A Three-dimensional Model of the Solar Wind Incorporating Solar Magnetogram Observations

By Ilia I. Roussev, Tamas I. Gombosi, Igor M. Sokolov, M. Velli, W. Manchester IV, D. Dezeeuw, P. Liewer, G. T'oth, Jan Luhmann. 2003

181 citations recorded by the source corpus.

Subfields: Artificial Intelligence, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fe1f5a32488b09b165c247fa9c9e08ec76df459c

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Citations in the corpus

Coronal Mass Ejection Shock and Sheath Structures Relevant to Particle Acceleration (2005, unknown): “While the magnetic field structure of this steady state solution is simple, more recent models incorporate synoptic magnetogram observations for more realistic magnetic field configurations (Roussev et al. 2003).”
THREE-DIMENSIONAL SOLAR WIND MODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID (2010, methodology): “Furthermore, Roussev et al. (2003) and Cohen et al. (2007) used the WSA model as an input to present an improved 3D MHD study for the solar wind, where the processes of turbulent heating in the solar wind are characterized by a varied polytropic index.”
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…”
STEREO IMPACT Investigation Goals, Measurements, and Data Products Overview (2008, unknown): “…the University of Colorado/SEC solar wind model (Riley et al. 2003; Odstrcil et al. 2002), and the University of Michigan 3D MHD adaptive grid solar wind and ICME transport model (Manchester et al. 2005; Roussev et al. 2003), will be brought to bear on the interpretation of IMPACT observations.”
Global MHD Modeling of the Solar Corona and Inner Heliosphere for the Whole Heliosphere Interval (2008, methodology): “Although we simplify these equations for the heliospheric solutions by employing a “polytropic” energy equation, where S = 0, (e.g., Linker et al., 1999; Mikić et al., 1999; Riley, Linker, and Mikić, 2001; Roussev et al., 2003), to more accurately compute densities and temperatures in the corona (an”
NUMERICAL SIMULATION OF AN EUV CORONAL WAVE BASED ON THE 2009 FEBRUARY 13 CME EVENT OBSERVED BY STEREO (2009, methodology): “Simulation results were obtained using the Space Weather Modeling Framework, developed by the Center for Space Environment Modeling, at the University of Michigan with funding support from NASA ESS, NASA ESTO-CT, NSF KDI, and DoD MURI.”
Three-dimensional MHD Simulation of the 2003 October 28 Coronal Mass Ejection: Comparison with LASCO Coronagraph Observations (2008, methodology): “This eruption generator follows from the work of Roussev et al. (2003a) who incorporated the Titov & Démoulin (1999) flux rope in the BATS-R-US code.”
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).”
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).”
A Semiempirical Magnetohydrodynamical Model of the Solar Wind (2007, unknown): “The application of varied polytropic index had been described in Roussev et al. (2003).”
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).”
Advances in Observing Various Coronal EUV Waves in the SDO Era and Their Seismological Applications (Invited Review) (2014, unknown): “Using the coronal module of the Block-Adaptive Tree Solar-wind Roe Upwind Scheme (BATSRUS) code (Roussev et al., 2003), Cohen et al. (2009) confirmed the wave/non-wave bimodality, and Schmidt and Ofman (2010) reproduced the observed EIT wave reflection from a coronal hole.”
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.”
Space Weather Modeling Framework: A new tool for the space science community (2005, unknown): “Finally, we close the paper with conclusions and our plans for future applications and development.”
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).”