Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence

By S. Cranmer, A. van Ballegooijen, R. Edgar. 2007

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We present a series of models for the plasma properties along open magnetic flux tubes rooted in solar coronal holes, streamers, and active regions. These models represent the first self-consistent solutions that combine (1) chromospheric heating driven by an empirically guided acoustic wave spectrum; (2) coronal heating from Alfvén waves that have been partially reflected, then damped by anisotropic turbulent cascade; and (3) solar wind acceleration from gradients of gas pressure, acoustic wave pressure, and Alfvén wave pressure. The only input parameters are the photospheric lower boundary conditions for the waves and the radial dependence of the background magnetic field along the flux tube. We have not included multifluid or collisionless effects (e.g., preferential ion heating), which are not yet fully understood. For a single choice for the photospheric wave properties, our models produce a realistic range of slow and fast solar wind conditions by varying only the coronal magnetic field. Specifically, a two-dimensional model of coronal holes and streamers at solar minimum reproduces the latitudinal bifurcation of slow and fast streams seen by Ulysses. The radial gradient of the Alfvén speed affects where the waves are reflected and damped, and thus whether energy is deposited below or above the Parker critical point. As predicted by earlier studies, a larger coronal "expansion factor" gives rise to a slower and denser wind, higher temperature at the coronal base, less intense Alfvén waves at 1 AU, and correlative trends for commonly measured ratios of ion charge states and FIP-sensitive abundances that are in general agreement with observations. These models offer supporting evidence for the idea that coronal heating and solar wind acceleration (in open magnetic flux tubes) can occur as a result of wave dissipation and turbulent cascade.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/d3b94c4b1605fc4dc982764563f184e2385320a8

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Citations in the corpus

EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “(5) Also, the electron Coulomb logarithm is approximated by lnΛee = 23.2+ 3 2 ln ( Te 106K ) − 1 2 ln ( ne 106cm−3 ) (6) wherene is the electron number density (see also Cranmer et al. 2007).”
Who Needs Turbulence? (2011, background): “In this view, the density fluctuations observed by scintillation would be forced, as a secondary effect, by the reflection generated turbulent cascade (Matthaeus et al. 1999; Verdini and Velli 2007; Cranmer et al. 2007).”
Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “…that propagate up into the extended corona (Coleman 1968; Hollweg 1986; Velli et al. 1991; Matthaeus et al. 1999; Suzuki and Inutsuka 2006; Cranmer et al. 2007; Ofman 2010; van Ballegooijen et al. 2011; Chandran et al. 2011; Matsumoto and Suzuki 2012; Perez and Chandran 2013; Lionello…”
Electron and proton heating by solar wind turbulence (2009, background): “These theories (with some exceptions [e.g., Cranmer et al., 2007]) have focused only on proton temperature, ignoring heat conduction and, in effect, assuming that dissipation of turbulence occurs only through proton kinetic channels.”
The FIELDS Instrument Suite for Solar Probe Plus (2016, methodology): “5 Rs), the model by Cranmer et al. (2007) for the equatorial density (blue curve) and the model by Leblanc et al.”
HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE (2011, background): “…(Hollweg 1986; Zhou & Matthaeus 1990; Matthaeus et al. 1999; Dmitruk et al. 2001; Dmitruk & Matthaeus 2003; Cranmer & van Ballegooijen 2003, 2005; Cranmer et al. 2007; Verdini & Velli 2007) and closed magnetic fields (Heyvaerts & Priest 1984, 1992; Longcope & Strauss 1994; Dmitruk & Gomez 1997;…”
A TURBULENCE-DRIVEN MODEL FOR HEATING AND ACCELERATION OF THE FAST WIND IN CORONAL HOLES (2009, methodology): “In these ways, the present model differs from other recent models that incorporate turbulent heating (Suzuki & Inutsuka 2005; Cranmer et al. 2007).”
Slow Solar Wind: Observations and Modeling (2016, unknown): “1990), the most stable of which is that one furthest from the Sun (Cranmer et al. 2007).”
Integrated Science Investigation of the Sun (ISIS): Design of the Energetic Particle Investigation (2016, background): “…particular ISIS, FIELDS and SWEAP enable studies to distinguish among heating mechanisms, such as reconnection, ion-cyclotron waves, and turbulent dissipation and associated stochastic heating (Cranmer and van Ballegooijen 2010; Isenberg and Vasquez 2013; Cranmer et al. 2007; Chandran et al. 2013).”
Solar Wind Electrons Alphas and Protons (SWEAP) Investigation: Design of the Solar Wind and Coronal Plasma Instrument Suite for Solar Probe Plus (2015, unknown): “…Isenberg (2001a), Galinsky and Shevchenko (2000), Marsch and Tu (2001), Kasper et al. (2008, 2013) bMatthaeus et al. (1999), Dmitruk et al. (2002), Cranmer et al. (2007), Chandran et al. (2009) cBruner (1978), Ulmschneider (1985) dParker (1979, 1987), Sturrock (1999), Priest et al. (2002), Axford…”
PROPAGATING WAVES ALONG SPICULES (2011, background): “Many theoretical models have been developed for coronal heating based on waves that are excited in the photosphere or chromosphere (e.g., Hollweg et al. 1982; Tu & Marsch 1997; Axford et al. 1999; Suzuki & Inutsuka 2005; Cranmer et al. 2007; Antolin & Shibata 2010).”
A Model of Turbulence in Magnetized Plasmas: Implications for the Dissipation Range in the Solar Wind (2007, background): “In the spirit of a long line of previous investigations [Hollweg, 1986; Isenberg, 1990; Li et al., 1999; Matthaeus et al., 1999; Dmitruk et al., 2001, 2002; Cranmer and van Ballegooijen, 2003, 2005; Cranmer et al., 2007 ], we briefly address what our cascade model predicts for ion heating in the so”
INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, methodology): “It is possible that L⊥⊙ is significantly larger than this value, but in this caseδB would have to be significantly smaller than in the model of Cranmer et al. (2007) in order to be consistent with the Faraday rotation measurements, preventing AW turbulence from providing the heating needed to power…”