Automated Author ProfileBingham, S.
UNH
Bingham, S.
Current S-Index
Sum of Dataset Indices for all datasets
Average Dataset Index per Dataset
Average Dataset Index per dataset
Total Datasets
Total datasets for this author
Average FAIR Score
Average FAIR Score per dataset
Total Citations
Total citations to the author's datasets
Total Mentions
Total mentions of the author's datasets
S-Index Interpretation
The S-Index (Sharing Index) is a comprehensive metric that represents the cumulative impact of all your datasets. It is calculated as the sum of Dataset Index scores across all your claimed datasets.
What it means:
- A higher S-index indicates greater overall impact of your datasets relative to typical datasets in their fields of research
- The S-Index grows as you add more datasets or as existing datasets gain more citations and mentions
- It provides a single number to track your research data impact over time
Current S-Index: 1.9 (sum of 2 datasets Dataset Index scores)
More information here.
S-Index Over Time
Cumulative Citations Over Time
Cumulative Mentions Over Time
Datasets
Summary of data files. This is the dataset for a paper "A case study on the origin of near-Earth Plasma"
submitted to JGR-space by Glocer et al The paper conducts multifluid MHD simulations of the magnetosphere by the
BATSRUS code, with solar wind input, ionospheric outflow by the PWOM code,
and ionospheric potential solver, and inner magnetospehre by the CIMI code.
Solutions with and without plasmasphere are considered. All plots in the paper are made with spacepy (specific fork:
https://github.com/aglocer/spacepy) or with tecplot The data is organized as follows Top directory:
imf.dat: Has the solar wind input as a simple time series. Can be read and
plotted with the "ImfInput" tool in spacepy tared Directories with "PS" and "noPS" tags have simulation
output with and without plasmasphere. Each has three subdirectories described
as follows: GM: Has the "Global Magnetosphere" output from BATSRUS for the images shown.
y=0*out are cuts in the y=0 GSM plane and the *log file is the log output
containing Dst. Both can be plotted with spacepy pybats. The 3d files are
used in a few images and are tecplot binary files and read and plotted with
tecplot. PW: Has the "Polar Wind" output from the PWOM code for images shown. The
*out files are time dependent binary output for each field line. They can be
read and plotted with the pybats.pwom tool in spacepy. North and South
indicte northern and southern hemisphere respectively IE: Has the "Ionosphere Electrodynamics" output from the potential solver for
plots shown. the *log files have the CPCP data as a function of time. They
can be read and plotted with pybats in spacepy IM: Has the "Inner Magnetosphere" output from the CIMI code. The CIMIeq.out
file has time dependent snapshots of the solution on the min B surface for
plots shown. The *log files have the total energy as a function of time for
each species (among other variables). Both files are read and plotted with
pybats and pybats.cimi code in spacepy.
Authors
- Glocer, A. ;
- Welling, D. ;
- Chappel, C.R. ;
- Toth, G. ;
- Fok, M.-C. ;
- Komar, C. ;
- Kang, S.-B. ;
- Buzulukova, N. ;
- Ferradas, C. ;
- Bingham, S. ;
- Mouikis, C.
Summary of data files. This is the dataset for a paper "A case study on the origin of near-Earth Plasma"
submitted to JGR-space by Glocer et al The paper conducts multifluid MHD simulations of the magnetosphere by the
BATSRUS code, with solar wind input, ionospheric outflow by the PWOM code,
and ionospheric potential solver, and inner magnetospehre by the CIMI code.
Solutions with and without plasmasphere are considered. All plots in the paper are made with spacepy (specific fork:
https://github.com/aglocer/spacepy) or with tecplot The data is organized as follows Top directory:
imf.dat: Has the solar wind input as a simple time series. Can be read and
plotted with the "ImfInput" tool in spacepy tared Directories with "PS" and "noPS" tags have simulation
output with and without plasmasphere. Each has three subdirectories described
as follows: GM: Has the "Global Magnetosphere" output from BATSRUS for the images shown.
y=0*out are cuts in the y=0 GSM plane and the *log file is the log output
containing Dst. Both can be plotted with spacepy pybats. The 3d files are
used in a few images and are tecplot binary files and read and plotted with
tecplot. PW: Has the "Polar Wind" output from the PWOM code for images shown. The
*out files are time dependent binary output for each field line. They can be
read and plotted with the pybats.pwom tool in spacepy. North and South
indicte northern and southern hemisphere respectively IE: Has the "Ionosphere Electrodynamics" output from the potential solver for
plots shown. the *log files have the CPCP data as a function of time. They
can be read and plotted with pybats in spacepy IM: Has the "Inner Magnetosphere" output from the CIMI code. The CIMIeq.out
file has time dependent snapshots of the solution on the min B surface for
plots shown. The *log files have the total energy as a function of time for
each species (among other variables). Both files are read and plotted with
pybats and pybats.cimi code in spacepy.
Authors
- Glocer, A. ;
- Welling, D. ;
- Chappel, C.R. ;
- Toth, G. ;
- Fok, M.-C. ;
- Komar, C. ;
- Kang, S.-B. ;
- Buzulukova, N. ;
- Ferradas, C. ;
- Bingham, S. ;
- Mouikis, C.