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264 results for “Stellarator”
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>
Circumnuclear Dust in Luminous Early-Type Galaxies -- I. Sample Properties and Stellar Luminosity Models
<p>This dataset contains the HST mosaic images created and described in the paper "Circumnuclear Dust in Luminous Early-Type Galaxies -- I. Sample Properties and Stellar Luminosity Models" by J. Davidson, B. Boizelle, J. Walsh, A. Barth, E. Rasmussen, A. Baker, D. Buote, J. Darling, L. Ho, K. Kabasares, and J. Cohn.</p> <p>Each mosaic was created by drizzling the data to a pixel scale of 0.08 and a pixel fraction of 0.75. The data are mostly in the infrared and optical and only occasionally in the ultraviolet.</p> <h2>Data Structure</h2> <p>These data are organized by target and each target has its own .zip file. Each .zip file is organized by HST camera, then by filter. For example, for the target Hydra A, the data are sorted into the following folders:</p> <ul> <li><strong>acs_sbc</strong> <ul> <li><strong>f140lp</strong></li> <li><strong>f150lp</strong></li> </ul> </li> <li><strong>acs_wfc</strong> <ul> <li><strong>f814w</strong></li> </ul> </li> <li><strong>wfc3</strong><br> <ul> <li><strong>f110w</strong></li> <li><strong>f160w</strong></li> <li><strong>f475w</strong></li> </ul> </li> <li><strong>aligned</strong></li> </ul> <p>The <strong>aligned</strong> folder for each target contains all the aligned mosaic images. These were aligned to their respective <em>wfc3/f160w</em> image using TweakReg, then further corrected using interpolation to obtain sub-pixel accuracy.</p> <h2>File Naming</h2> <p>All mosaic image files for all filters follow the same naming convention: <strong><target name + filter + pixel fraction + pixel scale>_ drz_sci.fits.</strong> For example, the Hydra A <em>f160w</em> mosaic is named <strong>hydraa_f160w_pxfr075_pxsc008_drz_sci.fits.</strong></p> <p>PSF files, both empirical and Tiny Tim (each drizzled to the same pixel scale and pixel fraction as the HST data), are included in each <strong>f110w</strong> and <strong>f160w</strong> folder and follow a similar naming convention. To these file names are added either *emp_psfdrz* for the empirical PSF or *psfdrz* for the Tiny Tim PSF. For example, the Hydra A <em>f160w</em> empirical PSF file is named <strong>hydraa_f160w_emp_psfdrz_pxfr075_pxsc008_drz_sci.fits,</strong> whereas the Tiny Tim PSF file is named <strong>hydraa_f160w_psfdrz_pxfr075_pxsc008_drz_sci.fits.</strong></p> <p>The <strong>f160w</strong> folders for all targets also contain a few extra files:</p> <ol> <li>Mask files, called <strong>f160w_mask.fits</strong> in all cases, which indicate the positions and extents of all extraneous sources of light (foreground stars, background galaxies, cosmic ray hits, etc.) in the respective <em>f160w</em> mosaics.</li> <li>A .txt file that contains the final GALFIT MGE solution and follows the naming convention <strong><target>_f160w_galfitmge_dustmask_tinytim_sol.txt.</strong> Note that the Tiny Tim PSF was used to obtain the final MGE solution in every case.</li> <li> A .fits file that contains the model based on the final GALFIT MGE solution. These follow the naming convention <strong><target>_f160w_pxfr075_pxs0080_drz_galfit_ttpsf_qbounds020.fits.</strong></li> <li><em>For NGC 3862 only</em>, we also obtained an MGE solution using the empirical PSF for comparison purposes. For this target, the .txt MGE solution that utilizes the empirical PSF is named <strong>ngc3862_f160w_galfitmge_dustmask_emp_sol.txt </strong>and the corresponding model .fits file is named <strong>ngc3862_f160w_pxfr075_pxs0080_drz_galfit_cenpsf_emppsf_qbounds020.fits.</strong></li> </ol> <p>For NGC 1387, NGC 3862, NGC 4261, and NGC 4435, a second round of observations were obtained using a subarray and shorter exposure times. The <strong>f110w</strong> and <strong>f160w</strong> folders for these galaxies therefore also have a few extra files that contain the drizzled images and empirical and Tiny Tim PSFs for these subarray exposures. These files follow the same naming conventions as previously described, with the addition of *subarr* to distinguish between the full array and subarray files. For example, the NGC 1387 drizzled subarray image is named <strong>ngc1387_f160w_subarr_pxfr075_pxsc008_drz_sci.fits, </strong>whereas the full-array, longer exposure time image is named <strong>ngc1387_f160w_pxfr075_pxsc008_drz_sci.fits. </strong>Please note that these subarray images were not used in any of the final MGEs or the analysis described in the paper, but are included here for sake of completeness.</p> <p>In the <strong>aligned </strong>folders, all aligned images follow the same naming convention: <strong><target>_<camera>_<filter>_pxfr075_pxsc008_drz_align_sci.fits.</strong></p>
FitteR for Accretion ProPErties of T Tauri stars (FRAPPE): A new approach to use Class III spectra to derive stellar and accretion properties (Additional Plots)
Open the record for dataset details and reuse information.
Data for J-PLUS: Beyond spectroscopy III. Stellar parameters and elemental-abundance ratios for five million stars from DR3
<p>The table contains stellar atmospehric parameters (Teff, logg, [Fe/H]), luminosity classification, element abundance ratios ([C/Fe], [Mg/Fe] and [alpha/Fe]), distance and age for over five million stars derived using J-PLUS DR3 + Gaia EDR3.</p><p>It includes the following parameters:</p><p>ra: Right Ascension from J-PLUS DR3 (J2000)</p><p>dec: Declination from J-PLUS DR3 (J2000)</p><p>gl: Galactic longitude derived from ICRS coordinates</p><p>gb: Galactic latitude derived from ICRS coordinates</p><p>mag[12]: Magnitudes of J-PLUS twelve bands (r, g, i, z, u, J0378, J0395, J0410, J0430, J0515, J0660, J0861)</p><p>err_mag[12]&Uncertainties of magnitudes of J-PLUS twelve bands (r, g, i, z, u, J0378, J0395, J0410, J0430, J0515, J0660, J0861)</p><p>gp1/rp1/ip1: Magnitudes from Pan-STARRS1</p><p>err_gp1/rp1/ip1: Uncertainties of magnitudes from Pan-STARRS1</p><p>G/BP/RP: Magnitudes for the Gaia three bands from EDR3; note G represents a calibration-corrected G magnitude</p><p>err_G/BP/RP: Uncertainties of magnitudes for the three Gaia bands from EDR3</p><p>ebv_sfd: Value of E(B - V) from the extinction map of SFD98, corrected for a 14% systematic</p><p>[Fe/H]: Photometric metallicity</p><p>err_[Fe/H]: Uncertainty of photometric metallicity</p><p>flg_[Fe/H]: Quality flag of [Fe/H]</p><p>[C/Fe]: Photometric carbon-to-iron abundance ratio</p><p>err_[C/Fe]:Uncertainty of photometric carbon-to-iron abundance ratio</p><p>flg_[C/Fe]: Quality flag of [C/Fe]</p><p>[Mg/Fe]: Photometric magnesium-to-iron abundance ratio</p><p>err_[Mg/Fe]: Uncertainty of photometric magnesium-to-iron abundance ratio</p><p>flg_[Mg/Fe]: Quality flag of [Mg/Fe]</p><p>[alpha/Fe]: Photometric alpha-to-iron abundance ratio</p><p>err_[alpha/Fe]: Uncertainty of photometric alpha-to-iron abundance ratio</p><p>flg_[alpha/Fe]: Quality flag of [alpha/Fe]</p><p>Teff: Effective temperature</p><p>err_Teff: Uncertainty of effective temperature</p><p>logg: Surface gravity</p><p>err_logg: Uncertainty of surface gravity</p><p>dist: Distance </p><p>err_dist: Uncertainty of distance</p><p>flg_dist: Flag to indicate the method used to derive distance, which takes the values ``parallax", ``CMF", and ``NO"</p><p>age: Stellar age</p><p>err_age: Uncertainty of stellar age</p><p>rv: Radial velocity</p><p>err_rv: Uncertainty of radial velocity</p><p>flg_rv: Flag to indicate the source of radial velocity, which takes the values ``GALAH", ``APOGEE'', ``Gaia",``RAVE", ``LAMOST", ``SEGUE"</p><p>parallax: Parallax from {it Gaia} EDR3</p><p>err_parallax: Uncertainty of parallax from {it Gaia} EDR3</p><p>pmra: Proper motion in Right Ascension direction from Gaia EDR3</p><p>err_pmra: Uncertainty of proper motion in Right Ascension direction from Gaia EDR3</p><p>pmdec: Proper motion in Declination direction from Gaia EDR3</p><p>err_pmdec&Uncertainty of proper motion in Declination direction from Gaia EDR3</p><p>ruwe: Renormalised unit weight error from Gaia EDR3</p><p>type: Flag to indicate classifications of stars, which takes the values ``dwarf" and ``giant" </p><p>subtype: Flag to indicate further sub-classifications of dwarf stars, which takes the values ``TO", ``MS" and ``Binary"</p>
Input files and data for paper "Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation"
<p>This entry contains input files to reproduce the results of the paper:</p> <p>Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation.</p> <p>Each zip archive corresponds to a section of the paper, and includes README files in ASCII format with a description. Raw output data and plotting tools are also provided for some of the results.</p>
The Compactness of Presupernova Stellar Cores
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2014ApJ...783...10S">The Compactness of Presupernova Stellar Cores</a></p>
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>
Data for Exploration of Stellar Variability in 20-second Cadence TESS Data
<p>This repository contains code, data, and plots related to "Exploration of Stellar Variability in 20-second Cadence TESS Data" by DeVane-Purgh et al. 2024, associated with the RNAAS manuscript number AAS5813. </p> <p>This repository contains the light curves created in this process, the code necessary to create them, the code used for analysis, and the plotting script used in the paper (Final Corrections and Plots_JT.ipynb) . It also includes some of the validation plots and so forth used to examine the lightcurves, and scripts to download the data directly from MAST. README.md explains the purpose of each file. </p> <p>For ease of use, it is possible to download either individual files, or the entire (zipped) archive tess_zenodo.zip</p>
QUASR: the QUAsisymmetric Stellarator Repository
<p>This is a dataset of approximately 370,000 vacuum field stellarators along with the electromagnetic coils that generate them. They are optimized for quasiaxisymmetry and quasihelical symmetry. The devices in the database are available in a couple of formats (SIMSOPT, VMEC) useful to the stellarator community. The most current version of the data set can be visualized at quasr.flatironinstitute.org</p> <p> </p> <p>=============</p> <p>Version history</p> <p>=============</p> <p>v4 (September 6, 2024): QH devices added.</p> <p>v3 (April 8, 2024): typo fixed.</p> <p>typo in uploads v1, v2: the 'total_coil_length' and 'coil_length_per_hp' keys in dataframe should read 'total_coil_length_threshold' and ''coil_length_threshold_per_hp'', i.e., the maximum allowable coil length and maximum allowable coil length per half period, respectively.</p> <p>v2 (January 29, 2024): additional QA devices added. </p> <p>v1 (October 29, 2023): initial upload. </p>
Stellar reddening map from DESI imaging and spectroscopy
<p>Data for reproducing figures in "Stellar reddening map from DESI imaging and spectroscopy" by Rongpu Zhou et al. 2024.</p>
The proper way to spatially decompose the gravitational-wave origin in stellar collapse simulations
<p>This data release contains a jupyter notebook and data that are necessary to reproduce all the figures in the corresponding paper at https://arxiv.org/abs/2405.09729. The readme file explain the nature of the files. You can contact the author for futher information.</p>
Stellar Parameter Estimation for Half a Million LAMOST M Dwarfs based on Cycle-StarNet
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The Data For Spatial Variations of Stellar Elemental Abundances in FIRE Simulations of Milky Way-Mass Galaxies: Patterns Today Mostly Reflect Those at Formation
<p>Spatial patterns of stellar elemental abundances encode rich information about a galaxy’s formation<br>history. We analyze the radial, vertical, and azimuthal variations of metals in stars, both today and at<br>formation, in the FIRE-2 cosmological simulations of Milky Way-mass galaxies, and we compare<br>with the Milky Way. Overall, spatial variations of stellar metallicities show only modest differences between formation and today; spatial variations today primarily reflect the conditions of stars at birth, with spatial redistribution of stars after birth contributing secondarily. </p> <p> </p> <p>This data abides by CC-BY.</p>
Supporting data for "Magnetic Archaeology of Early-Type Stellar Dynamos"
<p>Supporting data for "Magnetic Archaeology of Early-Type Stellar Dynamos". The `run_grid.sh` script runs a grid of models generated by copying and modifying entries in the `template` folder. The various python scripts provide a way of generating the figures in our manuscript.</p>
Inlists for paper: Stellar response after stripping as a model for common-envelope outcomes
<p>MESA (r11554) inlists for the models shown the "Stellar response after stripping as a model for common-envelope outcomes" paper (2107.14526). The inlists reproduce both the pre-stripped and stripped stellar models.</p> <p>Contents:</p> <p>strippedStars_MESA_inlists.zip</p> <ul> <li>single_star_evolution<br> - inlist_project<br> - run_star_extras.f</li> <li>stripped_star<br> - inlist_project<br> - run_star_extras.f</li> </ul>
MOBSTER - At the crossroads of stellar astrophysics in the upper HR Diagram
<p>Contrarily to low-mass stars, in which dynamo-generated surface magnetism is essentially ubiquitous, only about 10% of stars with radiative envelopes (O, B and A) exhibit detectable magnetic fields at their surfaces. Yet, this small magnetic subpopulation includes potential progenitors of exotic astronomical objects, such as high-mass stellar black holes (even at solar metallicity) and magnetars. Therefore, there is a strong motivation to learn more about the as-yet misunderstood formation of these stars, and what is currently lacking is a robust statistical basis to interpret their properties. In this talk, I will briefly review massive star magnetism and some of the critical gaps in knowledge that currently plague their study. I will then discuss the observational limitations that prevent us from learning more, and argue that all-sky broadband photometric missions such as the Transiting Exoplanet Survey Satellite (TESS) offer a valuable indirect method of addressing these limitations. Finally, I will present the MOBSTER (Magnetic OB[A] Stars with TESS: probing their Evolutionary and Rotational properties) collaboration, and highlight some of its early results, as well as offer a glimpse of the road that lies ahead.</p>
Detecting sub-stellar companions using the stellar pulsation timing method
<p>Video introduction to the poster <a href="http://wwwuser.gwdg.de/~felix.mackebrandt/plato21/">Detecting sub-stellar companions using the stellar pulsation timing method</a></p>
The mass fallback rate in relativistic stellar tidal disruption events
<p>MESA inlist files for the paper "The mass fallback rate in relativistic stellar tidal disruption events". Versions 15140 of MESA and MESA SDK 20.3.1 were used for the simulations. More details are in the README.txt file and in the paper.</p>
Modules for Experiments in Stellar Astrophysics (MESA): Time-Dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure
<p>We update the capabilities of the open-knowledge software instrument Modules for Experiments in Stellar Astrophysics (MESA). The new auto_diff module implements automatic differentiation in MESA, an enabling capability that alleviates the need for hard-coded analytic expressions or finite difference approximations. We significantly enhance the treatment of the growth and decay of convection in MESA with a new model for time-dependent convection, which is particularly important during late-stage nuclear burning in massive stars and electron degenerate ignition events. We strengthen MESA's implementation of the equation of state, and we quantify continued improvements to energy accounting and solver accuracy through a discussion of different energy equation features and enhancements. To improve the modeling of stars in MESA we describe key updates to the treatment of stellar atmospheres, molecular opacities, Compton opacities, conductive opacities, element diffusion coefficients, and nuclear reaction rates. We introduce treatments of starspots, an important consideration for low-mass stars, and modifications for superadiabatic convection in radiation-dominated regions. We describe new approaches for increasing the efficiency of calculating monochromatic opacities and radiative levitation, and for increasing the efficiency of evolving the late stages of massive stars with a new operator split nuclear burning mode. We close by discussing major updates to MESA's software infrastructure that enhance source code development and community engagement.</p>
Constructing the space of quasisymmetric stellarators
<p>Data files for figures 5-7 in the paper "Constructing the space of quasisymmetric stellarators"</p>
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