galacticwinds/Catastrophic_Cooling_Superwinds_II_Data: Catastrophic-Cooling-Superwinds-II-Data.1.2
Galacticwinds/Catastrophic Cooling Superwinds II Data: Catastrophic-Cooling-Superwinds-II-Data.1.2 (Dataset published at Zenodo repository.)
DOI10.5281/zenodo.5099614Zenodo5099614MaRDI QIDQ6724197
Dataset published at Zenodo repository.
Author name not available (Why is that?)
Publication date: 14 July 2021
Catastrophic Cooling in Superwinds. II. Exploring the Parameter Space, Supplementary Material The files of the interactive figure (64 images) of Figure 2, the interactive animation (64 videos) of Figure 3, the interactive figure (192 images) of Figure 6, and the compressed (tar.gz) file of the 6machine-readable table files (a portion shown for guidance regarding its form and content in Table 3) are archived on Zenodo. Figure 2. From top to bottom: the interactive figure of the temperature and density profiles of the superwinds on a logarithmic scale. The different regions separated by dotted lines: (a) freely expanding wind, (b) shocked-wind, (c) shell, and (d) ambient medium. The adiabatic temperature and density profile for each model are shown by dashed lines. Figure 3. From top to bottom: the interactive animation of the temperature and density profiles of the superwinds on a logarithmic scale. The different regions separated by dotted lines: (a) freely expanding wind, (b) shocked-wind, (c) shell, and (d) ambient medium. The adiabatic temperature and density profile for each model are shown by dashed lines. Figure 6. Top Panels: The hydrogen temperature profiles (left panels) along with the adiabatic prediction (red dashed line) in the CPI case, and the line emissivities (right panels) of the superwind models on a logarithmic scale, from top to bottom, in the PIand CPI cases. Bottom Panels: The hydrogen density profiles (left panels) along with the adiabatic prediction (red dashed lines), and the ionic fractions (right panels) on a logarithmic scale for the PI and CPI cases. The start and end of the hot bubble (region b), the end of the shell (region c), and the Strmgren radius are shown by dotted, dashed, dash-dotted, and solid lines (gray color), respectively. Table 3. Integrated luminosities (unit in erg/s) from the different ionization models. Citation @article{Danehkar2021, author = {{Danehkar}, Ashkbiz and {Oey}, M.~S. and {Gray}, William~J.}, title = {Catastrophic Cooling in Superwinds. II. Exploring the Parameter Space}, journal = {ApJ}, volume = {921}, number = {1}, pages = {91}, year = {2021}, doi = {10.3847/1538-4357/ac1a76} } Learn More Website:https://superwinds.astro.lsa.umich.edu/ GitPage:https://galacticwinds.github.io/
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