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10 results for “AGB stars”
Three-component modelling of O-rich AGB star winds I. Effects of drift using forsterite – dataset
<p>The data provided here include all parameter files, log files, and a set of the<br> binary output files that are the basis for the publication in A&A.</p> <p>The file 'file_listing.txt' contains a complete list of files and directories<br> in all gzipped tar files. Each individual gzipped tar file is formatted as<br> follows:</p> <p> Mm.m_Ll.ll_Ttttt.tar.gz</p> <p>where<br> m.m :: the assumed mass of the model, in solar masses<br> l.ll :: The assumed luminosity, in log10(solar luminosities)<br> tttt :: The effective temperature of the star, in Kelvin.</p> <p><br> The contents of the tar files vary according to the model, but here is the<br> general directory structure:</p> <p> nodr/ :: non-drift / PC models<br> drift/ :: drift models</p> <p> nodr/init<br> drift/init :: Initial model files created using John Connor.</p> <p><br> File suffixes are the following:</p> <p> .par :: Plain-text parameter file that contains all parameters that are<br> different from the respective default value in the model.<br> Consequently, to see what parameters were actually used, it is<br> necessary to look in the log file (see below).</p> <p> .bin :: Binary file that contains output of converged models. Each model is<br> stored in two versions, first the previous time step and then the<br> current time step (having access to the model code T-800, data of both<br> time steps are needed to restart model calculations at that time<br> step).</p> <p> The initial model file only contains one model; where the previous<br> time step data are the same as the current time step data.</p> <p> We provide a tool to read this file, see below.</p> <p> Note! These files can get pretty large and are therefore only<br> available for a smaller number of the models in the Zenodo dataset.<br> Please ask the corresponding author for the missing files is the<br> need should appear.</p> <p> .log :: Plain-text log file that shows the used model parameters and a number<br> of key properties for each converged model.<br> The encoding of this file is UTF-8.</p> <p> .inf :: Plain-text secondary log file that contains the header of the<br> [primary] log file as well as timing information.<br> The encoding of this file is UTF-8.</p> <p> .tpb :: Secondary binary file that contains a number of properties specified<br> at the outer boundary, typically for each consecutive time step.</p> <p> We provide a tool to read this file, see below.</p> <p> .lis :: Plain-text file with the iteration history. Unavailable here.</p> <p> .liv :: Plain-text file with values specified for a number of properties at<br> each gridpoint. Unavailable here.</p> <p> .inp :: Plain-text file that is used to launch a model; some are present.<br> This file is automatically generated by the tool that launches T-800<br> and is typically removed when T-800 launches. Unavailable here.</p> <p> .eps :: Encapsulated PostScript file created by John Connor when calculating<br> the initial model.</p> <p><br> Model evolution structure - file endings before the suffix:</p> <p> _rlx :: Files related to relaxing the T-800 calculations on the initial model<br> created by John Connor.</p> <p> _exp :: Files related to expanding the initially compact model to using the<br> full radial domain.</p> <p> _fix :: Files related to the intermediate stage where calculations are changed<br> from expansion to outflow.<br> <br> _out :: Files related to the outflow stage of the calculations; this is what<br> you want to look at to see the wind evolution. Results in the paper<br> are calculated using these data.</p> <p> Note! Some outflow stage calculations continue the evolution of the previous<br> set of files. The underlying reason for continued calculations is typically<br> that the calculated time interval is too short. Such files are typically<br> given the extension '_cont.lin_out', '_cont2.lin_out', etc.</p> <p><br> Stored data in the binary files:</p> <p> The binary files (suffix '.bin') contain the full radial structure in the<br> following 10 (PC models) or 11 (drift models) primary variables:</p> <p> mr: radius<br> mm: integrated [gas] mass<br> md: gas density<br> mu: gas velocity<br> me: internal energy<br> mj: radiative energy<br> mh: radiative flux<br> n0: dust moment, forsterite (Fo)<br> nm: number density of magnesium atoms<br> ns: number density of silicon atoms<br> v0: dust velocity, forsterite (only drift models)</p> <p> Other properties are derived from these primary variables using auxiliary code<br> that isn't part of this dataset.</p> <p><br> Load files:</p> <p> Two tools are provided here that can load the binary data files using the<br> Interactive Data Language (IDL):</p> <p> sc_load_bin (for files with the suffix '.bin'):</p> <p> Loads the full content of a T-800 binary file and returns a structure<br> with the data.</p> <p><br> sc_load_tpb (for files with the suffix '.tpb'):</p> <p> Loads the full content of a T-800 'tpb' binary file and returns a<br> structure with the data.</p> <p> Note! Due to the way models run on clusters, this file is sometimes<br> incomplete; this happens when the model code T-800 is stopped as the<br> cluster-specific walltime is reached. If this is the case, it is<br> necessary to use the binary file instead, where data are saved<br> typically every 20:th time step.</p> <p> Alternative tools for use with Python and Julia could be considered for<br> writing, but where not yet available when this dataset was made public.<br> Please contact the corresponding author for a current status on this issue.</p> <p> </p>
Three-component modelling of C-rich AGB-star winds V. – dataset
<p>The provided data include all parameter files, binary output files, and log<br> files that are the basis for the publication in MNRAS.</p> <p>The file 'file_listing.txt' contains a complete list of files and<br> directories in all gzipped tar files. Each individual gzipped tar file is<br> formatted as follows:</p> <p> Mm.m_Ll.ll_Ttttt_CtOc.cc.tar.gz</p> <p>where<br> m.m :: the assumed mass of the model, in solar masses<br> l.ll :: The assumed luminosity, in log10(solar luminosities)<br> tttt :: The effective temperature of the star, in Kelvin.<br> c.cc :: The carbon-to-oxygen excess, in log10(n_C/n_H-n_O/n_H)+12</p> <p><br> The contents vary according to the model, but here is the general directory<br> structure:</p> <p> nodr/ :: non-drift / PC models<br> drift/ :: drift models</p> <p> nodr/init<br> drift/init :: Initial model files created using John Connor.</p> <p><br> File suffixes are the following:</p> <p> .par :: Plain-text parameter file that contains all parameters that are<br> different from the respective default value in the model.<br> Consequently, to see all used parameters it is necessary to look in<br> the log file (see below).</p> <p> .bin :: Binary file that contains converged models. Each model is stored in<br> two versions, first the previous time step and then the current time<br> step (both are needed to restart model calculations at that time<br> step).</p> <p> The initial model file only contains one model; where the previous<br> time step data are the same as the current time step data.</p> <p> The format of this file is explained below.</p> <p> Note! These files can get pretty large and are therefore only<br> available for a smaller number of the models here. Please ask the<br> corresponding author for the missing files should the need appear.</p> <p> .log :: Plain-text log file that shows the used model parameters and a number<br> of key properties for each converged model. The encoding of this file<br> is UTF-8.</p> <p> .inf :: Plain-text secondary log file that contains the header of the<br> [primary] log file as well as timing information.</p> <p> .tpb :: Secondary binary file that contains a number of properties specified<br> at the outer boundary, typically for each consecutive time step.</p> <p> .lis :: Plain-text file with the iteration history. Available for some files.</p> <p> .liv :: Plain-text file with values specified for a number of properties at<br> each gridpoint. Available for a smaller number of files.</p> <p> .inp :: Plain-text file that is used to launch a model; some are still there.</p> <p> .eps :: Encapsulated PostScript files created by John Connor when calculating<br> the initial model.</p> <p><br> Model evolution structure - file endings before the suffix:</p> <p> _rlx :: Files related to relaxing the T-800 calculations on the initial model<br> created by John Connor.</p> <p> _exp :: Files related to expanding the initially compact model to using the<br> full radial domain.</p> <p> _fix :: Files related to the intermediate stage where calculations are changed<br> from expansion to outflow.<br> <br> _out :: Files related to the outflow stage of the calculations; this is what<br> you want to look at to see the wind evolution. Results in the paper<br> are calculated using these data.</p> <p> <br> Note! Some outflow stage calculations continue the evolution of the previous<br> set of files. The underlying reason for continued calculations is typically<br> that the calculated time interval is too short. Such files are typically<br> given the extension '_cont.lin_out', '_cont2.lin_out', etc.</p> <p><br> Load files:</p> <p> Two tools are provided here that can load the binary data files using the<br> Interactive Data Language (IDL):</p> <p> sc_load_bin (for files with the suffix '.bin'):</p> <p> Loads the full content of a T-800 binary file and returns a structure<br> with the data.</p> <p><br> sc_load_tpb (for files with the suffix '.tpb'):</p> <p> Loads the full content of a T-800 'tpb' binary file and returns a<br> structure with the data.</p> <p> Note! Due to the way models run on clusters, this file is sometimes<br> incomplete; this happens when the model code T-800 is stopped as the<br> cluster-specific walltime is reached. If this is the case, it is<br> necessary to use the binary file instead, where data are saved<br> typically every 20:th time step.</p> <p> Alternative tools for use with Python and Julia could be considered for<br> writing, but where not yet available when this dataset was made public.<br> Please contact the corresponding author for a current status on this issue.</p>
Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II: Spectroscopic Data of Thorne-Zytkow Object and Super-AGB Star Candidates
<p>This dataset contains Magellan MIKE spectroscopy of a population of cool, luminous stars in the Magellanic Clouds, a sample of confirmed Magellanic Cloud red supergiants, and spectrophotometric standard stars. The spectra were analyzed in the paper "Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II: Spectroscopic and Environmental Analysis of Thorne-\.Zytkow Object and Super-AGB Star Candidates" by O'Grady et al. (2022). More details are provided in the README. </p>
A WISE view of extreme AGB stars
<p>The files in this distribution are related to the paper:</p> <p>"A WISE view of extreme AGB stars", by M.A.T. Groenewegen published in Astronomy & Astrophysics 659, A145 (2022).<br> </p>
The C-flame Quenching by Convective Boundary Mixing in Super-AGB Stars and the Formation of Hybrid C/O/Ne White Dwarfs and SN Progenitors
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2013ApJ...772...37D/abstract">Denissenkov et al. (2013)</a>. MESA version 4631.</p> <p>Publication DOI: <a href="https://doi.org/10.1088/0004-637X/772/1/37">10.1088/0004-637X/772/1/37</a></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>
The VMC Survey - XXXVII. Pulsation periods of dust enshrouded AGB stars in the Magellanic Clouds
<p>FigA1.tar and FigC2.tar contain postscript files of the 1299 light curves and 254 spectral energy distributions, respectively, as described in the paper.</p>
Correlations between the abundances of Barium stars, the AGB model residuals and the delta parameter
<p>Additional figures for Világos et al. 2024, Sect. 3.2. For the sample of Barium stars, correlations between the observationally dervied abundances; the residuals between the AGB models and the abundances; and the delta parameter.</p> <p>The figures are divided into the following directories:</p> <ul> <li>'1-obs_feh': Abundances and elemental ratios of different peaks as a function of the [Fe/H] (Sect. 3.2.1 and Fig. 5).</li> <li>'2-res_feh': Residuals of the abundances and elemental ratios as a function of the [Fe/H] (Sect. 3.2.2 and Fig. 6).</li> <li>'3-obs_obs': Abundances as a function of the other abundances (Sect. 3.2.3 and Fig. 7).</li> <li>'4-res_res': Residuals of the abundances as a function of the other residuals (Sect. 3.2.4 and Fig. 8).</li> <li>'5-res_obs': Residuals of the abundances as a function of the abundances (see Sect. 3.2.5 and Fig. 9).</li> <li>'6-delta': Abundances and residuals as a function of the delta parameter, that indicates the fraction of AGB material in the Ba star envelope (Sect. 3.2.6 and Fig. 10).</li> </ul> <p>For figures in directories 1-2, we refer to some elements as [A/B], although sometimes [B/A] vs. [Fe/H] is shown. Visually, this swapping of the numerator and denominator elements means a vertical reflection around the y = 0 axis. Thus, $r_S$ and $a$ for [B/A] vs. [Fe/H] have the same absolute value but different sign than for [A/B] vs. [Fe/H].</p> <p>For figures in directories 3-5, if we refer to [A/Fe] vs [B/Fe], but plot [B/Fe] vs [A/Fe], the sign of the relationship (correlation or anti-correlation) remains the same. The swap of the two axes results in a reflection around a diagonal line with a slope of 1. The resulting slope is therefore $1/a$, while $r_S$ is the same in both cases.</p>
DEATHSTAR - Nearby AGB stars with the Atacama Compact Array
<p>Low- and intermediate-mass stars develop slow and massive stellar winds when they reach the end of their lives. Investigating the mass-loss phenomenon on the asymptotic giant branch (AGB) is crucial in gaining a better understanding of late stellar evolution, as well as of the galactic chemical evolution, as AGB stars contribute significantly to the enrichment of the interstellar medium. DEATHSTAR is a large project aimed at improving the accuracy of stellar wind-parameter measurements. Constraining the size of the CO-emitting circumstellar envelope is the first step of the project, by mapping the envelopes in CO J=2–1 and 3–2 lines with the Atacama Compact Array (ACA). The first published DEATHSTAR sample consists of 69 nearby (<1 kpc) AGB stars of the three chemical types. In this video, I present the results from our initial analysis and the current status of the DEATHSTAR project.</p>
Supplementary material for "Millimetre observations of the S-type AGB star χ Cygni: variability of the emission of the inner envelope"
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