A global MHD solar wind model with WKB Alfvén waves: Comparison with Ulysses data

By A. Usmanov, M. Goldstein, B. Besser, J. Fritzer. 2000

140 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/2c6d226e2b6fd12f665f0799a13dabe2c7e0a017

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Citations in the corpus

A Semiempirical Magnetohydrodynamical Model of the Solar Wind (2007, background): “In more realistic models, the solar wind is heated and accelerated by the energy and momentum interchange between the solar plasma and large-scale Alfve´n turbulence (Jacques 1977; Dewar 1970; Barnes 1992; Usmanov et al. 2000; Usmanov & Goldstein 2003).”
Three-dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations (2008, background): “The physics of this domain is described by the equations of MHD with additional source terms required to take into account the heating and acceleration of the solar wind (Groth et al. 2000; Usmanov et al. 2000).”
ALFVÉN WAVE SOLAR MODEL (AWSoM): CORONAL HEATING (2013, methodology): “The earliest solar wind models that incorporated Alfvén wave turbulence were presented in Belcher & Davis (1971) and Alazraki & Couturier (1971), followed by 2D global corona models by Usmanov et al. (2000) and Hu et al. (2003).”
Ultraviolet spectroscopy of the extended solar corona (2006, background): “…analytic studies (Suess & Nerney 2002; Nerney & Suess 2005) to time-dependent multidimensional simulations (e.g., Suess et al. 1999; Wiegelmann et al. 2000; Usmanov et al. 2000; Wu et al. 2000; Ofman 2000, 2004; Lionello et al. 2001, 2005; Roussev et al. 2003; Hu et al. 2003; Li et al. 2004).”
Three‐dimensional MHD simulation of a flux rope driven CME (2004, background): “It is also thought that momentum deposited by Alfven waves may accelerate this component of the wind [cf. Hollweg et al., 1982; Usmanov et al., 2000].”
MAGNETOHYDRODYNAMIC WAVES AND CORONAL HEATING: UNIFYING EMPIRICAL AND MHD TURBULENCE MODELS (2012, background): “We now arrive at an important conclusion, that is, the most common heating functions may be parameterized in terms of an effective absorption coefficients for the Alfvén wave turbulence! The desired absorption coefficient, VA/L, may be directly included to the WKB equation for total wave intensities”
THREE-DIMENSIONAL SOLAR WIND MODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID (2010, methodology): “For instance, Usmanov et al. (2000) and Usmanov & Goldstein (2003) used a shortwavelength Wentzel–Kramers–Brillouin approximation of the Alfvén wave turbulence to mimic the energy deposit for solar wind heating and acceleration.”
Coronal Holes and the High-Speed Solar Wind (2002, background): “…and Kopp 1971; Steinolfson et al. 1982; Low 1990; Wang et al. 1993; Cuperman et al. 1995; Stewart and Bravo 1997; Ofman and Davila 1998; Guo and Wu 1998; Suess et al. 1999; Sittler and Guhathakurta 1999, 2002; Linker et al. 1999; Keppens and Goedbloed 1999; Groth et al. 1999; Usmanov et al. 2000).”
Space Weather Modeling Framework: A new tool for the space science community (2005, unknown): “The physics of this domain is well approximated with the equations of magnetohydrodynamics; however, additional source terms are required to take into account gravity, the heating, and acceleration of the solar wind [Groth et al., 2000; Usmanov et al., 2000].”
A Three-dimensional Model of the Solar Wind Incorporating Solar Magnetogram Observations (2003, background): “The effect of an Alfvén wave flux on the flow properties of the solar wind, in a WKB approximation, was recently studied in two dimensions by Usmanov et al. (2000).”