Combining radiative transfer and diffuse interstellar medium physics to model star formation (Dataset)
BE_Collapse_LinesOfSight.zip (13.15Gb) BE_Collapse_OverlappingCircles.zip (12.35Gb) BE_Collapse_WhiBat2006_10K.zip (8.780Gb) BE_Collapse_WhiBat2006_14K.zip (8.868Gb) BE_KF05_1.zip (968.5Mb) BE_KF05_1_hexagonal.zip (31.74Mb) BE_KF05_2.zip (290.6Mb) GloverClark2012_Analysis.zip (10.74Gb) Paper.zip (2.096Gb) Uniform.zip (1.228Gb) nH_300.zip (534.7Mb) nH_300_H2_Metal001_H2full.zip (15.57Gb) nH_300_H2_Metal001_H2full_NoCR.zip (22.72Gb) nH_300_H2_Metal001_H2full_NoCR_NoPhotoHeat.zip (20.11Gb) nH_300_H2_Metal001_H2full_atomic.zip (16.15Gb) nH_300_H2_Metal001_H2full_atomic_NoCR.zip (28.70Gb) nH_300_H2_Metal001_H2full_atomic_NoCR_NoPhotoHeat.zip (28.70Gb) nH_300_H2_Metal01_H2full.zip (20.84Gb) nH_300_H2_Metal01_H2full_NoCR.zip (20.81Gb) nH_300_H2_Metal01_H2full_NoCR_NoPhotoHeat.zip (20.49Gb) nH_300_H2_Metal01_H2full_atomic.zip (26.29Gb) nH_300_H2_Metal01_H2full_atomic_NoCR.zip (26.29Gb) nH_300_H2_Metal01_H2full_atomic_NoCR_NoPhotoHeat.zip (26.55Gb) nH_300_H2_Metal1_H2full.zip (20.85Gb) nH_300_H2_Metal1_H2full_NoCR.zip (19.99Gb) nH_300_H2_Metal1_H2full_NoCR_NoPhotoHeat.zip (19.97Gb) nH_300_H2_Metal1_H2full_atomic.zip (27.30Gb) nH_300_H2_Metal1_H2full_atomic_NoCR.zip (26.96Gb) nH_300_H2_Metal1_H2full_atomic_NoCR_NoPhotoHeat.zip (26.57Gb) nH_300_H2_Metal1_selfshield3_heating_GC165_dissipative_Depl_NoHeating.zip (21.16Gb) nH_300_H2_Metal1_selfshield3_heating_GC165_dissipative_Depl_NoHeating_Cplus.zip (16.95Gb) nH_300_H2_Metal1_selfshield3_heating_GC165_dissipative_Depl_NoHeating_DustKF.zip (21.79Gb) nH_300_H2_Metal1_selfshield3_heating_GC165_dissipative_Depl_NoHeating_Line3.zip (18.32Gb) nH_300_H2_Metal1_selfshield3_heating_GC165_dissipative_NoDepl_NoHeating.zip (19.91Gb) nH_300_H2_Metal1_selfshield3_heating_GC165_dissipative_NoDepl_NoHeating_2.zip (19.90Gb) nH_300_H2_Metal3_H2full_NoCR.zip (18.55Gb) nH_300_H2_Metal3_H2full_NoCR_NoPhotoHeat.zip (18.42Gb) nH_300_H2_Metal3_H2full_atomic_NoCR.zip (19.74Gb) nH_300_H2_Metal3_H2full_atomic_NoCR_NoPhotoHeat.zip (22.46Gb)Show MoreShow Less
Keto, Eric R.
Bate, Matthew R.
Monthly Notices of the Royal Astronomical Society
University of Exeter (dataset) / Oxford University Press (paper)
Creative Commons Attribution (BY) license. Acknowledge source by citing the authors' names, the published MNRAS paper, and the ORE handle for the dataset.
This is the dataset that was used to produce the associated paper, published in MNRAS. It contains the output from each of the SPH simulations, including dump files and the scripts used to generate the figures for the paper. To view the paper follow the DOI or linked handle.
DiRac Complexity computer: jointly funded by Science and Technology Facilities Council (STFC) and the Large Facilities Capital Fund of BIS
University of Exeter Supercomputer: jointly funded by Science and Technology Facilities Council (STFC), Large Facilities Capital Fund of BIS, and the University of Exeter
European Research Council (ERC)
This repository contains the datasets from the original smoothed particle hydrodynamics (SPH) calculations for the associated paper (Bate & Keto, 2015, MNRAS, 449 (3) 2643-2667). It includes dump files and all of the scripts for generating the figures that appear in the paper. The scripts are contained either in the GloverClark2012_Analysis.zip file or in the Paper.zip file. The former mainly contains SPLASH scripts (see below) for generating images from the SPH dump files. The latter mainly contains the final (or intermediate) SPLASH figures, plus the data files and scripts for making the other figures (line plots). Line plots use supermongo scripts. There are 4 results sections in the paper (Sections 4.1 to 4.4). The output from the SPH calculations discussed in Section 4.1 are contained in the file: Uniform.zip. SPH calculations discussed in Section 4.2 are contained in the files: BE_KF05_*.zip. SPH calculations discussed in Section 4.3 are contained in the files: BE_Collapse_*.zip. The remaining files (all beginning with nH_300_H2_*) contain the turbulent cloud calculations associated with Section 4.4 of the paper. The initial conditions for these turbulent cloud calculations are contained in the file nH_300.zip. The SPH dump files for each calculation begin at TEST000 at time zero and then are numbered sequentially. The SPH calculations for Sections 4.1 and 4.2 are static calculations (i.e. there is only an initial dump file, with the required data written out separately). The SPH dump files are Fortran binary files, written in big endian format and generated by the sphNG code. They can be read, visualised, and manipulated using the free, publicly available SPLASH visualisation code (which reads sphNG dump files), written by Daniel Price, that can be downloaded from: http://users.monash.edu.au/~dprice/splash/
The journal article associated with this dataset can be found in ORE at http://hdl.handle.net/10871/18335
Vol. 449 (3), pp. 2643-2667