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20 results for “Stellar evolution”
The Effects of Asymmetric Dark Matter on Stellar Evolution I: Spin-Dependent Scattering - Supporting Data
<p>Supporting code and data for the paper: </p> <p><em>The Effects of Asymmetric Dark Matter on Stellar Evolution I: Spin-Dependent Scattering</em></p> <p>Raen (2020)</p> <p><strong>Supporting code</strong> includes `run_star_extras.f`, inlist templates, and our dark matter module (to be used in conjunction with MESA: <a href="http://mesa.sourceforge.net/index.html">Modules for Experiments in Stellar Astrophysics</a>). The full source code used in the production of this paper is available at <a href="https://github.com/troyraen/DM-in-Stars/">github.com/troyraen/DM-in-Stars</a> in the Raen2020 branch. (The master branch is intended for use by those wishing to use our module to explore DM effects beyond the scope of this paper.) We used MESA version 12115, and MESA SDK version 20190830.</p> <p><strong>Model data</strong> includes MESA history and profile data for the models highlighted in the paper (<span class="math-tex">\(1.0\ \mathrm{M}_\odot\)</span> and <span class="math-tex">\(3.5\ \mathrm{M}_\odot\)</span> models with <span class="math-tex">\(\Gamma_B = 0\)</span> (no dark matter), <span class="math-tex">\(\Gamma_B = 10^4\)</span>, and <span class="math-tex">\(\Gamma_B = 10^6\)</span>). The specific inlists used to generate the models are also included. Additional data will be shared on reasonable request to the paper's corresponding author.</p>
Stellar Evolution Models from "Finding the Fuse: Prospects for the Detection and Characterization of Hydrogen-Rich Core-Collapse 5 Supernova Precursor Emission with the LSST"
<p>These data consist of all runs from the Modules for Experiments in Stellar Astrophysics (MESA; Paxton et al. 2011, 2013, 2015, 2018, 2019) code, used to construct radius priors for modeling supernova precursor emission in<em> <a href="https://arxiv.org/abs/2408.13314">Finding the Fuse: Prospects for the Detection and Characterization of Hydrogen-Rich Core-Collapse 5 Supernova Precursor Emission with the LSST</a></em> (Gagliano+2024, submitted). </p> <p>The contents of the data files are detailed in the file <strong>ReadmeMESA.txt</strong>. Additional detail concerning the simulations can be found in Section 2.2 of the linked publication. </p>
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>
Dartmouth Stellar Evolution Grids
<p>Dartmouth stellar model grids, used by the 'isochrones' python package (github.com/timothydmorton/isochrones). Update from previous grids; these now include WISE bands, ages < 1Gyr, and have coarser Fe/H sampling.</p>
A Study of Primordial Very Massive Star Evolution II: Stellar Rotation and Gamma-Ray Burst Progenitors
<p>Wind ejecta tables of rotating very massive stars from the paper:</p> <p><a href="https://iopscience.iop.org/article/10.3847/1538-4357/ad1185">A Study of Primordial Very Massive Star Evolution II: Stellar Rotation and Gamma-Ray Burst Progenitors</a></p>
All mixed up: investigating the impact of internal mixing on stellar evolution
<p>The main-sequence evolution of intermediate- and high-mass stars is driven by the mass of their convective core and the amount of hydrogen that can take part in the nuclear burning. Both of these quantities are controlled by physical mixing processes at work in the deep stellar interior. Due to computational limitations, the implementations of these 3D time-dependent processes into 1D stellar evolution codes are based on unconstrained time-independent free parameters which represent individual mixing efficiencies. Traditional observational methods relying on global stellar characteristics, such as the surface gravity and effective temperature, have limited capacity in constraining the efficiencies of these mixing efficiencies and their impact on stellar evolution. Here, we combine the highly precise interior modelling enabled by asteroseismology with the sub-percent level precision on fundamental stellar properties such as masses and radii dictated by eclipse modelling of binary systems to rigorously calibrate stellar evolution models. Relying on model-independent masses and radii allows us to investigate how the internal mixing process alter the convective core masses of intermediate and high-mass stars. We demonstrate that populations of pulsating stars, multiple systems, and multiple systems with pulsating components all indicate that stellar evolution models without enhanced mixing in the core-boundary layers predict under-massive convective cores. We compare our binary asteroseismic results with a growing sample of magnetic stars in eclipsing binaries to investigate the impact of a measurable magnetic field on internal mixing in stellar evolution models.</p>
The excess of cool supergiants from contemporary stellar evolution models defies the metallicity-independent Humphreys-Davidson limit
<p>Input files and simulation results for stellar evolution tracks computed for the paper "The excess of cool supergiants from contemporary stellar evolution models defies the metallicity-independent Humphreys-Davidson limit", as well as synthetic populations generated and catalogues of observed cool supergiants in the Magellanic Clouds used in the analysis. Version 10398 of MESA was used for the simulations. More details in the README.txt file and in the paper.</p>
Dartmouth stellar evolution models
<p>Dartmouth stellar evolution models 2012 version.</p> <p>HST_ACSWF.tgz<br> HST_WFPC2.tgz<br> PanSTARRS.tgz<br> SDSSugriz.tgz<br> UBVRIJHKsKp.tgz</p>
Daset from the paper "Compact object mergers: exploring uncertainties from stellar and binary evolution with SEVN"
<p>This repository contains the dataset produced by the population-synthesis code SEVN for the paper:<br> "Compact object mergers: exploring uncertainties from stellar and binary evolution with SEVN"</p> <p>In this paper, we exploit the SEVN code (publicly available at <a href="https://gitlab.com/sevncodes/sevn">https://gitlab.com/sevncodes/sevn</a>) to analyse the formation and properties of binary compact objects.</p> <p>The repository also includes the initial condistions used as input and the SEVN version used to run the simulations.</p> <p>#Content</p> <p>The repository contains the following folders:</p> <p>- data_from_simulations: the folder contains all the data produced by the simulations and used in the Iorio+22 paper<br> - InitialConditions: the folder contains all the intial conditions (and the code to generate them) that have been used for the Iorio+22 paper<br> - SEVN_iorio22: this folder contains the version of the SEVN code that has been used to run the simulations in the Iorio+22 paper</p> <p>Each folder contains a specific README with additional information</p> <p> </p> <p>#Contatcts</p> <p>giuliano.iorio.astro@gmail.com</p> <p> </p> <p> </p>
Dust formation and mass loss around intermediate-mass AGB stars with initial metallicity Zini ≤ 10-4 in the early Universe - I. Effect of surface opacity on stellar evolution and the dust-driven wind
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017MNRAS.466.1709T">Dust formation and mass loss around intermediate-mass AGB stars with initial metallicity Zini ≤ 10-4 in the early Universe - I. Effect of surface opacity on stellar evolution and the dust-driven wind</a></p>
Presupernova neutrinos: realistic emissivities from stellar evolution
<p>MESA inlists associated with <a href="http://Presupernova neutrinos: realistic emissivities from stellar evolution">Presupernova neutrinos: realistic emissivities from stellar evolution</a></p>
A calibration point for stellar evolution from massive star asteroseismology: supplementary dataset
<p>Dataset related to the article "A calibration point for stellar evolution from massive star asteroseismology" by Burssens et al. 2022 published in Nature Astronomy on the 22nd of June 2023. </p> <p>This dataset contains:</p> <p>1) The frequency list derived from the cycle 2 TESS data set of HD192575 in machine-readable format. Units are provided in the article. </p> <p>2) The MESA/GYRE inlists needed to reproduce models and figures. </p> <p>See the article for more detailed information.</p> <p> </p> <p> </p> <p> </p> <div> </div>
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>
Exploring Stellar Evolution Models of sdB Stars using MESA
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2015ApJ...806..178S">Exploring Stellar Evolution Models of sdB Stars using MESA</a></p>
Explaining the luminosity spread in young clusters: proto and pre-main sequence stellar evolution in a molecular cloud environment
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2018MNRAS.474.1176J">Jensen & Haugbølle (2018)</a>. MESA version 8845.</p> <p>Publication DOI: <a href="https://doi.org/10.1093/mnras/stx2844">10.1093/mnras/stx2844</a></p>
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>
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.