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7 results for “stellar evolution tracks”
The SPOTS Models: A Grid of Theoretical Stellar Evolution Tracks and Isochrones For Testing The Effects of Starspots on Structure and Colors
<p><strong>The SPOTS Models: A Grid of Theoretical Stellar Evolution Tracks and Isochrones For Testing The Effects of Starspots on Structure and Colors</strong></p> <p>This repository contains the Stellar Parameters of Tracks with Starspots (SPOTS) grid of theoretical stellar evolutionary tracks and isochrones, presented in Somers, Pinsonneault, and Cao (2020, in prep). Our models were calculated with the Yale Rotating Evolution Code (e.g. van Saders & Pinsonneault, 2013, ApJ 776, 67), including updated which incorporate a treatment of surface starspots (Somers & Pinsonneault, 2015, ApJ 807, 174S). Modelling details can be found in these references. The purpose of this evolutionary suite is to provide the community with state-of-the-art predictions for the influence of starspots and magnetic activity on the structure of stars.</p> <p>The grid includes both isochrones and tracks. They can be downloaded individually from this repository, or in bulk by downloading the .zip files.</p> <p><strong>Isochrones (.isoc):</strong></p> <p>Each isochrone file contains a series of isochrones (stellar properties for a range of masses at fixed age) for ages between 1 Myrs and 4 Gyrs. Each file contains these isochrones for a different surface starspot covering fraction, given by the name of the file -- f000.isoc = 0% covering fraction, f017.isoc = 17% covering fraction, etc. Each isochrone contains several columns with different information, including,</p> <ol> <li>Fundamental properties: mass, age, luminosity, radius, logg, Teff, convective overturn timescale (TauCZ), lithium abundance relative to initial (Li/Li0).</li> <li>Starspot properties: Covering fraction (Fspot), ratio of spot temperature to ambient temperature (Xspot), the temperatures of hot and cool regions (T_hot, T_cool).</li> <li>Two-temperature colors, including Johnson BV, Cousins RI, 2MASS JHK, WISE W1, and Gaia G, BP, RP.</li> </ol> <p>Colors that fell outside of the calibrated range are listed as -99.0.</p> <p><strong>Tracks (.track):</strong></p> <p>We also include individual tracks for every combination of Fspot and Mass considered in the paper. Each .track file lists the mass and starspot covering fraction in the filename -- i.e. m055_f034.track is the model of mass 0.55Msun and with a 34% surface covering fraction. In addition to all the properties included in the isochrones, the track files also include:</p> <ol> <li>The total moment of interia of the model (total_I) and the moment of interia of the surface convection zone (CZ_I)</li> <li>The central and surface hydrogen abundances (X_cen, X_surf) and the surface metallicity (Z/X_surf)</li> <li>The deuterium abundance relative to initial (H2/H2_0)</li> </ol>
Stellar evolution tracks comparing turbulent pressure driven mass loss and the de Jager mass-loss rates
<p>The uploaded files provide a series of stellar evolution tracks with initial masses from 16 to 20 <span class="math-tex">\(M_\odot\)</span>. The two sets of tracks compare the evolution of stars evolved on the red supergiant branch with the Kee et al. turbulent pressure driven mass-loss rates to stars that instead use the de Jager mass-loss rates.</p>
Evolutionary tracks accompanying Stellar Evolution in Real Time II (1/4)
<p>Evolutionary tracks generated with MESA accompanying the project ``Stellar Evolution in Real Time II: R Hydrae and an Open-Source Grid of >3000 Seismic TP-AGB Models Computed with MESA'' ApJ, 2024</p> <p>Due to data volume, this is one of four Zenodo repositories associated to this project. The full list of related dataset DOIs is:</p> <ul> <li>https://doi.org/10.5281/zenodo.11280179</li> <li>https://doi.org/10.5281/zenodo.11282597</li> <li>https://doi.org/10.5281/zenodo.11353933</li> <li>https://doi.org/10.5281/zenodo.11357395</li> </ul> <p><strong>Details on archive files:</strong></p> <p>All phase 1 and phase 2 evolutionary tracks are contained in the files</p> <p>ZAMS_to_TCHeB_y-fixed.tar.gz<br>TCHeB_to_AGB_y-fixed.tar.gz<br>ZAMS_to_TCHeB_y-varied.tar.gz<br>TCHeB_to_AGB_y-varied.tar.gz</p> <p>sorted by whether a varied or static helium assumption was used.</p> <p>To use the smallest number of separate Zenodo listings possible, not all data are grouped in the same way.</p> <p>The tar.gz archive files labeled with a string of the form "AGB_to_end_M1.XX_y-fixed.tar.gz" include all models having a mass beginning with 1 (1.00, 1.10, 1.20, etc) and adopting the fixed helium assumption.</p> <p>Archive files labeled in the form "AGB_to_end_M1.XX_y-varied.tar.gz" include the same, but using the helium-varied assumption. </p> <p>Archive files labeled with a string of the form "AGB_to_end_M3.10_all.tar.gz" include both the fixed-helium and varied-helium tracks for all masses that start with 3 (3.00, 3.10, 3.20, etc).</p> <p> </p> <p><strong>Details on files unpacked from archives:</strong></p> <div>Every unpacked file has a name of the form </div> <div> </div> <div>history_m4.90_z0.0060_y0.261_eta0.01_yi-on_seismic_p3.data</div> <div> </div> <div>Anything that starts with "history" and ends with ".data" is an evolutionary track. Tracks that have "_p3" are the third phase: AGB to end (or failure of the model) and these files are large.</div> <div> </div> <div>Tracks that have "_p1" are the evolution from the zero-age main sequence (ZAMS) to the terminal age core helium burning (TCHeB). Tracks that have "_p2" evolve from TACHeB to the onset of the asymptotic giant branch (AGB).<br><br>In the file name, the two-decimal number after m, four-decimal number after z and 3-decimal number after y encode the evolutionary track's initial mass, initial metallicity (Z) and initial helium abundance (Y), respectively. In cases where there is no y value provided, the helium abundance is fixed as described in the paper. </div> <div> </div> <div>When the file name contains "yi-on" in the name, it means the helium-varied assumption was used. When the file contains "seismic" (should only be the case for p3's), it means the GYRE calculations are included in the output. </div>
Evolutionary tracks accompanying Stellar Evolution in Real Time II (4/4)
<p>Evolutionary tracks generated with MESA accompanying the project <br>``Stellar Evolution in Real Time II: R Hydrae and an Open-Source Grid of >3000 Seismic TP-AGB Models Computed with MESA'' ApJ 2024</p> <div> <div> <div> <p>Due to data volume, this is one of four Zenodo repositories associated to this project. The full list of related dataset DOIs is:</p> <ul> <li>https://doi.org/10.5281/zenodo.11280179</li> <li>https://doi.org/10.5281/zenodo.11282597</li> <li>https://doi.org/10.5281/zenodo.11353933</li> <li>https://doi.org/10.5281/zenodo.11357395</li> </ul> <p><strong>Details on archive files:</strong></p> <p>All phase 1 and phase 2 evolutionary tracks are contained in the files</p> <p>ZAMS_to_TCHeB_y-fixed.tar.gz<br>TCHeB_to_AGB_y-fixed.tar.gz<br>ZAMS_to_TCHeB_y-varied.tar.gz<br>TCHeB_to_AGB_y-varied.tar.gz</p> <p>sorted by whether a varied or static helium assumption was used.</p> <p>To use the smallest number of separate Zenodo listings possible, not all data are grouped in the same way.</p> <p>The tar.gz archive files labeled with a string of the form "AGB_to_end_M1.XX_y-fixed.tar.gz" include all models having a mass beginning with 1 (1.00, 1.10, 1.20, etc) and adopting the fixed helium assumption.</p> <p>Archive files labeled in the form "AGB_to_end_M1.XX_y-varied.tar.gz" include the same, but using the helium-varied assumption. </p> <p>Archive files labeled with a string of the form "AGB_to_end_M3.10_all.tar.gz" include both the fixed-helium and varied-helium tracks for all masses that start with 3 (3.00, 3.10, 3.20, etc).</p> <p> </p> <p><strong>Details on files unpacked from archives:</strong></p> <div>Every unpacked file has a name of the form </div> <div> </div> <div>history_m4.90_z0.0060_y0.261_eta0.01_yi-on_seismic_p3.data</div> <div> </div> <div>Anything that starts with "history" and ends with ".data" is an evolutionary track. Tracks that have "_p3" are the third phase: AGB to end (or failure of the model) and these files are large.</div> <div> </div> <div>Tracks that have "_p1" are the evolution from the zero-age main sequence (ZAMS) to the terminal age core helium burning (TCHeB). Tracks that have "_p2" evolve from TACHeB to the onset of the asymptotic giant branch (AGB).<br><br>In the file name, the two-decimal number after m, four-decimal number after z and 3-decimal number after y encode the evolutionary track's initial mass, initial metallicity (Z) and initial helium abundance (Y), respectively. In cases where there is no y value provided, the helium abundance is fixed as described in the paper. </div> <div> </div> <div>When the file name contains "yi-on" in the name, it means the helium-varied assumption was used. When the file contains "seismic" (should only be the case for p3's), it means the GYRE calculations are included in the output. </div> </div> <p> </p> </div> <p> </p> </div>
Evolutionary tracks accompanying Stellar Evolution in Real Time II (3/4)
<p>Evolutionary tracks generated with MESA accompanying the project <br>``Stellar Evolution in Real Time II: R Hydrae and an Open-Source Grid of >3000 Seismic TP-AGB Models Computed with MESA'' ApJ 2024</p> <div> <div> <p>Due to data volume, this is one of four Zenodo repositories associated to this project. The full list of related dataset DOIs is:</p> <ul> <li>https://doi.org/10.5281/zenodo.11280179</li> <li>https://doi.org/10.5281/zenodo.11282597</li> <li>https://doi.org/10.5281/zenodo.11353933</li> <li>https://doi.org/10.5281/zenodo.11357395</li> </ul> <p><strong>Details on archive files:</strong></p> <p>All phase 1 and phase 2 evolutionary tracks are contained in the files</p> <p>ZAMS_to_TCHeB_y-fixed.tar.gz<br>TCHeB_to_AGB_y-fixed.tar.gz<br>ZAMS_to_TCHeB_y-varied.tar.gz<br>TCHeB_to_AGB_y-varied.tar.gz</p> <p>sorted by whether a varied or static helium assumption was used.</p> <p>To use the smallest number of separate Zenodo listings possible, not all data are grouped in the same way.</p> <p>The tar.gz archive files labeled with a string of the form "AGB_to_end_M1.XX_y-fixed.tar.gz" include all models having a mass beginning with 1 (1.00, 1.10, 1.20, etc) and adopting the fixed helium assumption.</p> <p>Archive files labeled in the form "AGB_to_end_M1.XX_y-varied.tar.gz" include the same, but using the helium-varied assumption. </p> <p>Archive files labeled with a string of the form "AGB_to_end_M3.10_all.tar.gz" include both the fixed-helium and varied-helium tracks for all masses that start with 3 (3.00, 3.10, 3.20, etc).</p> <p> </p> <p><strong>Details on files unpacked from archives:</strong></p> <div>Every unpacked file has a name of the form </div> <div> </div> <div>history_m4.90_z0.0060_y0.261_eta0.01_yi-on_seismic_p3.data</div> <div> </div> <div>Anything that starts with "history" and ends with ".data" is an evolutionary track. Tracks that have "_p3" are the third phase: AGB to end (or failure of the model) and these files are large.</div> <div> </div> <div>Tracks that have "_p1" are the evolution from the zero-age main sequence (ZAMS) to the terminal age core helium burning (TCHeB). Tracks that have "_p2" evolve from TACHeB to the onset of the asymptotic giant branch (AGB).<br><br>In the file name, the two-decimal number after m, four-decimal number after z and 3-decimal number after y encode the evolutionary track's initial mass, initial metallicity (Z) and initial helium abundance (Y), respectively. In cases where there is no y value provided, the helium abundance is fixed as described in the paper. </div> <div> </div> <div>When the file name contains "yi-on" in the name, it means the helium-varied assumption was used. When the file contains "seismic" (should only be the case for p3's), it means the GYRE calculations are included in the output. </div> </div> <p> </p> </div>
Evolutionary tracks accompanying Stellar Evolution in Real Time II (2/4)
<p>Evolutionary tracks generated with MESA accompanying the project <br>``Stellar Evolution in Real Time II: R Hydrae and an Open-Source Grid of >3000 Seismic TP-AGB Models Computed with MESA'' ApJ 2024</p> <div> <p>Due to data volume, this is one of four Zenodo repositories associated to this project. The full list of related dataset DOIs is:</p> <ul> <li>https://doi.org/10.5281/zenodo.11280179</li> <li>https://doi.org/10.5281/zenodo.11282597</li> <li>https://doi.org/10.5281/zenodo.11353933</li> <li>https://doi.org/10.5281/zenodo.11357395</li> </ul> <p><strong>Details on archive files:</strong></p> <p>All phase 1 and phase 2 evolutionary tracks are contained in the files</p> <p>ZAMS_to_TCHeB_y-fixed.tar.gz<br>TCHeB_to_AGB_y-fixed.tar.gz<br>ZAMS_to_TCHeB_y-varied.tar.gz<br>TCHeB_to_AGB_y-varied.tar.gz</p> <p>sorted by whether a varied or static helium assumption was used.</p> <p>To use the smallest number of separate Zenodo listings possible, not all data are grouped in the same way.</p> <p>The tar.gz archive files labeled with a string of the form "AGB_to_end_M1.XX_y-fixed.tar.gz" include all models having a mass beginning with 1 (1.00, 1.10, 1.20, etc) and adopting the fixed helium assumption.</p> <p>Archive files labeled in the form "AGB_to_end_M1.XX_y-varied.tar.gz" include the same, but using the helium-varied assumption. </p> <p>Archive files labeled with a string of the form "AGB_to_end_M3.10_all.tar.gz" include both the fixed-helium and varied-helium tracks for all masses that start with 3 (3.00, 3.10, 3.20, etc).</p> <p> </p> <p><strong>Details on files unpacked from archives:</strong></p> <div>Every unpacked file has a name of the form </div> <div> </div> <div>history_m4.90_z0.0060_y0.261_eta0.01_yi-on_seismic_p3.data</div> <div> </div> <div>Anything that starts with "history" and ends with ".data" is an evolutionary track. Tracks that have "_p3" are the third phase: AGB to end (or failure of the model) and these files are large.</div> <div> </div> <div>Tracks that have "_p1" are the evolution from the zero-age main sequence (ZAMS) to the terminal age core helium burning (TCHeB). Tracks that have "_p2" evolve from TACHeB to the onset of the asymptotic giant branch (AGB).<br><br>In the file name, the two-decimal number after m, four-decimal number after z and 3-decimal number after y encode the evolutionary track's initial mass, initial metallicity (Z) and initial helium abundance (Y), respectively. In cases where there is no y value provided, the helium abundance is fixed as described in the paper. </div> <div> </div> <div>When the file name contains "yi-on" in the name, it means the helium-varied assumption was used. When the file contains "seismic" (should only be the case for p3's), it means the GYRE calculations are included in the output. </div> </div>
Stellar Tracks (i.e., MESA history files) used in the article "On Stellar Evolution In A Neutrino Hertzsprung-Russell Diagram"
<p>MESA history files (i.e. stellar tracks) for all masses in the article "On Stellar Evolution In A Neutrino Hertzsprung-Russell Diagram". Files have been compressed with xz. To decompress, xv --decompress filename.</p>
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