Alfvén Waves and Turbulence in the Solar Atmosphere and Solar Wind

By A. Verdini, M. Velli. 2007

231 citations recorded by the source corpus.

We solve the problem of propagation and dissipation of Alfvénic turbulence in a model solar atmosphere consisting of a static photosphere and chromosphere, transition region, and open corona and solar wind using a phenomenological model for the turbulent dissipation based on wave reflection. We show that most of the dissipation for a given wave-frequency spectrum occurs in the lower corona, and the overall rms amplitude of the fluctuations evolves in a way consistent with observations. The frequency spectrum for a Kolmogorov-like slope is not found to change dramatically from the photosphere to the solar wind; however, it does preserve signatures of transmission throughout the lower atmospheric layers, namely, oscillations in the spectrum at high frequencies reminiscent of the resonances found in the linear case. These may disappear once more realistic couplings for the nonlinear terms are introduced or if time-dependent variability of the lower atmospheric layer is introduced.

Subfields: Astronomy and Astrophysics, Oceanography

View Paper: https://www.semanticscholar.org/paper/5f1b867d6fa64627120ae381d0ff945185f336ca

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Citations in the corpus

Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, background): “…in the photosphere up into the upper chromosphere and corona, playing the role as the dominant energy carrier in many simulations that appear to be able to generate hot coronae (e.g., Cranmer and van Ballegooijen 2005; Suzuki and Inutsuka 2005; Verdini and Velli 2007; Matsumoto and Shibata 2010).”
HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE (2011, background): “…( Z± − Z∓ ) ∇· ( 1 2U±VA ) −Z∓ · ( ∇U± 1√ 4πρ0 ∇B0 ) − 1 ρ0 ∇P− Z∓ ·∇Z±, (A2) whereVA ≡ B0/ √ 4πρ0 is the Alfvén velocity vector,U is the outflow velocity, andP is the perturbation in the total pressure (also see Dmitruk et al. 2001; Verdini & Velli 2007; Buchlin &Velli 2007; Cranmer et al. 2007).”
The FIELDS Instrument Suite for Solar Probe Plus (2016, background): “Some turbulence-driven solar wind models (i.e. Cranmer and van Ballegooijen 2005; Cranmer et al. 2009; Verdini and Velli 2007; Verdini et al. 2010) provide predictions of the radial evolution of solar wind plasma parameters, as well as important fluctuating quanti- ties.”
ALFVÉN WAVE SOLAR MODEL (AWSoM): CORONAL HEATING (2013, background): “…outward from the Sun are partially reflected by gradients due to stratification, which produces waves propagating in opposite directions, see for instance (Heinemann & Olbert 1980; Leroy 1980; Mattheus et al. 1999; Dmitruk et al. 2002; Verdini & Velli 2007; Cranmer 2010; Chandran et al. 2011).”
The Heliospheric Magnetic Field (2013, background): “On the right, the corona is heated by waves and/or turbulence (e.g., Cranmer and van Ballegooijen, 2005; Verdini and Velli, 2007).”
INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, background): “Whilez+rms is likely ≫ z−rms in coronal holes (Cranmer & van Ballegooijen 2005; Verdini & Velli 2007; Cranmer 2010), Helios measurements in the fast solar wind show thatz+rms/z − rms decreases from≃ 4 to ≃ 2 asr increases from 80R⊙ to 1 AU (Bavassano et al. 2000).”
The Solar Probe Plus Mission: Humanity’s First Visit to Our Star (2016, background): “…nonlinear cascade of lower frequency Alfvén waves—the open field counterpart of the closed field heating model discussed above (Velli et al. 1989; Matthaeus et al. 1999; Verdini and Velli 2007; Cranmer et al. 2007; Verdini et al. 2010; Perez and Chandran 2013; Lionello et al. 2014).”
PERPENDICULAR ION HEATING BY LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE IN THE SOLAR WIND (2010, background): “…generated near the Sun by non-WKB wave reflection arising from the gradient in the Alfvén speed (Heinemann and Olbert 1980; Velli et al. 1989; Matthaeus et al. 1999; Dmitruk et al. 2002; Cranmer and van Ballegooijen 2005; Verdini and Velli 2007; Hollweg and Isenberg 2007; Verdini et al. 2009a).”
The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere (2019, background): “…speed was suggested to cause the outward-propagating waves to be partially reflected (Heinemann & Olbert 1980; Velli 1993) and initiate the cascade (Matthaeus et al. 1999a; Dmitruk et al. 2002; Cranmer & van Ballegooijen 2005; Verdini & Velli 2007; Chandran & Hollweg 2009; Verdini et al. 2009).”
TIME–DISTANCE SEISMOLOGY OF THE SOLAR CORONA WITH CoMP (2009, background): “…large non-thermal line widths in the corona and exploit the developing self-consistent theories which involve the effective dissipation of low-frequency Alfvénic motions (e.g., Cranmer & van Ballegooijen 2005; Suzuki & Inutsuka 2005; Cranmer, van Ballegooijen & Edgar 2007; Verdini & Velli 2007).”
Electron and proton heating by solar wind turbulence (2009, methodology): “S R ] 2 3 Ju l 2 00 9 JOURNAL OF GEOPHYSICAL RESEARCH, VOL. ???, XXXX, DOI:10.1029/,”
A TURBULENCE-DRIVEN MODEL FOR HEATING AND ACCELERATION OF THE FAST WIND IN CORONAL HOLES (2009, unknown): “We include spatial transport (Verdini & Velli 2007) in a non-uniform wind with speedU(r)r̂.”