MULTISPECTRAL EMISSION OF THE SUN DURING THE FIRST WHOLE SUN MONTH: MAGNETOHYDRODYNAMIC SIMULATIONS

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The Physical Processes of CME/ICME Evolution (2017, methodology): “After calculating a global potential magnetic field based on this boundary condition, a thermodynamic MHD model of the corona is produced, using the equations and coronal-heating specification described by Lionello et al. (2009).”
ALFVÉN WAVE SOLAR MODEL (AWSoM): CORONAL HEATING (2013, background): “Lionello et al. (2009) demonstrated that a 3D magnetohydrodynamic (MHD) lower corona model based on a combination of ad hoc coronal heating functions and with heat conduction was able to well reproduce many features in the observed EUV images.”
The Open Flux Problem (2017, methodology): “These models are elements of CORHEL (Corona-Heliosphere, Riley et al. 2012).”
A MODEL FOR THE SOURCES OF THE SLOW SOLAR WIND (2010, methodology): “The MAS code and its implementation are described in detail by Mikić & Linker (1994), Mikić et al. (1999), Linker et al. (1999), and Lionello et al. (2009).”
Slow Solar Wind: Observations and Modeling (2016, unknown): “In the more sophisticated “thermodynamic” approximation, energy transport processes are included more explicitly (Lionello et al. 2009).”