A TURBULENCE-DRIVEN MODEL FOR HEATING AND ACCELERATION OF THE FAST WIND IN CORONAL HOLES

By A. Verdini, M. Velli, William H. Matthaeus, S. Oughton, P. Dmitruk. 2009

155 citations recorded by the source corpus.

A model is presented for generation of fast solar wind in coronal holes, relying on heating that is dominated by turbulent dissipation of MHD fluctuations transported upward in the solar atmosphere. Scale-separated transport equations include large-scale fields, transverse Alfvénic fluctuations, and a small compressive dissipation due to parallel shears near the transition region. The model accounts for proton temperature, density, wind speed, and fluctuation amplitude as observed in remote sensing and in situ satellite data.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/349843d2ac7db3e2d9e7c72cccaa720e064a7178

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In Astronomy and Astrophysics

Citations in the corpus

PERPENDICULAR ION HEATING BY LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE IN THE SOLAR WIND (2010, result): “…observational constraints on the Alfvén-wave amplitudes; in all of these models, the turbulent heating rate appears to be consistent with the requirements for generating the fast wind (Cranmer and van Ballegooijen 2005; Cranmer et al. 2007; Chandran and Hollweg 2009; Verdini et al. 2009b, 2010).”
INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, background): “Two other groups of authors have developed solar-wind models based on energy and momentum deposition by lowfrequency AW turbulence driven by non-WKB wave reflection (Cranmer et al. 2007; Verdini et al. 2010).”
The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere (2019, background): “…properties such as heat fluxes, pressure anisotropy, and turbulent dissipation, to achieve a self-consistent solar wind solutions that can match many properties of observational data (Cranmer et al. 2007; Verdini et al. 2010; Chandran et al. 2011; van der Holst et al. 2014; Usmanov et al. 2018).”
HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE (2011, background): “…have shown that there is significant reflection of waves in the corona, and that Alfvén wave turbulence can explain the heating and acceleration of the solar wind (e.g., Dmitruk et al. 2002; Cranmer & van Ballegooijen 2005; Cranmer et al. 2007; Chandran & Hollweg 2009; Verdini et al. 2010).”
MAGNETOHYDRODYNAMIC WAVES AND CORONAL HEATING: UNIFYING EMPIRICAL AND MHD TURBULENCE MODELS (2012, background): “The same criticism seems to be applicable to the more refined and physics-based Alfvén-wave-driven models of the solar wind Suzuki and Inutsuka (2005); Verdini et al. (2010); Osman et al. (2011).”
Theory and Transport of Nearly Incompressible Magnetohydrodynamic Turbulence (2017, unknown): “The heating term St can be written as (Verdini et al. 2010; Adhikari et al. 2022c) a l l = á ñá ñ + á ñá ñ+ - + - + -”
TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS (2011, background): “…coronal heating and solar wind acceleration have begun to succeed in reproducing a wide range of observations without the need for ad hoc free parameters (e.g., Suzuki 2006; Cranmer et al. 2007; Rappazzo et al. 2008; Verdini et al. 2010; Bingert & Peter 2011; van Ballegooijen et al. 2011).”
The Solar Probe Plus Mission: Humanity’s First Visit to Our Star (2016, background): “Such incompressible turbulence models of coronal heating appear to be successful in creating realistic high-speed solar wind streams (Cranmer 2010; Verdini et al. 2010, Figs.”