The dependence of protostar formation on the geometry and strength of the initial magnetic field (Dataset)
Lewis, Benjamin T.
Bate, Matthew R.
Monthly Notices of the Royal Astronomical Society
University of Exeter (dataset) / Oxford University Press (paper)
Available under a CC-BY (v. 2.0 UK: England and Wales) License. Please acknowledge source by citing the published MNRAS paper and the ORE handle for this dataset.
This is the dataset that was used to produce the paper published in MNRAS. Included are the binary dump files from all twelve of the calculations in the paper.
Science and Technology Facilities Council
European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)
Australian Research Council
This work used the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of the National E-Infrastructure.
Calculations were also performed on the University of Exeter Supercomputer, a DiRAC Facility jointly funded by STFC, the Large Facilities Capital Fund of BIS and the University of Exeter.
The compressed tarballs in this repository contain the binary output data from the SPMHD (smoothed particle magnetohydrodynamics) simulation presented in the paper. The data is a Fortran binary file in big-endian format. The DAT???? files are dumps of the simulation spaced every 1/100 of a free-fall time and can be read in Splash (written by Daniel Price, see http://users.monash.edu.au/~dprice/splash/). The Atest_? and Ptest_? files contain information on accreted particles and sink particles respectively (again in big-endian format) which can be converted to ASCII for further processing using the ptdump and accdump utilities (see utils.tar.xz in https://ore.exeter.ac.uk/repository/handle/10871/17109).
The tarballs themselves are named according to the following scheme: YY-XX.tar.xz, where YY is the mass-to-flux ratio used in the calculation (so a ratio of 5 would be 05, etc.) and where XX is the inclination angle between the rotation and magnetic field axes in degrees (so 00 would be parallel, and 90 would be perpendicular, and so on).
Aside from figure 13, the rendered plots in the paper can be produced using the splash code and the `DAT' files directly. Line plots either use data from the `DAT' files or the `A' and `P' files as appropriate; figure 13 is a projection of data from the `A' files.