THREE-DIMENSIONAL SOLAR<i>WIND</i>MODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID

Feng, Xueshang; Yang, Liping; Cui, Xiang; Wu, S. T.; Zhou, Yufen; Zhong, Dingkun

doi:10.1088/0004-637x/723/1/300

Cited by 174 publications

(156 citation statements)

References 114 publications

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“…The Alfvén wave pressure prediction is determined along the PFSS magnetic field, while the final obtained field line topology of the solar wind model departs from this PFSS field so that the velocity profile at 1 AU is likely to be different from the WSA predicted values. Actually, some studies found the WSA model yields higher solar wind speed at the source surface than the MHD model does (Feng et al 2010). To overcome this issue, we may need a self-consistent method to treat the inner boundary for Alfvén wave energy.…”

Section: Discussionmentioning

confidence: 99%

A Global Two-Temperature Corona and Inner Heliosphere Model: A Comprehensive Validation Study

Jin

Manchester

Holst

et al. 2011

ApJ

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The recent solar minimum with very low activity provides us a unique opportunity for validating solar wind models. During CR2077 (2008 November 20 through December 17), the number of sunspots was near the absolute minimum of solar cycle 23. For this solar rotation, we perform a multi-spacecraft validation study for the recently developed three-dimensional, two-temperature, Alfvén-wave-driven global solar wind model (a component within the Space Weather Modeling Framework). By using in situ observations from the Solar Terrestrial Relations Observatory (STEREO) A and B, Advanced Composition Explorer (ACE), and Venus Express, we compare the observed proton state (density, temperature, and velocity) and magnetic field of the heliosphere with that predicted by the model. Near the Sun, we validate the numerical model with the electron density obtained from the solar rotational tomography of Solar and Heliospheric Observatory/Large Angle and Spectrometric Coronagraph C2 data in the range of 2.4 to 6 solar radii. Electron temperature and density are determined from differential emission measure tomography (DEMT) of STEREO A and B Extreme Ultraviolet Imager data in the range of 1.035 to 1.225 solar radii. The electron density and temperature derived from the Hinode/Extreme Ultraviolet Imaging Spectrometer data are also used to compare with the DEMT as well as the model output. Moreover, for the first time, we compare ionic charge states of carbon, oxygen, silicon, and iron observed in situ with the ACE/Solar Wind Ion Composition Spectrometer with those predicted by our model. The validation results suggest that most of the model outputs for CR2077 can fit the observations very well. Based on this encouraging result, we therefore expect great improvement for the future modeling of coronal mass ejections (CMEs) and CME-driven shocks.

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Section: Discussionmentioning

confidence: 99%

A Global Two-Temperature Corona and Inner Heliosphere Model: A Comprehensive Validation Study

Jin

Manchester

Holst

et al. 2011

ApJ

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“…The details of the 3D SIP-CESE MHD model were described in Feng, Zhou, and Wu (2007) and Feng et al (2010). In this section only the basic features and modifications specific to this study are given.…”

Section: The 3d Sip-cese Mhd Modelmentioning

confidence: 99%

“…In the present study, we will use the three-dimensional (3D) SolarInterPlanetary Conservation Element/Solution Element (SIP-CESE) Magnetohydrodynamic (MHD) model (Feng, Zhou, and Wu, 2007;Feng et al, 2010) to numerically investigate the peculiarities of the current minimum and to explore their relationship with the polar magnetic fields on the solar surface. In order to achieve this, we have chosen CR 2070 as the simulation time interval and we will compare the numerical results with observations from multiple satellites, such as SOHO, Ulysses, Solar Terrestrial Relations Observatory (STEREO, Kaiser et al, 2008), Wind (Lepping et al, 1995) and ACE.…”

Section: Introductionmentioning

confidence: 99%

Simulation of the Unusual Solar Minimum with 3D SIP-CESE MHD Model by Comparison with Multi-Satellite Observations

et al. 2011

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The observations both near the Sun and in the heliosphere during the activity minimum between solar cycles 23 and 24 exhibit different phenomena from those typical of the previous solar minima. In this paper, we have chosen Carrington rotation 2070 in 2008 to investigate the properties of the background solar wind by using the three-dimensional (3D) Solar-InterPlanetary Conservation Element/Solution Element Magnetohydrodynamic (MHD) model. We also study the effects of polar magnetic fields on the characteristics of the solar corona and the solar wind by conducting simulations with an axisymmetric polar flux added to the observed magnetic field. The numerical results are compared with the observations from multiple satellites, such as the Solar and Heliospheric Observatory (SOHO), Ulysses, Solar Terrestrial Relations Observatory (STEREO), Wind and the Advanced Composition Explorer (ACE). The comparison demonstrates that the first simulation with the observed magnetic fields reproduces some observed peculiarities near the Sun, such as relatively small polar coronal holes, the presence of mid-and low-latitude holes, a tilted and warped current sheet, and the broad multiple streamers. The numerical results also capture the inconsistency between the locus of the minimum wind speed and the location of the heliospheric current sheet, and predict slightly slower and cooler polar streams with a relatively smaller latitudinal width, broad low-latitude intermediate-speed streams, and globally weak magnetic field and low density in the heliosphere. The second simulation with strengthened polar fields indicates that the weak polar fields in the current minimum play a crucial role in determining the states of the corona and the solar wind.

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“…These, however, require some form of interpolation scheme to establish a seamless connection between the sub-grids, which usually destroys the conservative properties of the code within the interpolation region. For applications of these grids to 3-D solar wind modeling see Feng et al (2010Feng et al ( , 2011. Cartesian coordinates, which do not present such difficulties, remain popular among CME modelers for exactly this reason, although the implementation of spherical boundaries like the photosphere then either requires some form of weighted interpolation procedure (e.g.…”

Section: Numerical Mhd Propagation Modelsmentioning

confidence: 99%

4π Models of CMEs and ICMEs (Invited Review)

Kleimann¹

2012

Sol Phys

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Coronal mass ejections (CMEs), which dynamically connect the solar surface to the far reaches of interplanetary space, represent a major manifestation of solar activity. They are not only of principal interest but also play a pivotal role in the context of space weather predictions. The steady improvement of both numerical methods and computational resources during recent years has allowed for the creation of increasingly realistic models of interplanetary CMEs (ICMEs), which can now be compared to high-quality observational data from various space-bound missions. This review discusses existing models of CMEs, characterizing them by scientific aim and scope, CME initiation method, and physical effects included, thereby stressing the importance of fully 3-D ('4π') spatial coverage.

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THREE-DIMENSIONAL SOLARWINDMODELING FROM THE SUN TO EARTH BY A SIP-CESE MHD MODEL WITH A SIX-COMPONENT GRID

Cited by 174 publications

References 114 publications

A Global Two-Temperature Corona and Inner Heliosphere Model: A Comprehensive Validation Study

A Global Two-Temperature Corona and Inner Heliosphere Model: A Comprehensive Validation Study

Simulation of the Unusual Solar Minimum with 3D SIP-CESE MHD Model by Comparison with Multi-Satellite Observations

4π Models of CMEs and ICMEs (Invited Review)

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