Abstract
An asynchronous and parallel time-marching method for three-dimensional (3D) time-dependent magnetohydrodynamic (MHD) simulation is used for large-scale solar wind simulation. It uses different local time steps in the corona and the heliosphere according to the local Courant-Friedrichs-Levy (CFL) conditions. The solar wind background with observed solar photospheric magnetic field as input is first presented. The simulation time for the background solar wind by using the asynchronous method is <1/6 of that by using the normal synchronous time-marching method with the same computation precision. Then, we choose the coronal mass ejection (CME) event of 13 November, 2003 as a test case. The time-dependent variations of the pressure and the velocity configured from a CME model at the inner boundary are applied to generate transient structures in order to study the dynamical interaction of a CME with the background solar wind flow between 1 and 230 Rs. This time-marching method is very effective in terms of computation time for large-scale 3D time-dependent numerical MHD problem. In this validation study, we find that this 3D MHD model, with the asynchronous and parallel time-marching method, provides a relatively satisfactory comparison with the ACE spacecraft observations at L1 point.
Similar content being viewed by others
References
Gosling J T. Coronal mass ejections and magnetic flux ropes in interplanetary space. In: Priest E R, Lee L C, Russell C T, eds. Physics of Magnetic Flux Ropes. Geophys Monogr. Washington D. C.: AGU, 1990, 58: 343–364
Wu S T, Guo W P, Dryer M, et al. Dynamical evolution of a coronal streamer-flux rope system: II. A self-consistent non-planar magnetohydrodynamic solution. Sol Phys, 1997, 170(2): 265–282
Wu S T, Guo W P, Michels D J, et al. MHD description of the dynamical relationships between a flux rope, streamer, coronal mass ejection, and magnetic cloud: An analysis of the January 1997 Sun- Earth connection event. J Geophys Res, 1999, 104(A7): 14789–14802
Odstrcil D, Linker J A, Lionello R, et al. Merging of coronal and heliospheric numerical 2-D MHD models. J Geophys Res, 2002, 107(A12): SSH 14-1, 1493
Usmanov A V, Goldstein M L, Besser B P, et al. A global MHD solar wind model with WKB Alfven waves: Comparison with Ulysses data. J Geophys Res, 2000, 105(A6): 12675–12696
Feng X. A comparative study on 3-D solar wind structure observed by Ulysses and MHD simulation. Chin Sci Bull, 2005, 50(7): 672–678
Shen F, Feng X, Wu S T, et al. Three-dimensional MHD simulation of CMEs in three-dimensional background solar wind with the self-consistent structure on the source surface as input: Numerical simulation of the January 1997 Sun-Earth connection event. J Geophys Res, 2007, 112(A6): A06109
Karimabadi H, Driscoll J, Omelchenko Y A, et al. A new asynchronous methodology for modeling of physical systems: breaking the curse of Courant condition. J Comput Phys, 2005, 205(2): 755–775
Omelchenko Y A, Karimabadi H. Self-adaptive time integration of flux-conservativeequations with sources. J Comput Phys, 2006, 216(1): 179–194
Omelchenko Y A, Karimabadi H. Event-driven hybrid particle-in-cell simulation: a new paradigm for multi-scale plasma modeling. J Comput Phys, 2006, 216(1): 153–178
Omelchenko Y A, Karimabadi H. A time-accurate explicit multi-scale technique for gas dynamics. J Comput Phys, 2007, 226(1): 282–300
Unfer T, Boeuf J P, Rogier F, et al. An asynchronous scheme with local time stepping for multi-scale transport problems: Application to gas discharges. J Comput Phys, 2007, 227(2): 898–918
Feng X. A class of TVD type combined numerical scheme for MHD equations and its application to MHD numerical simulation (in Chinese). Chin J Space Sci, 2002, 22(4): 300–308
Tóth G. The ∇ · B =0 constraint in shock-capturing magnetohydrodynamics codes. J Comput Phys, 2000, 161(2): 605–652
Parker E N. Interplanetary Dynamical Processes. New York: Wiley-Interscience, 1963
Hu Y, Feng X, Wu S T, et al. Three-dimensional MHD modeling of the global corona throughout Solar Cycle 23. J Geophys Res, 2008, 113(A3): A03106
Svalgaard L, Duvall T L, Scherrer P H. The strength of the suns polar fields. Sol Phys, 1978, 58(2): 225–239
Svalgaard L. How good (or bad) are the inner boundary conditions for heliospheric solar wind modeling. SHINE 2006 Workshop. Utah: Rice University, 2006
Wang Y M, Sheeley Jr N R. On potential field models of the solar corona. Astrophys J, 1992, 392(1): 310–319
Luhmann J G, Li Y, Arge C N, et al. Solar cycle changes in coronal holes and space weather cycles. J Geophys Res, 2002, 107(A8): 1154
McComas D J, Barraclough B L, Funsten H O, et al. Solar wind observations over Ulysses’ first full polar orbit. J Geophys Res, 2000, 105(A5): 10419–10434
McComas D J, Elliott H A, Schwadron N A, et al. The three-dimensional solar wind around solar maximum. Geophys Res Lett, 2003, 30(10): 24–1
McComas D J, Elliott H A, Gosling J T, et al. Ulysses observations of very different heliosphere structure during the declining phase of solar activity cycle 23. Geophys Res Lett, 2006, 33(9): L09102
Ogawa T, Den M, Tanaka T. Three-dimensional hydrodynamic code for interplanetary shock wave. In: Proceedings of ISSS-7. Kyoto: Kyoto University, 2005. 26–28
Dryer M. Multi-dimensional MHD simulation of solar-generated disturbances: Space weather forecasting of geomagnetic storms. AIAA J, 1998, 36(3): 365–370
Fry C D, Sun W, Deehr C S, et al. Improvements to the HAF solar wind model for space weather predictions. J Geophys Res, 2001, 106(A10): 20985–21002
Odstrcil D, Riley P, Zhao X P. Numerical simulation of the 12 May 1997 interplanetary CME event. J Geophys Res, 2004, 109(A2): A02116
Zhou Y F, Feng X, Wu S T. Numerical simulation of the 12 May 1997 CME event. Chin Phys Lett, 2008, 25(2): 790–793
Lepping R P, Jones J A, Burlaga L F. Magnetic field structure of interplanetary magnetic clouds at 1AU. J Geophys Res, 1990, 95(A8): 957–965
Lynch B J, Zurbuchen T H, Fisk L A, et al. Internal structure of magnetic clouds: plasma and composition. J Geophys Res, 2003, 108(A6): SSH 6-1, 1239
Author information
Authors and Affiliations
Corresponding author
Additional information
Supported by the National Natural Science Foundation of China (Grant No. 40874077, 40621003, 40874091, 40536029, 40523006 and 40604019), the National Basic Research Program of China (“973” Project) (Grant No. 2006CB806304), and the Specialized Research Fund for State Key Laboratories
Rights and permissions
About this article
Cite this article
Shen, F., Feng, X. & Song, W. An asynchronous and parallel time-marching method: Application to three-dimensional MHD simulation of solar wind. Sci. China Ser. E-Technol. Sci. 52, 2895–2902 (2009). https://doi.org/10.1007/s11431-009-0291-1
Received:
Accepted:
Published:
Issue Date:
DOI: https://doi.org/10.1007/s11431-009-0291-1