz) ioncyclotron wave highlighted for the heating of the heavy ions (Kohl et al. 1998), it is difficult to heat the protons (Cranmer 2000).”
Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus (2015, unknown): “…Dominate as a Function of Distance from the Sun Numerous models to describe the heating and acceleration mechanisms of the aHollweg (2008), Cranmer (2000), Hollweg and Isenberg (2002), Isenberg (2001a), Galinsky and Shevchenko (2000), Marsch and Tu (2001), Kasper et al. (2008, 2013)…”
Ultraviolet spectroscopy of the extended solar corona (2006, background): “…(e.g., McKenzie et al. 1995; Tu & Marsch 1997, 2001; Hollweg 1999a, 1999b, 2000b, 2005; Axford et al. 1999; Cranmer et al. 1999a; Li et al. 1999; Cranmer 2000, 2001, 2002a, 2002b; Hollweg & Isenberg 2002; Vocks & Marsch 2002; Gary et al. 2003; Marsch et al. 2003; Cranmer & van Ballegooijen…”
Kinetic Physics of the Solar Corona and Solar Wind (2006, methodology): “(2001), Cranmer (2001), Vocks and Marsch (2001), Vocks and Marsch (2002) and Vocks and Mann (2003) applied QLT also to the solar corona and solar wind (see the subsequent Section 7).”
Solar winds driven by nonlinear low‐frequency Alfvén waves from the photosphere: Parametric study for fast/slow winds and disappearance of solar winds (2005, background): “This is first because the low-frequency wave is expected to have more power, and second because the resonance frequency of the proton is higher than those of heavier ions so that the energy of the ioncyclotron wave is in advance absorbed by the heavy ions [Cranmer , 2000].”
Coronal Heating Distribution Due to Low-Frequency, Wave-driven Turbulence (2002, methodology): “This idea, recently employed by Li et al. 1999 and reviewed by Cranmer 2000 involve phenomenological turbulent rates (being called of the Kolmogorov and Kraichnan type) but two important problems are faced.”