A Comparison between Global Solar Magnetohydrodynamic and Potential Field Source Surface Model Results

By Pete Riley, Jon A. Linker, Z. Mikić, Roberto Lionello, S. Ledvina, Jan Luhmann. 2006

272 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/264a2c71a76b4ae3ae07d66f487de230fc12ffb3

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Citations in the corpus

Origins of the Ambient Solar Wind: Implications for Space Weather (2017, methodology): “The PFSS technique is computationally efficient to implement, and it reproduces a number of large-scale features of the corona as seen with coronagraphs and during eclipses (Riley et al. 2006).”
MULTISPECTRAL EMISSION OF THE SUN DURING THE FIRST WHOLE SUN MONTH: MAGNETOHYDRODYNAMIC SIMULATIONS (2008, background): “MHD models that include the photospheric magnetic field as a boundary condition have existed for more than a decade (Usmanov 1993, 1996; Mikić & Linker 1996; Linker et al. 1999; Mikić et al. 1999; Roussev et al. 2003; Riley et al. 2006; Cohen et al. 2007).”
The Heliospheric Magnetic Field (2013, background): “…are strongly associated with short-term enhancements in 𝐵 and ICME rates are known to vary in phase with the solar cycle (Cane and Richardson, 2003; Riley et al., 2006b), Richardson et al. (2000) concluded that the solar cycle variation in 𝐵 was not a direct result of spacecraft being…”
MAGNETOHYDRODYNAMIC WAVES AND CORONAL HEATING: UNIFYING EMPIRICAL AND MHD TURBULENCE MODELS (2012, background): “…Hu et al. (2000); Li and Habbal (2003); Dmitruk et al. (2002)) on one hand, and well established models with semi-empirical heating function, such as that presented in Lionello et al. (2001); Riley et al. (2006); Titov et al. (2008); Lionello et al. (2009); Downs et al. (2010), on the other hand.”
Slow Solar Wind: Observations and Modeling (2016, unknown): “…photospheric magnetic field as the primary driving boundary condition, single-fluid global MHD models can often reproduce the Sun’s magnetic and emission properties during both quiet (e.g., Riley et al. 2001, 2006; Riley and Luhmann 2012) and active (e.g., Riley et al. 2003, 2007, 2008) periods.”
Nonlinear Force-Free Modeling of Coronal Magnetic Fields. II. Modeling a Filament Arcade and Simulated Chromospheric and Photospheric Vector Fields (2008, background): “We suggest that a global Potential Field Source Surface (PFSS) model (e.g., Riley et al., 2006) might be a good way to set the side walls of the extrapolation to account for magnetic flux that is not included in the box when a full-sphere nonlinear force-free code is prohibitive.”
EMPIRICAL CONSTRAINTS ON PROTON AND ELECTRON HEATING IN THE FAST SOLAR WIND (2009, background): “Most advanced globalmodeling efforts currently include only a one-fluid treatment of the internal energy equation (e.g., Riley et al. 2001, 2006; Roussev et al. 2003; Tóth et al. 2005; Usmanov & Goldstein 2006; Feng et al. 2007).”
THREE-DIMENSIONAL SOLAR WIND MODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID (2010, methodology): “Following Linker et al. (1999) and Riley et al. (2006), by identifying the closed-field regions and the open-field regions through tracing magnetic field lines on the lower boundary, a map of the coronal hole boundaries obtained by the MHD model and the PFSS model is presented in Figure 12(a).”
The Open Flux Problem (2017, background): “The introduction of shear and/or twist in a model can also cause more flux to open (e.g., Riley et al. 2006; Edwards et al. 2015), but this will also increase the open field area predicted by the model.”