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32 results for “stars: rotation”
Axisymmetric models for neutron star merger remnants with realistic thermal and rotational profiles: dataset
<p>Dataset containing the results of the parameter space exploration of binary neutron star merger remnants and 12 selected models:<br> * `search_results.dat` contains the parameters and properties of the successful results of the study.<br> * `model_*.log` are the logs with settings, parameters, and properties of the selected models.<br> * `model_*.out` are the profiles of the selected models in binary format.<br> * `XNS_reader.py` is a python script to read the binary format, convert it to text, and compute some derived and global quantities. EDIT 2022-05-30: the output file in binary format does contain the profiles of temperature and entropy per baryon, but those are not outputted in the converted text file. You can manually modify the python script in order to output these profiles too.<br> * `properties.csv` is a summary of the parameters and properties of the selected models.<br> <br> This dataset has been obtained with the stationary code XNS in General Relativity with the Conformal Flatness Approximation [Bucciantini and Del Zanna 2011; Pili et al. 2014; Camelio et al. 2018 and 2019].<br> The EOS is implemented as a cold piecewise polytrope [Read et al. 2009] plus a thermal gamma law.<br> The models have been selected between those obtained in the parameter space exploration.<br> For details see the companion paper [Camelio et al. 2021, PRD 103:063014].<br> <br> If you use this dataset, please cite its Zenodo DOI and the companion paper [Camelio et al. 2021, PRD 103:063014].</p> <p>EDIT 2022-05-30: an updated version of the code that has been used to produce this dataset is now on Zenodo (https://doi.org/10.5281/zenodo.6594069).<br> This updated version is called ASWNS code, and it does not contain the model of binary neutron star merger remnant used for this dataset, but an older version of the model of nonbarotropic neutron star (from Camelio et al. 2019).<br> You can implement any neutron star model on top of ASWNS, as shown in the examples provided with ASWNS.</p>
Non-linear three-mode coupling of gravity modes in rotating slowly pulsating B stars: Stationary solutions and modeling potential
<p>This repository contains the material available online that accompanies <a href="https://arxiv.org/abs/2311.02972" target="_blank" rel="noopener">Van Beeck et al. (2024)</a> (ArXiv link). </p> <p>It contains zipped archives that contain inlists and final data products for the MESA stellar evolution code\(^1\) (version 15140), the GYRE stellar pulsation/oscillation code\(^2\) (version 6.0.1) and the AESolver stellar oscillation mode coupling code\(^3\).</p> <p>In the technical information section below you may find a description of the contents of this repository. The abstract of <a href="https://arxiv.org/abs/2311.02972" target="_blank" rel="noopener">Van Beeck et al. (2024)</a> is also available below.</p> <p> </p> <p><em>Footnotes :</em></p> <p><em>\(^1\): see <a href="https://docs.mesastar.org/en/r15140/" target="_blank" rel="noopener">https://docs.mesastar.org/en/r15140/</a> for additional details about the MESA stellar evolution code.</em></p> <p><em>\(^2\): see <a href="https://gyre.readthedocs.io/en/v6.0.1/">https://gyre.readthedocs.io/en/v6.0.1/</a> for additional details about the GYRE stellar pulsation/oscillation code.</em></p> <p><em>\(^3\): the AESolver code can be downloaded from its Github repository: <a href="https://github.com/JVB11/AESolver" target="_blank" rel="noopener">https://github.com/JVB11/AESolver</a>; its documentation may be consulted at <a href="https://jvb11.github.io/AESolver/" target="_blank" rel="noopener">https://jvb11.github.io/AESolver/</a>.</em></p>
Reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - II. Implementation of magnetic braking in MESA and implications for the evolution of surface rotation in OB stars "
<p>This is a reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution - II. Implementation of magnetic braking in MESA and implications for the evolution of surface rotation in OB stars" by Keszthelyi et al. (2020), https://doi.org/10.1093/mnras/staa237</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>
Data products from "oMEGACat II - Photometry and proper motions for 1.4 million stars in Omega Centauri and its rotation in the plane of the sky"
<p>This repository contains the data products of the publication:<br><a href="https://ui.adsabs.harvard.edu/abs/2024arXiv240403722H/abstract"> Häberle et al (2024): "oMEGACat II - Photometry and proper motions for 1.4 million stars in Omega Centauri and its rotation in the plane of the sky"</a></p> <p>A detailed description of the data products and their creation is given in the accompanying paper.</p> <p>The data products include:</p> <ul> <li>The astrometric catalog with position and proper motion information for around 1.4 million sources within the half-light radius of Omega Centauri. We provide the catalog in both the .fits and .mrt format.</li> <li>The 7 photometric catalogs (for the 7 different used Hubble Space Telescope filters), both in .fits and .mrt format.</li> <li>The 7 deep, stacked image mosaics (one for each filter) in .fits format</li> <li>In addition, we include an IPython Notebook with basic usage examples for all these files.</li> </ul> <p>Please cite the catalog paper <a href="https://ui.adsabs.harvard.edu/abs/2024arXiv240403722H/abstract">Häberle et al. (2024)</a> when using this work.</p> <p>In case of any questions, feel free to contact us using <a href="mailto:haeberle@mpia.de">haeberle@mpia.de</a></p> <p> </p> <p> </p>
General relativistic self-gravitating equilibrium disks around rotating neutron stars: dataset
<p><strong>Dataset containing the results from <em>arXiv:2406.00945 (Y.Kim et al. 2024)</em></strong></p> <ul> <li>`model_list.asc` contains the name of the model (can be looked up from the Table 4 in the manuscript) and basic information.</li> </ul> <p>All equilibrium solutions are generated with (N_s x N_mu) = (801 x 401) resolution. See section 3.4 of the manuscript.</p> <ul> <li>`radial_grid.dat` contains the radial grid in the unit of the neutron star coordinate radius. A zero value at the end of the file corresponds to the endpoint (infinity) of the radial grid, which can be ignored.</li> <li>Angular grid is simply a uniformly divided interval of `mu = cos (theta)`, which can be easily generated and is not included in this dataset. Note that the angle `theta` is measured from the polar axis (z) toward the equatorial plane.</li> </ul> <p>Main data files (`<model_name>_<quantity_name>.dat`) include a flattened 2D array of the four metric functions, rest mass density, and the angular velocity of the fluid. They all contain a single long column of numbers, and can be opened with normal text editors or loaded with other packages (e.g. numpy) without difficulty. Data value at a grid point (mu_i, r_j) is located as a (801 * i + j)th entry with zero-based indexing. For example, the first 801 numbers correspond to the data on the equator (mu=0), then a radial profile along `mu=1/400`, then `mu=2/400`, and so on.</p> <ul> <li>The metric function `rho` and `gamma` correspond to `nu - beta` and `nu + beta` (see Eq 8-9 of Komatsu+1989: https://ui.adsabs.harvard.edu/abs/1989MNRAS.237..355K/abstract).</li> <li>Other metric functions `alpha` and `omega` have the same definition.</li> <li>`restenergydensity` is the rest energy density, and `angvel` is the coordinate angular velocity (see Eq 5 of the manuscript) of the fluid.</li> <li>Neutron star (r<=r_e) is modeled with K=100, Gamma=2 polytropic EoS, where the disk is modeled with K=0.468, Gamma=4/3 polytropic EoS. See the section 4 of the paper.</li> </ul> <p> </p> <p>If you use this dataset, please cite the Zenodo DOI and the companion manuscript <em>Y.Kim et al. 2024 (arXiv:2406.00945).</em></p>
MOBSTER: Identifying Candidate Magnetic O Stars through Rotational Modulation of TESS Photometry
<p>O-type stars display rotational modulation of their photometric brightness due to surface features induced by fossil magnetic fields, and possibly through dynamos driven by subsurface convection. These features introduce wind perturbations that may drive large-scale structures and flows, including magnetospheres and corotating interaction regions. Until recently there has been a lack of high-precision, high-cadence photometry of O stars capable of detecting this variability. The wealth of new observations provided by the Transiting Exoplanet Survey Satellite (TESS) offers an unparalleled opportunity to conduct comprehensive studies of O-star variability at the sub-mmag level. Using the Galactic O-Stars Catalogue (GOSC) we have identified a sample of confirmed Galactic O stars observed by TESS with existing high-resolution spectroscopy from the IACOB and OWN surveys. Frequency analysis of the photometry is preceded by a careful examination of potential blending sources. Existing spectroscopy of each candidate is employed to test the rotational modulation hypothesis. In this presentation we describe the preliminary results of our study and outline plans for future analysis.</p>
Catalog of Cool Host Stars with Established Rotation Periods
<p>Catalog of 249 late K- and M-type exoplanet host stars with rotation periods obtained from the literature or new analysis of space- or ground-based time-series photometry as of August 2022. Model-based, metallicity-dependent corrections are provided but not included in gyrochronological age estimates. Please cite the reference paper if any information from this table is used. Table 1 in Gaidos et al. 2023, in press, in CDS format.</p>
Dataset for 'Rotational dependence of turbulent transport coefficients in global convective dynamo simulations of solar-like stars'
<p>For moderate and slow rotation, magnetic activity of solar-like stars is observed to strongly depend on rotation, while for rapid rotation, only a very weak or no dependency is detected. These observations do not yet have a solid explanation in terms of dynamo theory. To work towards such an explanation, we numerically investigated the rotational dependency of dynamo drivers in solar-like stars, that is, stars that have a convective envelope of similar thickness as in the Sun. We ran semi-global convection simulations of stars with rotation rates from 0 to 30 times the solar value, corresponding to Coriolis numbers, Co, of 0 to 110. We measured the turbulent transport coefficients describing the magnetic field evolution with the help of the test-field method, and compared with the dynamo effect arising from the differential rotation, self-consistently generated in the models. The trace of the <strong><span class="math-tex">\(\alpha\)</span></strong> tensor increases for moderate rotation rates with Co<sup>0.5</sup> and levels off for rapid rotation. This behavior is in agreement with the kinetic <span class="math-tex">\(\alpha\)</span> based on the kinetic helicity, if one takes into account the decrease of the convective scale with increasing rotation. The <strong><span class="math-tex">\(\alpha\)</span></strong> tensor becomes highly anisotropic for Co > 1, <span class="math-tex">\(\alpha_{rr}\)</span> dominates for moderate rotation (1<Co<10), and <span class="math-tex">\(\alpha_{\phi\phi}\)</span> for rapid rotation (Co > 10). The effective meridional flow, taking into account the turbulent pumping effects, is markedly different from the actual meridional circulation profile. Hence, the turbulent pumping effect is dominating the meridional transport of the magnetic field. Taking all dynamo effects into account, we find three distinct regimes. For slow rotation, the <span class="math-tex">\(\alpha\)</span> and Rädler effects are dominating in presence of anti-solar differential rotation. For moderate rotation, <span class="math-tex">\(\alpha\)</span> and <span class="math-tex">\(\Omega\)</span> effects are dominant, indicative of <span class="math-tex">\(\alpha\Omega\)</span> or <span class="math-tex">\(\alpha^2\Omega\)</span> dynamos in operation, producing equatorward-migrating dynamo waves with the qualitatively solar-like rotation profile. For rapid rotation, an <span class="math-tex">\(\alpha^2\)</span> mechanism, with an influence from the Rädler effect, appears to be the most probable driver of the dynamo. Our study reveals the presence of a large variety of dynamo effects beyond the classical <span class="math-tex">\(\alpha\Omega\)</span> mechanism, which need to be investigated further to fully understand the dynamos of solar-like stars. The highly anisotropic <strong><span class="math-tex">\(\alpha\)</span></strong> tensor might be the primary reason for the change of axisymmetric to non-axisymmetric dynamo solutions in the moderate rotation regime.</p> <p>For the full article see <a href="https://arxiv.org/abs/1910.06776">https://arxiv.org/abs/1910.06776</a></p>
Photometric Activity Cycles in fast-rotating stars: Revisiting the reality of stellar activity cycle branches
<p>The provided files comprise the tables and Activity cycle fits presented in our manuscript titled "Photometric Activity Cycles in fast-rotating Stars". The files are denoted as Table 1 (main-sequence stars), Table 2 (RS CVn candidates) and a folder containing activity cycle fits for all main-sequence and RSCVn candidates listed in the aforementioned tables. DOI: <a href="https://doi.org/10.1093/mnras/staf754" target="_blank" rel="noopener">10.1093/mnras/staf754</a> </p>
Accurate and Robust Stellar Rotation Periods catalog for 82771 Kepler stars using deep learning
<p>This repository is for the paper "Rotation Period for 83022 Kepler Stars: A Deep Learning Approach" by I. Kamai and H. B. Perets. It is associated with manuscript number AAS56501. It consists a frozen repository and the published catalog</p>
The Three-Dimensional Collapse Of A Rapidly Rotating 16 $M_{\odot}$ Star
<p>Data products from ApJL article The Three-Dimensional Collapse Of A Rapidly Rotating 16 $M_{\odot}$ Star, 2022. 3D rapidly rotating core-collapse supernova progenitor model at two different times. MESA inlist and model at time of mapping also included. All 3D data are in FLASH4 format using the HDF5 data structure. </p>
Population Models of Rotating Field Stars in Kepler
<p>Model populations are constructed using TRILEGAL galaxy models coupled to YREC stellar evolutionary models and a magnetic braking law, and are described in van Saders, Pinsonneault, & Barbieri, "Forward Modeling of the Kepler Stellar Rotation Period Distribution: Interpreting Periods from Mixed and Biased Stellar Populations," 2019, ApJ, 872, 128 and updated in Hall et al. 2021 (Nature Astronomy, 5, 707) to incorporate the Berger et al. 2020 (AJ, 159, 280) Kepler Stellar Properties Catalog. </p> <p>Two model populations are provided: one in which rotation is modeled with a "standard" magnetic braking law of the form in van Saders et al. 2013, and a second in which stars are subject to weakened magnetic braking past a critical Rossby number, Rocrit. </p> <p>Models can be unpacked with the hdf with pandas functionality, using key='sample'. The keys should be self-explanatory with the possible exception of "evo", which is the evolutionary state. Choose evo = 1 to select only the main sequence.</p> <p>If you use these models in your work, please cite van Saders et al. 2019, with an additional citation to Hall et al. 2021 appreciated. </p> <p> </p>
Asymmetric core collapse of rapidly rotating massive star
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.474.2419G/abstract">Gilkis (2018)</a>. MESA version 7624.</p> <p>Publication DOI: 10.1093/mnras/stx2934<a href="https://doi.org/10.1093/mnras/stx2934">10.1093/mnras/stx2934</a></p>
Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2013ApJS..208....4P">Modules for Experiments in Stellar Astrophysics (MESA): Planets, Oscillations, Rotation, and Massive Stars</a></p>
Yields from paper: ALUMINIUM-26 FROM MASSIVE BINARY STARS II. ROTATING SINGLE STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM
<p>Title: Aluminium-26 From Massive Binary Stars II: ROTATING SINGLE STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM<br> Authors: Brinkman H.E., den Hartogh J. W., Doherty C.L., Pignatari M., Lugaro M.<br> ================================================================================<br> Description of contents: A .tar.gz package containing three files with the complete set<br> of yields from the models presented in this paper. YieldsNR.txt contains the yields for the<br> non-rotating models and Yields150.txt and Yields300.txt the yields for the models<br> rotating at an initial velocity of 150 and 300 km/s, respectively.</p> <p>================================================================================</p>
3D MHD Simulations of Magnetospheres from Obliquely Rotating Magnetic Massive Stars
<p>We present results from the first 3D MHD simulations of the stellar-wind-fed magnetospheres from massive stars with a dipole magnetic axis that has an arbitrary obliquity angle (<span class="math-tex">\(\beta\)</span>) to the star’s rotation axis. As an initial direct application, we examine the global structure of co-rotating disks for tilt angles <span class="math-tex">\(\beta =\)</span> 0, 45 and 90 degrees using <span class="math-tex">\(\zeta\)</span> Pup stellar parameters as a prototype. We find that for models with rapid stellar rotation (~0.7 critical rotation), accumulation surfaces closely resemble the form predicted by the analytic Rigidly Rotating Magnetosphere (RRM) model, but with a mass distribution and outer disk termination set by centrifugal breakout processes. Moreover, models with low stellar rotation rates show a far more variable and complex structure than simple predictions. These models can be used to synthesize rotational modulation of photometric absorption and H-alpha emission for a direct comparison with observations.</p>
The Complicated Case of δ Scuti Pulsations and Rotation in KIC 6951642; a long-orbit Single-lined Spectroscopic Binary Star
<p>Abstract: More than four years of HERMES observations have confirmed KIC 6951642 is a very long orbit (≈1770 d) single-lined spectroscopic binary (F0-type) with a fast-rotating companion (vsin i = 123±3 Km/s). The Fourier spectrum of its four-year photometric observations includes plenty of significant frequencies (594) in low- and high-frequency regions. The high-frequency modes appear with various time-delay patterns. We detected several rotationally split 𝛿 Scuti pulsations centered at 13.96 per day (and average frequency spacing of Δ𝑓= 0.723±0.006 per day) for KIC 6951642. The detailed study of all significant low frequencies, extended from 0.72 to 3.60 per day, revealed that the two most dominant frequencies (with the same amplitude and larger than of p-modes) are a combina3on the lowest-frequency modes (𝑓<sub>3</sub> = 𝑓< 0.17 per day), i.e. 𝑓<sub>orhrm</sub> + 𝑚𝑓<sub>orhrm </sub>(𝑚 = 12,14). We suggest the lowest-frequency modes are very large harmonics (orders of 10) of orbital frequency (≈0.0006 per day). We verified the other most dominant low-frequencies as harmonics of rotation frequency 0.721 per day and its combinations. Finally, we reject the probability of hybrid pulsations in the fast-rotating companion of KIC 6951642. We introduce it as a 𝛿 Scuti pulsator with a candidate rotation frequency of 0.721 per day.</p>
Rotation Period Predictions for Low-mass Stars with Kinematic Information from Gaia DR3
<pre><strong>DR3_kine_prot_pred.csv:</strong> 17.6 million predicted periods for all stars with Gaia DR3 RVs. This data should only be used to vet periods and not directly as period measurements. Works best for stars with GBP-GRP > 1.5 and rotation period > 20 days. Do not work for fast-rotating low-mass stars. Column descriptions see below </pre> <p><strong>source_id</strong>: Gaia DR3 source_id</p> <p><strong>ra</strong>: Gaia DR3 ra measurements</p> <p><strong>dec</strong>: Gaia DR3 dec measurements</p> <p><strong>parallax</strong>: Gaia DR3 parallax measurements</p> <p><strong>bp_rp</strong>: Gaia DR3 G<sub>BP</sub>-G<sub>RP</sub> measurements</p> <p><strong>phot_g_mean_mag</strong>: Gaia DR3 G mag</p> <p><strong>abs_G</strong>: absolute Gaia G magnitude derived from Gaia DR3 G mag and parallax</p> <p><strong>ruwe</strong>: Gaia DR3 ruwe measurements </p> <p><strong>Prot_pred</strong>: Predicted periods using Gaia DR3 parameters and kinematics</p> <p> </p> <p><strong>vet_ztf_lowmass.csv</strong>: 65k vetted ZTF period measurements for stars with G<sub>BP</sub>-G<sub>RP</sub> > 1.5. Column descriptions see below</p> <p><strong>source_id</strong>: Gaia DR3 source_id</p> <p><strong>ra</strong>: Gaia DR3 ra measurements</p> <p><strong>dec</strong>: Gaia DR3 dec measurements</p> <p><strong>parallax</strong>: Gaia DR3 parallax measurements</p> <p><strong>bp_rp</strong>: Gaia DR3 G<sub>BP</sub>-G<sub>RP</sub> measurements</p> <p><strong>gmag</strong>: Gaia DR3 G mag</p> <p><strong>abs_G</strong>: absolute Gaia G magnitude derived from Gaia DR3 G mag and parallax</p> <p><strong>rv</strong>: Gaia DR3 rv measurements</p> <p><strong>Prot</strong>: measured and vetted periods from ZTF </p>
Phase plots for the sample of super-slowly rotating Ap (ssrAp) stars from the Zwicky Transient Facility survey
<p>This figure (B.1) is supplementary material to the paper "A new sample of super-slowly rotating Ap (ssrAp) stars from the Zwicky Transient Facility survey" by S. Huemmerich, K. Bernhard and E. Paunzen that has been accepted at Astronomy & Astrophysics (A&A). It shows the light curves of all sample stars, phased with the periods derived in our study (cf. Table A.1) and indicated in the plots. Red and blue symbols correspond to Zwicky Transient Facility (ZTF) <em>r</em> and <em>g</em> band data, respectively. For clarity, <em>g</em> band data have been shifted by varying amounts in the phase plots.</p>
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