An empirically‐driven global MHD model of the solar corona and inner heliosphere

By Pete Riley, Jon A. Linker, Zoran Mikic. 2001

268 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/166dfb53f7ba59c8008e272076a8fb79e33aeb49

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Citations in the corpus

Ensemble Modeling of CMEs Using the WSA–ENLIL+Cone Model (2015, methodology): “Other coronal models, such as MAS (MHD around a Sphere) (Riley, Linker, and Mikić, 2001) or heliospheric tomography from interplanetary scintillation (IPS) (Jackson et al., 2011) can also provide the background solar wind and have been coupled with ENLIL heliospheric simulations.”
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).”
Slow Solar Wind: Observations and Modeling (2016, unknown): “The simplest is the so-called polytropic approximation, where the energy equation is replaced by a simple polytropic relationship between density and pressure (i.e., S = 0), and γ is set to 1.05 to mimic the near-isothermal nature of the corona (e.g., Linker et al. 1990; Riley et al. 2001).”
A Comparison between Global Solar Magnetohydrodynamic and Potential Field Source Surface Model Results (2006, methodology): “Although models can be run on single processor machines, the codes in use today (e.g., Linker et al. 1999; Riley et al. 2001; Roussev et al. 2003) typically use theMessage Passing Interface (MPI) to run on massively parallel architectures.”
Numerical simulation of the 12 May 1997 interplanetary CME event (2004, methodology): “We use data from the SAIC repository of synoptic maps of magnetic field and velocity at 30 RS [Linker et al., 1999; Riley et al., 2001] (http://www.”
The association of coronal mass ejections with their effects near the Earth (2005, methodology): “The travel time of limb CME fronts from the Sun to the location of Helios 1 (at about 900 off the Earth-Sun line) as function of the CME radial speed Vrad obtained from the SOLWIND coronagraph. Only those cases were selected where a unique association could be achieved, in particular when Helios 1 w”
EUHFORIA: European heliospheric forecasting information asset (2018, methodology): “The empirical model employed in this work follows the path laid out by the Wang–Sheeley model (Wang & Sheeley, 1990), the DCHB model (Riley et al., 2001) as well as the Wang–Sheeley–Argemodel (Arge, 2003) in that the solar wind speed is given as a function of the flux tube expansion factor f and…”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, unknown): “…description of MHD turbulence can be applied to more advanced modeling efforts—specifically those that attemptto reproduce the full three-dimensional and time-dependent nature of the corona and heliosphere (e.g., Riley et al. 2001; Roussev et al. 2003; Tóth et al. 2005; Usmanov & Goldstein 2006).”
ILCT: Recovering Photospheric Velocities from Magnetograms by Combining the Induction Equation with Local Correlation Tracking (2004, methodology): “While some studies of the large-scale outer corona (Roussev et al. 2003; Riley et al. 2001) incorporate line-of-sightmagnetograms into the bottom boundary of time-dependent MHD solar wind solutions, no method of incorporating time-varying vector magnetogram data intoMHDmodels of the corona has been…”