Block-Adaptive-Tree-Solarwind-Roe-Upwind-Scheme Research Articles

Efficient OpenMP parallelization to a complex MPI parallel magnetohydrodynamics code

The state-of-the-art finite volume/difference magnetohydrodynamics (MHD) code Block Adaptive Tree Solarwind Roe Upwind Scheme (BATS-R-US) was originally designed with pure MPI parallelization. The maximum problem size achievable was limited by the storage requirements of the block tree structure. To mitigate this limitation, we have added multi-threaded OpenMP parallelization to the previous pure MPI implementation. We opted to use a coarse-grained approach by making the loops over grid blocks multi-threaded and have succeeded in making BATS-R-US an efficient hybrid parallel code with modest changes in the source code while preserving the performance. Good weak scalings up to hundreds of thousands of cores were achieved both for explicit and implicit time stepping schemes. This parallelization strategy greatly extended the possible simulation scale from 16,000 cores to more than 500,000 cores with 2GB/core memory on the Blue Waters supercomputer. Our work also revealed significant performance issues for some of the compilers when the code is compiled with the OpenMP library, probably related to the less efficient optimization of a complex multi-threaded region.

Study of Variation of Polar Cap Potential During Geomagnetic Storm Events of 24 November 2001 and 24 August 2005 as Observed From LFM and BATS‐R‐US Simulation

AbstractIn this paper we examine variation of polar cap potential (PCP) during two storm events that occurred on 24 November 2001 and 24 August 2005 using Lyon‐Fedder‐Mobarry (LFM) and Block‐Adaptive‐Tree‐Solarwind_Roe‐Upwind‐Scheme (BATS‐R‐US) simulations and compare it to Weimer model. These events were simulated for zero, pure By, pure Bz, and full IMF conditions separately, and the PCP obtained were compared with the zero IMF PCP value as a baseline (viscous) potential. For southward IMF, PCP is defined as sum of reconnection and viscous, whereas for northward IMF, it is peak to peak potential, which either will be viscous potential or reconnection potential, whichever is larger. Both events were simulated for a constant ionospheric conductivity of 5 mhos and the variation of PCP was found to be consistent with previous literatures. Furthermore, we found that BATS‐R‐US PCP fluctuated similar to LFM PCP for most parts although their PCP values did not exactly match. We observed that BATS‐R‐US PCP also goes below viscous value for northward IMF condition, something which was observed previously in LFM simulation only. We also found that BATS‐R‐US PCP is more sensitive to smaller fluctuation of IMF compared to LFM. For 24 August 2005 event, we found the PCP reach up to 550 and 440 kV and the viscous potential reached up to 120 and 110 kV for BATS‐R‐US and LFM, respectively. Similarly, for 24 November 2001 event PCP reached up to 800 and 400 kV and viscous potential reached up to 300 and 200 kV, respectively, for BATS‐R‐US and LFM.

Synthetic Radio Imaging for Quiescent and CME-flare Scenarios

Abstract Radio observations grant access to a wide range of physical processes through different emission mechanisms. These processes range from thermal and quiescent to eruptive phenomena, such as shock waves and particle beams. We present a new synthetic radio imaging tool that calculates and visualizes the bremsstrahlung radio emission. This tool works concurrently with state-of-the-art magnetohydrodynamic simulations of the solar corona using the code Block-Adaptive Tree Solarwind Roe Upwind Scheme (BATS-R-US). Our model produces results that are in good agreement with both high- and low-frequency observations of the solar disk. In this study, a ray-tracing algorithm is used, and the radio intensity is computed along the actual curved ray trajectories. We illustrate the importance of refraction in locating the radio-emitting source by comparison of the radio imaging illustrations when the line of sight is considered instead of the refracted paths. We are planning to incorporate nonthermal radio emission mechanisms in a future version of the radio imaging tool.

Advances in Space Weather Data Interpretation and Simulations

This editorial highlights recent data and model results for Space Weather readers. One of the ways that American Geophysical Union (AGU) features some of the most interesting journal articles is Editors' Highlights. As of late 2017 these are now hosted on the Eos website: https://eos.org/editor-highlights, giving them new prominence. Editors contribute a short summary of the highlighted article in language that will appeal to general Eos readers and include a “teaser” line and visually attractive figure from the manuscript. Doing so helps to share scientific content beyond a journal's readership to a broader audience. However, occasionally a situation arises, wherein an Editor sees a manuscript worthy of additional notoriety, but the summary simply needs more technical wording than might be appropriate for general readers. Below, I am highlighting two such manuscripts that illustrate advances in Space Weather (SWE). Based on analysis of total electron content estimated from Global Positioning System (GPS) and Defense Meteorological Satellite Program spacecraft measurements, Katamzi-Joseph et al. (2017) report the occurrence of ionospheric depletions (plasma bubbles) at anomalously high, European latitudes (42°N geographic) during two intense geomagnetic storms in 2000 and 2001. Somewhat counterintuitively, such depletions may develop in the postsunset sector where plasma density has been previously enhanced. GPS signals often scintillate passing through these bubbles. The authors suggest that conditions supporting rapid upward plasma drift near the equator can extend to the midlatitude ionosphere during storm time, making these regions susceptible to navigation signal scintillation during intense geomagnetic storms. They estimate a maximum apex height of the postsunset plasma depletions as ~4,000 km. The data for the two intense storms show that the evening enhancement of the equatorial ionization anomaly extended to middle-latitude Europe during the time of the plasma bubble occurrence. The authors propose an eastward penetrating electric field-associated with the interplanetary Bz southward turning as a possible mechanism for plasma enhancement and subsequent middle-latitude plasma bubbles. Although the midlatitude ionosphere is generally considered safe from radio signal scintillation effects, this study confirms that there may be no safe zone from space-based signal scintillation during intense storms. (See Mendillo et al., 2018; Wei et al., 2015, and references, within these for previous examples and further impacts.) The Space Weather Prediction Center (SWPC) now runs subsets of the models that comprise the Space Weather Modeling Framework (SWMF). See http://www.swpc.noaa.gov/news/announcing-geospace-model-version-15. Haiducek et al. (2017) simulated a month of geospace response for January 2005 using SWMF with the University of Michigan global magnetohydrodynamic code Block-Adaptive-Tree-Solarwind-Roe-Upwind-Scheme (BATS-R-US) coupled to the Rice Convection Model (RCM) inner magnetosphere and the Ridley Ionosphere Model. The interval included three large, previously simulated, and well-studied geospace storms. The authors launched the simulation three times. The first launch was with a standard 0.25 Earth radii (RE) SWMF resolution, corresponding to the operational version at SWPC. Then a higher (0.125 RE) resolution grid was applied with and without the RCM inner magnetosphere model. Various indices of geomagnetic activity (Kp, Sym-H, and AL) and the cross polar cap potential (CPCP), which is a proxy for geospace interaction with the solar wind, were calculated from the simulation and compared with observations and an empirical model that estimates CPCP. The SWMF model predicted the Sym-H (proxy for ring current) index very well. The Kp geomagnetic index and the CPCP are well predicted during storm conditions, but these indicators are overpredicted during quiet time. The model tends to underpredict the magnitude of the auroral electrojet, AL index. The Generally, the grid resolution has limited influence for the accuracy of the predictions except for auroral activity. However, the use of the inner magnetosphere model is essential. For the CPCP there is little effect from turning off the RCM. The Sym-H, AL, and Kp indexes, however, are very different when the inner magnetosphere model was turned off. This study is a significant step in showing how well one of the new SWPC models performs during storm conditions and in detailing the sensitivity in model driving. Importantly, the authors provide access to the model output for others to use. As an applications journal, SWE content covers data, model description and validation, and aspects of engineering that challenge even our technically savvy readers. So there are times when technical terms and acronyms might be problematic for a short highlight aimed at a wider readership. You can help SWE Editors promote and publicize as much content as possible by providing illustrative graphics with easy-to-follow captions and by writing plain language summaries of your manuscripts. In turn your Editors will work to highlight the best work. No data were created for this editorial.

Multispacecraft observations and modeling of the 22/23 June 2015 geomagnetic storm

AbstractThe magnetic storm of 22–23 June 2015 was one of the largest in the current solar cycle. We present in situ observations from the Magnetospheric Multiscale Mission (MMS) and the Van Allen Probes (VAP) in the magnetotail, field‐aligned currents from AMPERE (Active Magnetosphere and Planetary Electrodynamics Response), and ionospheric flow data from Defense Meteorological Satellite Program (DMSP). Our real‐time space weather alert system sent out a “red alert,” correctly predicting Kp indices greater than 8. We show strong outflow of ionospheric oxygen, dipolarizations in the MMS magnetometer data, and dropouts in the particle fluxes seen by the MMS Fast Plasma Instrument suite. At ionospheric altitudes, the AMPERE data show highly variable currents exceeding 20 MA. We present numerical simulations with the Block Adaptive Tree‐Solarwind ‐ Roe ‐ Upwind Scheme (BATS‐R‐US) global magnetohydrodynamic model linked with the Rice Convection Model. The model predicted the magnitude of the dipolarizations, and varying polar cap convection patterns, which were confirmed by DMSP measurements.

CME flux rope and shock identifications and locations: Comparison of white light data, Graduated Cylindrical Shell model, and MHD simulations

AbstractCoronal mass ejections (CMEs) are major transient phenomena in the solar corona that are observed with ground‐based and spacecraft‐based coronagraphs in white light or with in situ measurements by spacecraft. CMEs transport mass and momentum and often drive shocks. In order to derive the CME and shock trajectories with high precision, we apply the graduated cylindrical shell (GCS) model to fit a flux rope to the CME directed toward STEREO A after about 19:00 UT on 29 November 2013 and check the quality of the heliocentric distance‐time evaluations by carrying out a three‐dimensional magnetohydrodynamic (MHD) simulation of the same CME with the Block Adaptive Tree Solar‐Wind Roe Upwind Scheme (BATS‐R‐US) code. Heliocentric distances of the CME and shock leading edges are determined from the simulated white light images and magnetic field strength data. We find very good agreement between the predicted and observed heliocentric distances, showing that the GCS model and the BATS‐R‐US simulation approach work very well and are consistent. In order to assess the validity of CME and shock identification criteria in coronagraph images, we also compute synthetic white light images of the CME and shock. We find that the outer edge of a cloud‐like illuminated area in the observed and predicted images in fact coincides with the leading edge of the CME flux rope and that the outer edge of a faint illuminated band in front of the CME leading edge coincides with the CME‐driven shock front.

A statistical study into the spatial distribution and dawn‐dusk asymmetry of dayside magnetosheath ion temperatures as a function of upstream solar wind conditions

AbstractThe magnetosheath contains the shocked solar wind and behaves as a natural filter to the solar wind plasma before it reaches the magnetosphere. The redistribution of kinetic energy at the bow shock results in significant thermalization of the solar wind plasma, resulting in a magnetosheath temperature profile which is highly nonhomogeneous and nonisotropic and differs between the dawn and dusk flanks. The present study attempts to study the spatial distribution of magnetosheath ion temperature as a function of upstream solar wind conditions. We pay particular attention to the dawn/dusk asymmetry in which we attempt to quantify using experimental data collected over a 7 year period. We also compare these data to simulated data from both the Block‐Adaptive‐Tree‐Solarwind‐Roe‐Upwind‐Scheme (BATS‐R‐US) MHD code and a kinetic hybrid model. We present evidence that the dawn flank is consistently hotter than the dusk flank for a variety of upstream conditions. Our statistical data also suggest a dependency on solar wind speed such that the level of asymmetry increases with faster speeds. We conclude that the dawn‐favored asymmetry of the magnetosheath seed population is insufficient to explain the dawn asymmetry (30–40%) of cold component ions in the cold, dense plasma sheet, and therefore, other mechanisms are likely required.

Comparative analyses of current three-dimensional numerical solar wind models

We present a comparative study of the most advanced three-dimensional time-dependent numerical simulation models of solar wind. These models can be classified into two categories: (I) theoretical, empirical and numerically based models and (II) self-consistent multi-dimensional numerical magnetohydrodynamic (MHD) models. The models of Category I are used to separately describe the solar wind solution in two plasma flows regions: transonic/trans-Alfvenic and supersonic/super-Alfvenic, respectively. Models of Category II construct a complete, single, numerical solar wind solution through subsonic/sub-Alfvenic region into supersonic/super-Alfvenic region. The Wang-Sheeley-Arge (WSA)/ENLIL in CISM is the most successful space weather model that belongs to Category I, and the Block-Adaptive-Tree-Solarwind-Roe-Upwind-Scheme (BATS-R-US) code in SWMF (Space Weather Modeling Framework) and the solar-interplanetary conservative element solution element MHD (SIP-CESE MHD) model in SWIM (Space Weather Integrated Model) are the most commonly-used models that belong to Category II. We review the structures of their frameworks, the main results for solar wind background studies that are essential for solar transient event studies, and discuss the common features and differences between these two categories of solar wind models. Finally, we conclude that the transition of these two categories of models to operational use depends on the availability of computational resources at reasonable cost and point out that the models’ prediction capabilities may be improved by employing finer computational grids, incorporating more observational data and by adding more physical constraints to the models.

Modeling subauroral polarization streams during the 17 March 2013 storm

AbstractThe subauroral polarization streams (SAPS) are one of the most important features in representing magnetosphere‐ionosphere coupling processes. In this study, we use a state‐of‐the‐art modeling framework that couples an inner magnetospheric ring current model RAM‐SCB with a global MHD model Block‐Adaptive Tree Solar‐wind Roe Upwind Scheme (BATS‐R‐US) and an ionospheric potential solver to study the SAPS that occurred during the 17 March 2013 storm event as well as to assess the modeling capability. Both ionospheric and magnetospheric signatures associated with SAPS are analyzed to understand the spatial and temporal evolution of the electrodynamics in the midlatitude regions. Results show that the model captures the SAPS at subauroral latitudes, where Region 2 field‐aligned currents (FACs) flow down to the ionosphere and the conductance is lower than in the higher‐latitude auroral zone. Comparisons to observations such as FACs observed by Active Magnetosphere and Planetary Electrodynamics Response Experiment (AMPERE), cross‐track ion drift from Defense Meteorological Satellite Program (DMSP), and in situ electric field observations from the Van Allen Probes indicate that the model generally reproduces the global dynamics of the Region 2 FACs, the position of SAPS along the DMSP, and the location of the SAPS electric field around L of 3.0 in the inner magnetosphere near the equator. The model also demonstrates double westward flow channels in the dusk sector (the higher‐latitude auroral convection and the subauroral SAPS) and captures the mechanism of the SAPS. However, the comparison with ion drifts along DMSP trajectories shows an underestimate of the magnitude of the SAPS and the sensitivity to the specific location and time. The comparison of the SAPS electric field with that measured from the Van Allen Probes shows that the simulated SAPS electric field penetrates deeper than in reality, implying that the shielding from the Region 2 FACs in the model is not well represented. Possible solutions in future studies to improve the modeling capability include implementing a self‐consistent ionospheric conductivity module from inner magnetosphere particle precipitation, coupling with the thermosphere‐ionosphere chemical processes, and connecting the ionosphere with the inner magnetosphere by the stronger Region 2 FACs calculated in the inner magnetosphere model.

Solar wind interaction with Mars upper atmosphere: Results from the one‐way coupling between the multifluid MHD model and the MTGCM model

The 3‐D multifluid Block Adaptive Tree Solar‐wind Roe Upwind Scheme (BATS‐R‐US) MHD code (MF‐MHD) is coupled with the 3‐D Mars Thermospheric general circulation model (MTGCM). The ion escape rate from the Martian upper atmosphere is investigated by using a one‐way coupling approach, i.e., the MF‐MHD model incorporates the effects of 3‐D neutral atmosphere profiles from the MTGCM model. The calculations are carried out for two cases with different solar cycle conditions. The calculated total ion escape flux (the sum of three major ionospheric species, O+, , and ) for solar cycle maximum conditions (6.6×1024 s−1) is about 2.6 times larger than that of solar cycle minimum conditions (2.5×1024 s−1). Our simulation results show good agreement with recent observations of 2–3×1024 s−1 (O+, , and ) measured near solar cycle minimum conditions by Mars Express. An extremely high solar wind condition is also simulated which may mimic the condition of coronal mass ejections or corotating interaction regions passing Mars. Simulation results show that it can lead to a significant value of the escape flux as large as 4.3×1025s−1.

Kelvin‐Helmholtz instabilities at the magnetic cavity boundary of comet 67P/Churyumov‐Gerasimenko

We investigate the plasma environment of comet 67P/Churyumov‐Gerasimenko, the target of the European Space Agency's Rosetta mission. Rosetta will rendezvous with the comet in 2014 at almost 3.5 AU and follow it all the way to and past perihelion at 1.3 AU. During its journey towards the inner solar system the comet's environment will significantly change. The interaction of the solar wind with a well developed neutral coma leads to the formation of an upstream bow shock and, closer to the comet, the inner shock separating the solar wind, with cometary pick‐up ions mass‐loaded, from the inner cometary ions which are dragged outward through abundant collisions and charge exchange with the expanding neutral gas. As a consequence the interplanetary magnetic field is prevented from penetrating the innermost region of the comet, the so‐called magnetic cavity. We use our magnetohydrodynamics model BATSRUS (Block‐Adaptive‐Tree‐Solarwind‐Roe‐Upwind‐Scheme) to simulate the solar wind – comet interaction. The model includes photoionization, ion‐electron recombination, and charge exchange. Under certain conditions our model predicts an unstable plasma flow at the inner shock. We show that the plasma shear flow around the magnetic cavity can lead to Kelvin‐Helmholtz instabilities. We investigate the onset of this phenomenon with change of heliocentric distance and furthermore show that a previously stable magnetic cavity boundary can become unstable when the neutral gas is predominately released from the dayside of the comet.

CRASH: A BLOCK-ADAPTIVE-MESH CODE FOR RADIATIVE SHOCK HYDRODYNAMICS—IMPLEMENTATION AND VERIFICATION

We describe the CRASH (Center for Radiative Shock Hydrodynamics) code, a block adaptive mesh code for multi-material radiation hydrodynamics. The implementation solves the radiation diffusion model with the gray or multigroup method and uses a flux limited diffusion approximation to recover the free-streaming limit. The electrons and ions are allowed to have different temperatures and we include a flux limited electron heat conduction. The radiation hydrodynamic equations are solved in the Eulerian frame by means of a conservative finite volume discretization in either one, two, or three-dimensional slab geometry or in two-dimensional cylindrical symmetry. An operator split method is used to solve these equations in three substeps: (1) solve the hydrodynamic equations with shock-capturing schemes, (2) a linear advection of the radiation in frequency-logarithm space, and (3) an implicit solve of the stiff radiation diffusion, heat conduction, and energy exchange. We present a suite of verification test problems to demonstrate the accuracy and performance of the algorithms. The CRASH code is an extension of the Block-Adaptive Tree Solarwind Roe Upwind Scheme (BATS-R-US) code with this new radiation transfer and heat conduction library and equation-of-state and multigroup opacity solvers. Both CRASH and BATS-R-US are part of the publicly available Space Weather Modeling Framework (SWMF).

Self‐consistent inner magnetosphere simulation driven by a global MHD model

We present results from a one‐way coupling between the kinetic Ring Current Atmosphere Interactions Model with Self‐Consistent B field (RAM‐SCB) and the Space Weather Modeling Framework (SWMF). RAM‐SCB obtains plasma distribution and magnetic field at model boundaries from the Block Adaptive Tree Solar Wind Roe Upwind Scheme (BATS‐R‐US) magnetohydrodynamics (MHD) model and convection potentials from the Ridley Ionosphere Model within SWMF. We simulate the large geomagnetic storm of 31 August 2005 (minimum SYM‐H of −116 nT). Comparing SWMF output with Los Alamos National Laboratory geostationary satellite data, we find SWMF plasma to be too cold and dense if assumed to consist only of protons; this problem is alleviated if heavier ions are considered. With SWMF inputs, we find that RAM‐SCB reproduces well storm time magnetosphere features: ring current morphology, dusk side peak, pitch angle anisotropy, and total energy. The RAM‐SCB ring current and Dst are stronger than the SWMF ones and reproduce observations much better. The calculated field‐aligned currents (FAC) compare reasonably well with 2 h averaged pictures from Iridium satellite data. As the ring current peak rotates duskward in the storm main phase, the region 2 FACs rotate toward noon, a feature also seen in observations. Finally, the RAM‐SCB magnetic field outperforms both the dipole and the BATS‐R‐US field at Cluster and Polar spacecraft locations. This study shows the importance of a kinetic self‐consistent approach and the sensitive dependence of the storm time inner magnetosphere on plasma sheet conditions and the cross polar cap potential. The study showcases the RAM‐SCB capability as an inner magnetosphere module coupled with a global MHD model.

A general Cluster data and global MHD simulation comparison

Abstract. Among the many challenges facing the space weather modelling community today, is the need for validation and verification methods of the numerical models available describing the complex nonlinear Sun-Earth system. Magnetohydrodynamic (MHD) models represent the latest numerical models of this environment and have the unique ability to span the enormous distances present in the magnetosphere, from several hundred kilometres to several thousand kilometres above the Earth's surface. This makes it especially difficult to develop verification and validation methods which posses the same range spans as the models. In this paper we present a first general large-scale comparison between four years (2001–2004) worth of in situ Cluster plasma observations and the corresponding simulated predictions from the coupled Block-Adaptive-Tree-Solarwind-Roe-Upwind-Scheme (BATS-R-US) MHD code. The comparison between the in situ measurements and the model predictions reveals that by systematically constraining the MHD model inflow boundary conditions a good correlation between the in situ observations and the modeled data can be found. These results have an implication for modelling studies addressing also smaller scale features of the magnetosphere. The global MHD simulation can therefore be used to place localised satellite and/or ground-based observations into a global context and fill the gaps left by measurements.

Global MHD simulation of flux transfer events at the high‐latitude magnetopause observed by the Cluster spacecraft and the SuperDARN radar system

A global magnetohydrodynamic numerical simulation is used to study the large‐scale structure and formation location of flux transfer events (FTEs) in synergy with in situ spacecraft and ground‐based observations. During the main period of interest on the 14 February 2001 from 0930 to 1100 UT the Cluster spacecraft were approaching the Northern Hemisphere high‐latitude magnetopause in the postnoon sector on an outbound trajectory. Throughout this period the magnetic field, electron, and ion sensors on board Cluster observed characteristic signatures of FTEs. A few minutes delayed to these observations the Super Dual Auroral Radar Network (SuperDARN) system indicated flow disturbances in the conjugate ionospheres. These “two‐point” observations on the ground and in space were closely correlated and were caused by ongoing unsteady reconnection in the vicinity of the spacecraft. The three‐dimensional structures and dynamics of the observed FTEs and the associated reconnection sites are studied by using the Block‐Adaptive‐Tree‐Solarwind‐Roe‐Upwind‐Scheme (BATS‐R‐US) MHD code in combination with a simple open flux tube motion model (Cooling). Using these two models the spatial and temporal evolution of the FTEs is estimated. The models fill the gaps left by measurements and allow a “point‐to‐point” mapping between the instruments in order to investigate the global structure of the phenomenon. The modeled results presented are in good correlation with previous theoretical and observational studies addressing individual features of FTEs.

Modeling the Sun-to-Earth propagation of a very fast CME

We present a three-dimensional (3-D) numerical ideal magnetohydrodynamics (MHD) model describing the time-dependent propagation of a CME from the solar corona to Earth in just 18 h. The simulations are performed using the BATS-R-US (Block Adaptive Tree Solarwind Roe Upwind Scheme) code. We begin by developing a global steady-state model of the corona that possesses high-latitude coronal holes and a helmet streamer structure with a current sheet at the equator. The Archimedian spiral topology of the interplanetary magnetic field is reproduced along with fast and slow speed solar wind. Within this model system, we drive a CME to erupt by the introduction of a Gibson–Low magnetic flux rope that is embedded in the helmet streamer in an initial state of force imbalance. The flux rope rapidly expands, driving a very fast CME with an initial speed of in excess of 4000 km/s and slowing to a speed of nearly 2000 km/s at Earth. We find our model predicts a thin sheath around the flux rope, passing the earth in only 2 h. Shocked solar wind temperatures at 1 astronomical unit (AU) are in excess of 10 million degrees. Physics based AMR allows us to capture the structure of the CME focused on a particular Sun–Earth line with high spatial resolution given to the bow shock ahead of the flux rope.

Modeling a space weather event from the Sun to the Earth: CME generation and interplanetary propagation

We present a three‐dimensional (3‐D) numerical ideal magnetohydrodynamics (MHD) model describing the time‐dependent expulsion of a coronal mass ejection (CME) from the solar corona propagating to 1 astronomical unit (AU). The simulations are performed using the Block Adaptive Tree Solar‐Wind Roe Upwind Scheme (BATS‐R‐US) code. We begin by developing a global steady‐state model of the corona that possesses high‐latitude coronal holes and a helmet streamer structure with a current sheet at the equator. The Archimedean spiral topology of the interplanetary magnetic field is reproduced along with fast and slow speed solar wind. Within this model system, we drive a CME to erupt by the introduction of a Gibson‐Low magnetic flux rope that is anchored at both ends in the photosphere and embedded in the helmet streamer in an initial state of force imbalance. The flux rope rapidly expands and is ejected from the corona with maximum speeds in excess of 1000 km/s. Physics‐based adaptive mesh refinement (AMR) allows us to capture the structure of the CME focused on a particular Sun‐Earth line with high spatial resolution given to the bow shock ahead of the flux rope as well as to the current sheet behind. The CME produces a large magnetic cloud at 1 AU (>100 R⊙) in which Bz undergoes a full rotation from north to south with an amplitude of 20 nT. In a companion paper, we find that the CME is very effective in generating strong geomagnetic activity at the Earth in two ways. First, through the strong sustained southward Bz (lasting more than 10 hours) and, second, by a pressure increase associated with the CME‐driven shock that compresses the magnetosphere.