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8 results for “stars: mass loss”
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>
Mass loss in main-sequence B stars
<p>MESA run_star_extras associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2014A&A...564A..70K">Krtička (2014)</a>. MESA version 7624.</p> <p>Publication DOI: <a href="https://doi.org/10.1051/0004-6361/201321980">10.1051/0004-6361/201321980</a></p>
Type IIP Supernovae IV. Shock Breakout from Progenitor Stars Modeled with Convective Overshoot and Mass Loss [Dataset]
<p>Input and output files of MESA and STELLA associated with the published journal article Balaji et al. (2022; doi:10.3847/1538-4357/ac7528). We used MESA version r-10398 and MESA SDK version 20180822.</p> <p>We employ two sets of mass loss schemes: a standard “Dutch” scheme and an “enhanced” episodic late mass loss scheme to construct circumstellar matter. Evolution of the enhanced mass loss models in MESA from the pre-main sequence stage through nuclear burning stages until just before core-collapse is contained in “pre-ccsn_enhanced_mass_loss.tar.xz”. The “MESA_inputs” folder contains all the inlist files and “run_star_extras.f”. “run_star_extras.f” is the same for all the enhanced mass loss models. The inlists for each of the different models can be easily obtained by editing the parameters: “initial_mass” in “inlist_cluster”, overshoot factors in “inlist_control” and the saved model names in “inlist_convert” and “inlist_star”. Each of the “#M_z0.0060_f_#_f0_0.005.tar.xz” directories, indicative of a model of particular ZAMS mass and overshoot parameter (f), contains “*.mod” files and a “LOGS” directory which in turn contains “history.data” files and the “profile#.data” file at core-collapse.</p> <p>Similar data files for the Dutch mass loss models are given in the Zenodo publication: <a href="https://doi.org/10.5281/zenodo.3783492">https://doi.org/10.5281/zenodo.3783492</a></p> <p>The “ccsn.tar.xz” folder contains input and output files from the core-collapse step executed in MESA, separately for the Dutch mass loss and enhanced mass loss models. The “MESA_inputs” folder contains all the inlist files where “run_star_extras.f” is the same for all the Dutch mass loss models and for all the enhanced mass loss models separately. The inlists for each of the different models can be obtained by editing “initial_mass” and “inject_until_reach_model_with_total_energy” in “inlist_edep”. Each of the “#M_z0.0060_f_#_f0_0.005_edep_#.tar.xz” directories, now, also indicative of the EDEP of explosion contains the “*.mod” files after every step, the “mesa.abn” and “mesa.hyd” files which initialise STELLA, and a LOGS directory which contains the “history.data” files after every step. </p> <p> The “STELLA.tar.xz” folder contains the output files and “stella_extras” from STELLA for each of the Dutch mass loss and Enhanced mass models separately in a “res” directory. For the Dutch mass loss, 12 solar mass, f = 0.025, EDEP = 1.0 FOE model which was studied extensively in our work, the “mesa.dat” file inside "/strad/run" of STELLA was modified to display profiles of radiation hydrodynamic variables (in “mesa.swd”) at earlier time instants than what is reported by STELLA, by default.</p> <p>The python code: "csm-profile-maker.py" constructs profiles of circumstellar matter from mass loss data from MESA which was then appended to the models before initialisation of STELLA.</p> <p>For more details on the methods of simulations, see section 4 of the published article. </p>
Shocking and Mass Loss of Compact Donor Stars in Type Ia Supernovae
<p>MESA inlists and output files, Athena++ input and output files and simulation movies for the paper "Shocking and Mass Loss of Compact Donor Stars in Type Ia Supernovae" . Uses MESA version 24.03.1, and MESA SDK version aarch64-macos-23.10.1. See README for details.</p>
X-Shooting ULLYSES: Massive Stars at low metallicity VI. Atmosphere and mass-loss properties of O-type giants in the SMC
<p>Figures from X-Shooting ULLYSES: Massive Stars at low metallicity VI. Atmosphere and mass-loss properties of O-type giants in the SMC. The individual fits of the stars and their explored parameter space. </p> <p>Caption:</p> <p>Overview of the fitting results of AV\,80. The \textit{top} part shows the line profiles included in the fitting process, with the name of each feature indicated in the bottom left. The green line shows the best fit, with the shaded region showing the 1$\sigma$ uncertainty on the model fit. The black vertical bars indicate the observed flux, with the length indicating the uncertainty. The horizontal axis shows the wavelength in \AA. The \textit{bottom} part shows the distribution of $1/\chi^2_{\rm r}$ for each parameter (indicated on the top left), with $\chi^2_{\rm r}$ the reduced $\chi^2$ value. Each scatter point indicates one {\sc Fastwind} model calculated by Kiwi-GA. The color indicates the generation in which the model was computed, with light gray the first generation and black the last. The vertical yellow line indicates the best fit value for each parameter, and the shaded regions are the 1 and 2 $\sigma$ confidence intervals. The distributions in the red shaded area are from the optical only GA fit.</p>
MESA inlists for "Coping with loss: Stability of mass transfer from post-main-sequence donor stars"
<p>Binary model inlists for MESA, as used for the paper <a href="https://ui.adsabs.harvard.edu/abs/2023A%26A...669A..45T/abstract">Coping with loss: Stability of mass transfer from post-main-sequence donor stars</a> . The inlists provided here are pared-down, minimal working examples of the ones used in the publication. Due to the nature of the calculations, it was often needed to fine-tune inlists for specific systems by hand. For example, AGB models typically required the additional setting of <em>use_gold_tolerances = .false.</em></p> <p>These binary calculations start from a previously-evolved single star model for the donor stars. These can be found in the compressed folder titled "sstar_models_CWL.tar.xz". Please note that several parameters in the inlists will need to be adjusted accordingly, such as the configuration (initial orbit; mass ratio) of the binaries.</p> <p> </p> <p><strong>NOTE:</strong> to ensure that the mass-transfer calculation is fully conservative, add the following line to the <em>binary_controls</em> namelist in the <em>inlist_project</em> file:</p> <blockquote> <p>use_radiation_corrected_transfer_rate = .false.</p> </blockquote> <p>Further advice, code and/or files are available upon reasonable request to the authors (<a href="mailto:Karel.Temmink@ru.nl">contact: Karel Temmink</a>).</p>
Pulsation-driven Mass Loss from Massive Stars behind Stellar Mergers in Metal-poor Dense Clusters
<p>MESA inlists, run_star_extras, and data associated with Nakauchi, Inayoshi, Omukai 2020. MESA version</p> <p>12115.</p>
Fit summary of "X-Shooting ULLYSES: Massive Stars at low metallicity IX: Empirical constraints on mass-loss rates and clumping parameters for OB supergiants in the Large Magellanic Cloud"
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