galacticwinds/Catastrophic_Cooling_Superwinds_II_Data: Catastrophic-Cooling-Superwinds-II-Data.1.2

<p><a href="https://galacticwinds.github.io/Catastrophic_Cooling_Superwinds_II_Data/"><strong>Catastrophic Cooling in Superwinds. II. Exploring the Parameter Space, Supplementary Material</strong></a></p> <p>The files of the interactive figure (<em>64 images</em>) of <strong>Figure 2</strong>, the interactive animation (<em>64 videos</em>) of <strong>Figure 3</strong>, the interactive figure (<em>192 images</em>) of <strong>Figure 6</strong>, and the compressed (tar.gz) file of the <em>6&nbsp;machine-readable table files</em> (a portion shown for guidance regarding its form and content in <strong>Table 3</strong>) are archived on Zenodo.</p> <ul> <li><a href="https://galacticwinds.github.io/Catastrophic_Cooling_Superwinds_II_Data/figure2/"><strong>Figure 2</strong></a>. 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.</li> <li><a href="https://galacticwinds.github.io/Catastrophic_Cooling_Superwinds_II_Data/figure3/"><strong>Figure 3</strong></a>. 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.</li> <li><a href="https://galacticwinds.github.io/Catastrophic_Cooling_Superwinds_II_Data/figure6/"><strong>Figure 6</strong></a>. 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 PI&nbsp;and 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 Str&ouml;mgren radius are shown by dotted, dashed, dash-dotted, and solid lines (gray color), respectively.</li> <li><a href="https://galacticwinds.github.io/Catastrophic_Cooling_Superwinds_II_Data/table3/"><strong>Table 3</strong></a>. Integrated luminosities (unit in erg/s) from the different ionization models.</li> </ul> <p><strong>Citation</strong></p> <pre><code class="language-bash">@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} }</code></pre> <p><strong>Learn More</strong></p> <p>Website:&nbsp;<a href="https://superwinds.astro.lsa.umich.edu/">https://superwinds.astro.lsa.umich.edu/</a><br> GitPage:&nbsp;<a href="https://galacticwinds.github.io/">https://galacticwinds.github.io/</a></p>