Coronal Heating Distribution Due to Low-Frequency, Wave-driven Turbulence

By P. Dmitruk, William H. Matthaeus, L. Milano, S. Oughton, Gary Zank, D. Mullan. 2002

165 citations recorded by the source corpus.

The heating of the lower solar corona is examined using numerical simulations and theoretical models of magnetohydrodynamic turbulence in open magnetic regions. A turbulent energy cascade to small length scales perpendicular to the mean magnetic field can be sustained by driving with low-frequency Alfvén waves reflected from mean density and magnetic field gradients. This mechanism deposits energy efficiently in the lower corona, and we show that the spatial distribution of the heating is determined by the mean density through the Alfvén speed profile. This provides a robust heating mechanism which can explain observed high coronal temperatures and accounts for the significant heating (per unit volume) distribution below 2 solar radii needed in models of the origin of the solar wind. The obtained heating per unit mass, on the other hand, is much more extended, indicating that the heating on a per-particle basis persists throughout all the lower coronal region considered here.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/1c70c32484c5e413fa952c7c082fd2ebaaa9adb9

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Citations in the corpus

Alfvén Waves and Turbulence in the Solar Atmosphere and Solar Wind (2007, background): “…which should effectively favor the development of a turbulent cascade in planes perpendicular to the direction of wave propagation (along the magnetic field), has been found (Zank et al. 1996; Matthaeus et al. 1998, 1999;Dmitruk et al. 2001a, 2002;Dmitruk&Matthaeus 2003; Oughton et al. 2001, 2004).”
INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, methodology): “First, we evaluate the toal turbulent heating rateQ using an analytical theory of lowfrequency AW turbulence driven by non-WKB wave reflection (Dmitruk et al. 2002; Chandran & Hollweg 2009).”
HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE (2011, methodology): “It is worthwhile to compare the computed heating ratesQ(z) with those predicted from phenomenological turbulence models (Hossain et al. 1995; Matthaeus et al. 1999; Dmitruk et al. 2001, 2002; Chandran et al. 2009).”
Evaluation of the turbulent energy cascade rates from the upper inertial range in the solar wind at 1 AU (2007, methodology): “[15] Analysis and simulations based on MHD equations also show that the turbulent cascades are mostly in the direction perpendicular to the background magnetic field and produce smaller perpendicular scales [e.g., Shebalin et al.,, 1983; Oughton et al., 1994; Matthaeus et al., 1996; Ghosh et al., 19”
On the Generation, Propagation, and Reflection of Alfvén Waves from the Solar Photosphere to the Distant Heliosphere (2004, background): “However, when looking only at their linear terms, one obtains ∂z± ∂t + (u∓VA) · ∇z± = ( z∓ − z± 2 ) ∇ · (u 2 ±VA ) − z∓ · ( ∇u± ∇B0√ 4πρ ) (B2) (see also Dmitruk, Milano, & Matthaeus 2001).”
Alfvénic Turbulence in the Extended Solar Corona: Kinetic Effects and Proton Heating (2003, methodology): “Dmitruk et al. (2001, 2002) also approximated the reflected inward powerZ+ as∼ Lout|∂VA/∂r|.”
MAGNETOHYDRODYNAMIC WAVES AND CORONAL HEATING: UNIFYING EMPIRICAL AND MHD TURBULENCE MODELS (2012, methodology): “or the turbulent heating in the corona, one of the most advanced models of this kind being recently described in Cranmer (2010) (see also Tu and Marsch (1997); Hu et al. (2000); Li and Habbal (2003); Dmitruk et al. (2002)) on one hand, and well established models with semi-empirical heating function”
ALFVÉN WAVE SOLAR MODEL (AWSoM): CORONAL HEATING (2013, methodology): “…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).”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, methodology): “Approximations for Z− andZ+ such as those given by Dmitruk et al. (2002) should be tested further to evaluate ways of estimating the amount of reflection without having to solve the full non-WKB equations.”
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 brifely address what our cascade model predicts for ion heating in the…”
TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS (2011, methodology): “The volumetric heating rate is given by Q = α̃ρv3 ⊥ λ⊥ (14) (Hollweg 1986; Hossain et al. 1995; Zhou & Matthaeus 1990; Matthaeus et al. 1999; Dmitruk et al. 2002).”
EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “…form for the turbulent heating rate has been found to be consistent with numerical simulations of strong MHD turbulence in a background magnetic field (e.g., Dobrowolny et al. 1980; Hossain et al. 1995; Zhou & Matthaeus 1990; Matthaeus et al. 1999a; Oughton et al. 2001; Dmitruk et al. 2001, 2002).”
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).”
Ultraviolet spectroscopy of the extended solar corona (2006, background): “…kinetic plasma instabilities (driven by non-Maxwellian velocity distributions or spatial gradients), and wave mode conversion driven by reflection or refraction (e.g., Hollweg 1986; Matthaeus et al. 1999; Kaghashvili & Esser 2000; Dmitruk et al. 2001, 2002; Cranmer & van Ballegooijen 2005).”