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2 results for “self-gravitating”
Datasets for "Dynamo effect in unstirred self-gravitating turbulence"
<pre>This directory contains an index.html file with links to the run directories with secondary data for Table I of the paper "Dynamo effect in unstirred self-gravitating turbulence" by Axel Brandenburg and Evangelia Ntormousi. If anything turns out to be incomplete, please email brandenb@nordita.org. </pre>
General relativistic self-gravitating equilibrium disks around rotating neutron stars: dataset
<p><strong>Dataset containing the results from <em>arXiv:2406.00945 (Y.Kim et al. 2024)</em></strong></p> <ul> <li>`model_list.asc` contains the name of the model (can be looked up from the Table 4 in the manuscript) and basic information.</li> </ul> <p>All equilibrium solutions are generated with (N_s x N_mu) = (801 x 401) resolution. See section 3.4 of the manuscript.</p> <ul> <li>`radial_grid.dat` contains the radial grid in the unit of the neutron star coordinate radius. A zero value at the end of the file corresponds to the endpoint (infinity) of the radial grid, which can be ignored.</li> <li>Angular grid is simply a uniformly divided interval of `mu = cos (theta)`, which can be easily generated and is not included in this dataset. Note that the angle `theta` is measured from the polar axis (z) toward the equatorial plane.</li> </ul> <p>Main data files (`<model_name>_<quantity_name>.dat`) include a flattened 2D array of the four metric functions, rest mass density, and the angular velocity of the fluid. They all contain a single long column of numbers, and can be opened with normal text editors or loaded with other packages (e.g. numpy) without difficulty. Data value at a grid point (mu_i, r_j) is located as a (801 * i + j)th entry with zero-based indexing. For example, the first 801 numbers correspond to the data on the equator (mu=0), then a radial profile along `mu=1/400`, then `mu=2/400`, and so on.</p> <ul> <li>The metric function `rho` and `gamma` correspond to `nu - beta` and `nu + beta` (see Eq 8-9 of Komatsu+1989: https://ui.adsabs.harvard.edu/abs/1989MNRAS.237..355K/abstract).</li> <li>Other metric functions `alpha` and `omega` have the same definition.</li> <li>`restenergydensity` is the rest energy density, and `angvel` is the coordinate angular velocity (see Eq 5 of the manuscript) of the fluid.</li> <li>Neutron star (r<=r_e) is modeled with K=100, Gamma=2 polytropic EoS, where the disk is modeled with K=0.468, Gamma=4/3 polytropic EoS. See the section 4 of the paper.</li> </ul> <p> </p> <p>If you use this dataset, please cite the Zenodo DOI and the companion manuscript <em>Y.Kim et al. 2024 (arXiv:2406.00945).</em></p>
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