Global three‐dimensional MHD simulation of a space weather event: CME formation, interplanetary propagation, and interaction with the magnetosphere

By C. Groth, D. D. De Zeeuw, Tamas I. Gombosi, Kenneth G. Powell. 2000

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In Astronomy and Astrophysics

Citations in the corpus

A Three-dimensional Model of the Solar Wind Incorporating Solar Magnetogram Observations (2003, methodology): “Similar magnetic configurations were used in the majority of later studies in two dimensions (see Wang et al. 1998 and Suess et al. 1999) and three dimensions (see Usmanov 1993 and Groth et al. 2000), in order to model the solar wind conditions representing the heliosphere at solar minimum.”
A Semiempirical Magnetohydrodynamical Model of the Solar Wind (2007, background): “Traditionally, the deposition of energy and/or momentum into the solar wind has been described by means of some empirical source terms (Usmanov 1993; McKenzie et al. 1997; Mikićet al. 1999; Suess et al. 1999; Wu et al. 1999; Groth et al. 2000, e.g.).”
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).”
Numerical simulation of the 12 May 1997 interplanetary CME event (2004, methodology): “Time-dependent pulses have been utilized in attempts to simulate transient disturbances, especially shocks, plasma clouds, and magnetic flux ropes [e.g., Detman et al., 1991; Groth et al., 2000; Manchester et al., 2002; Vandas et al., 2002; Wu et al., 1996].”
Coronal Mass Ejection Shock and Sheath Structures Relevant to Particle Acceleration (2005, unknown): “The dimensionless equations are then solved, using the block-adaptive tree solar wind Roe-type upwind scheme (BATSR-US) code (Powell et al. 1999; Groth et al. 2000).”
Space Weather Modeling Framework: A new tool for the space science community (2005, methodology): “heating, and acceleration of the solar wind [Groth et al., 2000; Usmanov et al., 2000].”
THREE-DIMENSIONAL SOLAR WIND MODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID (2010, methodology): “…to the numerical study of producing solar steady-state conditions (e.g., Usmanov 1993; McKenzie et al. 1997; Mikić et al. 1999; Suess et al. 1996, 1999; Wang et al. 1998; Wu et al. 1999; Groth et al. 2000; Feng et al. 2005, 2007; Zhou et al. 2008; Kleimann et al. 2009; Nakamizo et al. 2009).”
Constraints on the global structure of magnetic clouds: Transverse size and curvature (2006, background): “…cross section of MCs is also indicated by global magnetohydrodymic (MHD) simulations of the propagation both in a uniform [e.g., Cargill et al., 2000; Odstrcil et al., 2002; Riley et al., 2003] and structured solar wind [e.g., Groth et al., 2000; Odstrcil et al., 2004; Manchester et al., 2004].”
Three‐dimensional MHD simulation of a flux rope driven CME (2004, methodology): “The dimensionless equations are then solved, using the block-adaptive tree solar windRoe-type upwind scheme (BATS-R-US) code [Powell et al., 1999; Groth et al., 2000].”
Numerical Simulation of the Interaction of Two Coronal Mass Ejections from Sun to Earth (2005, methodology): “The dimensionless equations are then solved, using the block-adaptive tree solar wind Roe-type upwind scheme (BATS-R-US) code (Powell et al. 1999; Groth et al. 2000).”