DOI: 10.5061/dryad.m0cfxpp9v
title: Magnetic field enhancements in the solar wind: Diverse processes manifesting a uniform observation type?

description: Within the solar wind throughout the inner heliosphere, observations
 reveal the presence of magnetic field enhancements accompanied by thin
 current sheets at varying distances from the sun and across different
 longitudes and latitudes. Two primary explanations have been proposed to
 elucidate these phenomena: Solar wind-dust interaction and interlacing
 flux ropes. In this study, we employ multi-fluid Magnetohydrodynamics
 (MHD) and Hall MHD models to simulate these hypotheses, respectively. Our
 findings indicate a concurrence between both models and the observed
 phenomena, suggesting that both processes may result in the same kind of
 enhancement. Furthermore, both models make predictions pointing to
 additional types of observational data, occurring at distinct spatial or
 temporal stages of the interaction. This convergence of model predictions
 with empirical data underscores the need for further observational and
 modeling studies to comprehensively test these models. This research
 enhances our knowledge of the inner heliosphere's dynamics and the
 influence of the solar wind on the Earth's magnetosphere, thereby
 shedding light on critical aspects of space weather and its potential
 impact on our planet.
description: Two modeles has been used to calculate these datasets:
 1, Multi-fluid MHD model if dust in the solar wind
 2, Hall MHD model on interlaced magnetic flux ropes. Two cases
 are available: H=+1 and -1 for the flux rope at x&gt;0.
 They are not processed. They are raw model results.
  
description: # Magnetic field enhancements in the solar wind: Diverse processes
 manifesting a uniform observation type?
 [https://doi.org/10.5061/dryad.m0cfxpp9v](https://doi.org/10.5061/dryad.m0cfxpp9v) Please find 3-D data for Figures 2, 3 and Figures 4, 5 of the paper with the same title: Ying-Dong Jia, Hairong Lai, Nathan Miles, et al. Magnetic Field Enhancements in the Solar Wind: Diverse Processes Manifesting a Uniform Observation Type? *Journal of Geophysical Research: Space Physics*, 129(3), e2023JA032255. [https://doi.org/10.1029/2023JA032255](https://doi.org/10.1029/2023JA032255) The 1-D data in Figures 3 and 5 can be extracted from these two 3-d datasets with the description in the paper, respectively. \**Figures 2 and 3: ** Dust3DMFMHDT008.zip Time-dependent 3-D multifluid MHD model result of charged dust in the solar wind at 1 AU. This data is at 8 minutes after the simulation starts. In this ASCII data, the first several lines contain a header that lists the names of the variables. **Figures 4 and 5:** T=00h: IFR3DHMHDT000.zip T=07h: IFR3DHMHDT007.zip T=10h: IFR3DHMHDT010.zip T=17h: IFR3DHMHDT017.zip Time-dependent 3-D Hall MHD model results of interlaced magnetic flux ropes (IFRs). The four files contain simulation results at 0, 7, 10, and 17 hours. The list of variables is included in the header of the file. These four files are also used to generate Figures 1a, 2a, 2b, and 3 in the second paper mentioned below. **After these, there is one additional file, of the same Hall MHD IFR case, except now H=-1 at x&gt;0.** T=17h: IFR3DnHMHDT017.zip This data file is used for Figures 1b and 2d in another paper: Jia, Ying-Dong, Yi Qi; Xueyi Wang et al. (2024), Counter-helical magnetic flux ropes from magnetic reconnections in space plasmas, GeophysicalResearchLetters,51,e2024GL108270. [https://doi.org/10.1029/2024GL108270](https://doi.org/10.1029/2024GL108270) ## Description of the data and file structure ASCII data after zip compression. **File 1 "Dust3DMFMHDT008.dat" file header and sample data:** *xyz units R=1R_E, Earth radii 6378km. TITLE = "BATSRUS: 3D Data, 1986/12/27 12:40:04.351" VARIABLES = "X [R]" "Y [R]" "Z [R]" "B_x [nT]" "B_y [nT]" "B_z [nT]" "`rH^p [amu/cm^3]" "U_xH^p [km/s]" "U_yH^p [km/s]" "U_zH^p [km/s]" "pH^p [nPa]" "`r^D^u^s^t [amu/cm^3]" "U_x^D^u^s^ [km/s]" "U_y^D^u^s^ [km/s]" "U_z^D^u^s^ [km/s]" "p^D^u^s^t [nPa]" ZONE T="3D N=0006000 T=0000:08:04" STRANDID=0, SOLUTIONTIME=0 Nodes=12476537, Elements=12236800, ZONETYPE=FEBrick DATAPACKING=POINT AUXDATA BLOCKS="23900 8 x 8 x 8" AUXDATA BODYNUMDENSITY="5.00" AUXDATA BORIS="F" AUXDATA BTHETATILT="0.0000" AUXDATA CELLS="12236800" AUXDATA CELLSUSED="12236800" AUXDATA CODEVERSION="BATSRUS 9.20" AUXDATA COORDSYSTEM="GSM" AUXDATA COROTATION="F" AUXDATA FLUXTYPE="Linde" AUXDATA GAMMA="1.666667" AUXDATA ITER="6000" AUXDATA NPROC="800" AUXDATA ORDER="2 minmod, beta= 1.00000" AUXDATA RBODY="3.00" AUXDATA SAVEDATE="Save Date: 2022/06/08 at 22:56:53" AUXDATA TIMEEVENT="1986/12/27 12:40:04.351" AUXDATA TIMEEVENTSTART="1986/12/27 12:32:00.000" AUXDATA TIMESIM="T=0000:08:04" AUXDATA TIMESIMSHORT="T=0000:08" DT=(SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE ) -1.000000000E+01 -1.000000000E+01 -1.000000000E+01 3.000000000E+00 4.000000000E+00 2.136649927E-14 5.000000000E+00 6.000000000E+01 7.770169924E-11 1.112579984E-08 6.903499831E-03 4.999489889E-08 7.980580442E-03 -1.005470008E-02 -1.115090013E+00 6.903500124E-14 **All the rest Files 2-6 "IFR3D?HMHDT0??.dat" file header and sample data:** *xyz units R=1Mm. TITLE = "BATSRUS: 3D Data, 2015/05/01 00:00:00.000" VARIABLES = "X [R]" "Y [R]" "Z [R]" "Rho [amu/cm^3]" "U_x [km/s]" "U_y [km/s]" "U_z [km/s]" "B_x [nT]" "B_y [nT]" "B_z [nT]" "P [nPa]" "J_x [`mA/m^2]" "J_y [`mA/m^2]" "J_z [`mA/m^2]" ZONE T="3D N=0000000 T=0000:00:00" STRANDID=0, SOLUTIONTIME=0 Nodes=4515425, Elements=4423680, ZONETYPE=FEBrick DATAPACKING=POINT AUXDATA BLOCKS=" 8640 8 x 8 x 8" AUXDATA BODYNUMDENSITY=" 5.00" AUXDATA BORIS="F" AUXDATA BTHETATILT=" -18.0956" AUXDATA CELLS=" 4423680" AUXDATA CELLSUSED=" 4423680" AUXDATA CODEVERSION="BATSRUS 9.90" AUXDATA COORDSYSTEM="GSM" AUXDATA COROTATION="F" AUXDATA GAMMA=" 1.666667" AUXDATA ITER=" 0" AUXDATA NPROC=" 480" AUXDATA ORDER=" 2 minmod, beta= 1.00000" AUXDATA RBODY=" 0.00" AUXDATA SAVEDATE="Save Date: 2023/10/27 at 11:49:28" AUXDATA TIMEEVENT="2015/05/01 00:00:00.000" AUXDATA TIMEEVENTSTART="2015/05/01 00:00:00.000" AUXDATA TIMESIM="T=0000:00:00" AUXDATA TIMESIMSHORT="T=0000:00" AUXDATA TypeFlux="Linde " DT=(SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE SINGLE ) -3.2000000E+02 -1.6000000E+02 -1.6000000E+02 5.0000000E+00 -1.2756000E+01 0.0000000E+00 0.0000000E+00 0.0000000E+00 0.0000000E+00 0.0000000E+00 3.4517501E-02 0.0000000E+00 0.0000000E+00 0.0000000E+00 ## Code/Software The BARS-R-US code used in the study is available for download as a component of the Space Weather Modeling Framework at the University of Michigan ([http://clasp.engin.umich.edu/swmf](http://clasp.engin.umich.edu/swmf)).