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.本数据集包含10组数据文件，用于复现发表于2024年《皇家天文学会月报》的期刊论文《Elsender, Daniel 与 Bate, Matthew R.》中的11幅配图。 这些文件包含生成所有配图所需的原始数据与绘图脚本。其中部分文件为平滑粒子流体动力学（Smoothed Particle Hydrodynamics, SPH）输出文件，这类文件内附带了用于生成论文配图的SPLASH（Price, 2007）配置文件。 本数据集所用的SPH输出文件为大端序Fortran二进制文件，由sphNG代码生成（Benz 1990; Bate 1995; Whitehouse & Bate 2004; Price & Monaghan 2007）。可通过由Daniel J. Price开发的免费开源可视化工具SPLASH读取、可视化与处理该类文件，该工具支持读取sphNG输出文件，下载地址为：http://users.monash.edu.au/~dprice/splash/ 文件详情如下： fig_1：用于绘制尘埃波测试结果。包含4个子目录：k_1、k_10、k_100、k_1000，分别对应不同阻力系数。每个子目录内包含2个SPH输出文件（VD-与VG-）以及3个SPLASH配置文件。其中VD-文件用于绘制尘埃物理量分布，VG-文件用于绘制气体物理量分布。 fig_2：用于绘制尘埃激波测试结果。包含1个SPH输出文件与2个SPLASH配置文件。 fig_3_4：用于绘制4组不同原恒星坍缩计算的最大密度分布。该目录内包含1个Python脚本（central_dens.py）以及2个子目录：non-rotating（无自转）与B008。两个子目录下分别设有dust-as-mixture（尘埃混合态处理）与dust-as-particles（尘埃粒子态处理）两个子目录，对应两种不同的尘埃演化方法。每个方法目录下包含6个尘埃颗粒种类子目录，每个子目录内均设有文本文件dustmass.txt。该文件包含三列数据：时间、气体密度与尘埃密度。 fig_5：包含用于绘制3组尘埃混合态计算结果快照的SPH输出文件，对应尘埃颗粒尺寸分别为1、30、100微米。SPLASH配置文件位于该目录顶层，SPH输出文件分别存放在子目录1mu、30mu与100mu中。 fig_6：与fig_5功能类似，用于绘制部分尘埃粒子态计算的结果快照，对应尘埃颗粒尺寸为1、30、100微米。 fig_7：用于绘制4组尘埃混合态计算的径向尘埃密度剖面。其中2组采用论文中提出的隐式方法，另外2组采用显式时间步进方法。该目录顶层设有Python脚本profile.py，可用于复现配图。绘图所用数据存放在以QD-开头的文件中，半径单位为[cm]，密度单位为[g cm^(-3)]。 fig_8：包含用于绘制两颗行星在原行星盘内演化计算结果快照的原始数据，分别采用论文中的隐式方法与显式时间步进方法。SPLASH配置文件位于该目录顶层，显式与隐式方法对应的数据集分别存放在以对应方法命名的子目录中。每个子目录内包含论文中使用的4个SPH输出文件。 fig_9：包含3个文本文件与1个Python脚本。文本文件均包含三列数据：时间[yrs]、尘埃质量与气体质量[太阳质量]。这些文件对应不同尘埃处理方法下的行星嵌入盘系统计算结果：采用论文中隐式方法的数据集存放在dustmass_imp.txt中，采用该计算显式版本的数据集存放在dustmass.txt中，采用另一种尘埃处理方案（论文中提及）的显式计算数据集存放在dustmass_old.txt中。 fig_10：包含子目录implicit（隐式）与explicit（显式），分别存放20个轨道周期后尘埃沉降测试结果的SPH输出文件，以及用于设置绘图的SPLASH配置文件。 fig_11：包含explicit（显式）与implicit（隐式）两个子目录，每个子目录内均包含用于绘制盘截面图所需的SPH输出文件。配套SPLASH配置文件已预设为可生成盘截面视图。