Dataset for Elsender & Bate (2024): An implicit algorithm for simulating the dynamics of small dust grains with smoothed particle hydrodynamics

This dataset contains 10 files with the data used to create the 11 figures in the journal paper:

Elsender, Daniel & Bate, Matthew R., 2024, Monthly Notices of the Royal Astronomical Society 

The files contain the data and plotting scripts required to make the figures. Some files contain smoothed particle hydrodynamics (SPH) dump files, within these files are the SPLASH (Price 2007) config files that were used to produce the figures in the paper. 

The SPH dump files are Fortran binary files written in big endian format and generated by the sphNG code (Benz 1990; Bate 1995; Whitehouse & Bate 2004; Price & Monaghan 2007). They can be read, visualised, and manipulated using the free, publicly available SPLASH visualisation code (which reads sphNG dump files), written by Daniel J. Price, that can be downloaded from: 

http://users.monash.edu.au/~dprice/splash/ 

Files are as follows:

fig_1: Used for plotting the results of the dustywave tests. Contains 4 sub folders; k_1, k_10, k_100, k_1000, which refer to the drag coefficients. Each sub folder has 2 SPH dump files, VD- and VG-, along with 3 SPLASH config files. VD- contains information to plot the dust quantities, and VG- contains information to plot the gas quantities

fig_2: Used to plot the results of the dustyshock test. Contains 1 SPH dump and 2 SPLASH configs.

fig_3_4: Used to plot maximum densities in 4 different protostellar collapse calculations. Within this file is a python script (central_dens.py) and two sub folders: non-rotating and B008. Within these sub folders are dust-as-mixture and dust-as-particles, these refer to the two different dust evolution methods used. Within each of these folders there are 6 folders, one for each dust grain species, containing a text file 'dustmass.txt'. The 'dustmass.txt' files have three columns: time, gas density, and dust density.

fig_5: Contains SPH dump files used to plot snapshots of three of the dust-as-mixture calculations, grain sizes 1, 30, 100 microns. The SPLASH config files are in the top level of this folder with the SPH dump files within sub folders 1mu, 30mu, and 100mu.

fig_6: The same as fig_5 except to plot snapshots from some of the dust-as-particles calculations, with grain sizes 1, 30, and 100 microns. 

fig_7: Used to plot a radial dust density profile from 4 dust-as-mixture calculations; 2 calcultions use the implicit method described in the paper, and 2 use an explicit timestepping method. In the top level of the folder is the python script profile.py that will recreate the figure. The data used to make the plots are in files beginning QD-, radius is in units of [cm] and density in units of [g cm^(-3)]. 

fig_8: Contains data used to plot snapshots from 2 planet in disc calculations that employ either the implicit method from the paper or an explicit method. The SPLASH configs are in the top level of the folder and the explicit and implicit data files are in sub folders named as such. Each folder contains the 4 SPH dumps used in the paper.

fig_9: 3 text files and 1 python script. The text files contain 3 colunms: time [yrs], dust mass and gas mass [solar masses]. The files correspond to calculations of discs with embedded planets using different implementations of dust. The data from implicit method described in the paper is in dustmass_imp.txt, for the explicit version of this calculation in dustmass.txt, and in an explicit calculation with a different dust formulation (described in the paper) dustmass_old.txt

fig_10: Contains, in sub folders implicit and explicit, SPH dumps files for the results of the dust settle test after 20 orbits and the SPLASH config files to set the plot up. 

fig_11: Two sub folders, explicit and implicit, each containing the SPH dump file needed to plot the cross section of the disc. The SPLASH config files are set up to take a cross section of the disc.