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96 results for “binary star”
Different to the core: the pre-supernova structures of massive single and binary-stripped stars
<p>This is a basic reproduction package for the paper "Different to the core: the pre-supernova structures of massive single and binary-stripped stars".</p> <p>This package contains inlists for MESA and processed output.</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>
Yields from paper: ALUMINIUM-26 FROM MASSIVE BINARY STARS III. BINARY STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM
<p>================================================================================<br> Title: Aluminium-26 From Massive Binary Stars III: BINARY STARS UP TO CORE-COLLAPSE AND THEIR IMPACT ON THE EARLY SOLAR SYSTEM<br> Authors: Brinkman H.E., Doherty C.L., Pignatari M., Pols, O. R., Lugaro M.<br> ================================================================================<br> Description of contents: A .tar.gz package containing 12 files with the complete set<br> of yields from the models presented in this paper. Each file contains one primary mass,<br> e.g., Yields10Msun contains the yields for the binary systems with a 10Msun primary.<br> The second line in each file has the periods.<br> ================================================================================</p>
Data from: A pulsar-helium star compact binary system formed by common envelope evolution
Open the record for dataset details and reuse information.
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis
<p>We release dynamical ejecta data from binary neutron star merger simulations. The outflows are extracted at a fixed coordinate sphere with radius 300 G/c^2 Msun (= 443 km). Only material unbound according to the geodesic criterion is considered to be part of the dynamical ejecta. See [1] for more details.</p> <p>Included data:</p> <ul> <li>`Table2.txt`: Table 2 of the paper in machine readable format</li> <li>`tabulated_nucsyn.h5`: nucleosynthesis yields from pre-computed parametrized trajectories. The first three indices of each dataset are Ye, entropy, and expansion timescale tau. For example `Y_final[iYe, ientr, itau, iiso]` gives the final abundance of isotope `iiso` with `A[iiso]` and `Z[iiso]` for a trajectory with initial Ye = `Ye[iYe]`, initial entropy `s[ientr]`, and expansion timescale `tau[itau]`.</li> <li>`tabulated_rho.h5`: gives the density at T = 6 GK corresponding to the Ye, entropy, and expansion timescale used in `tabulated_nucsyn.h5`.</li> <li>`[model].tar`: ejecta data for individual simulations. The naming convention is the same as in the paper.</li> </ul> <p>For each model we provide:</p> <ul> <li>`outflow.txt`: angle integrated outflow rate and cumulated ejecta mass. Data are given in units with Msun = G = c = 1 (eg, the conversion factor for time to seconds is 4.9258e-6).</li> <li>`hist_entropy.dat`: histogram of the ejecta as a function of the entropy (in kb)</li> <li>`hist_vinf.dat`: histogram of the ejecta as a function of the asymptotic velocity (in units of c)</li> <li>`hist_ye.dat`: histogram of the ejecta as a function of the electron fraction Ye.</li> <li>`profile.txt`: time integrated ejecta profiles as a function of the polar angle.</li> <li>`hist_vinf_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.</li> <li>`hist_ye_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.</li> <li>`hist_ye_entropy_tau.h5`: histograms of the ejecta as a function of Ye, entropy, and expansion timescale tau.</li> </ul> <p>Additionally we distribute:</p> <ul> <li>Initial data generated with LORENE and associated EOS tables.</li> <li>EOS tables used for the evolution</li> <li>Parameter file used for each simulation</li> </ul> <p>For the multidimensional histograms the indices are ordered as specified in the file name, ie the file `hist_ye_theta.h5` tabulates the ejecta mass as a function of Ye (first index) and polar angle theta (second index).</p> <p><br> [1] D. Radice, A. Perego, K. Hotokezaka, S. A. Fromm, S. Bernuzzi, and L. F. Roberts, <em>Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis</em>, <a href="https://dx.doi.org/10.3847/1538-4357/aaf054">ApJ 869:130 (2018)</a>, <a href="https://arxiv.org/abs/1809.11161">arXiv:1809.11161</a></p>
Reproduction package for the paper "A strongly changing accretion morphology during the outburst decay of the neutron star X-ray binary 4U 1608-52"
<p>This is a basic reproduction package for the paper "A strongly changing accretion morphology during the outburst decay of the neutron star X-ray binary 4U 1608-52" by J. van den Eijnden et al. (2020). It provides reduced data sets, simulation scripts, X-ray spectral fits, and plotting scripts to allow the reproduction of the work performed in this paper. It also lists software used and data archives containing the public observational data. </p> <p>An open access version of the paper can be found at <a href="https://arxiv.org/abs/2002.04003">https://arxiv.org/abs/2002.04003</a>.</p>
The evolution of massive binary stars
<p>Input files and data to reproduce the figures of the review paper "The Evolution of Massive Binary Stars".</p><p>Simulations shown in the paper were computed using the Modules for Experiments in Stellar Astrophysics code (MESA), with version r23.05.1 and compiled with the MESA SDK version x86_64-linux-22.6.1.</p><p>Figures were produced using the julia programming language version 1.9.2 together with Makie.jl. A Project.toml and Manifest.toml file are provided to reproduce the environment used to produce the figures.</p>
Light curves from Gaia for single stars reported as unresolved binary candidates
<p>Light curves corresponding to the <em>Gaia</em> passbands <em>RP</em> (red), <em>G</em> (green), and <em>BP</em> (blue) for single stars reported as unresolved binary candidates. Isolated outliers (represented by crosses) are photometric errors, not consistent with flares, automatically rejected by variability processing. </p>
Particle tracer and horizon data of equal-mass, binary neutron stars simulations
<p>We provide the particle tracer and black hole (BH) horizon data obtained from two binary neutron star (BNS) simulations performed with IllinoisGRMHD.</p> <p>The first dataset, MissingLink_gammalaw_particle_data.tar.bz2, contains data from a magnetized, equal-mass BNS simulation of the missing link initial data. The equation of state (EOS) used was a simple gamma-law with Gamma=2.</p> <p>The second dataset, Magnetized_equalmass_BNS_LS220_particle_data.tar.bz2, contains data from a magnetized, equal-mass BNS simulation that employs an advanced, tabulated EOS—LS220.</p> <p>Both simulations have gone through inspiral, merger, and the formation of a remnant hypermassive neutron star that eventually collapses to a BH.</p>
Astrometrically identified nearby binary stars
<p>22,699 astrometric binary candidates identified via Gaia astrometry from the <a href="https://ui.adsabs.harvard.edu/abs/2021A%26A...649A...6G/abstract">Gaia Catalog of Nearby Stars</a>.</p> <p>Details of the specific data products and how the sample was selected can be found in <a href="https://ui.adsabs.harvard.edu/abs/2022MNRAS.513.5270P/abstract">Penoyre, Belokurov & Evans 2022</a>, with a description of the specific data included here provided in Table 2.</p>
Observing Runs for Binary Neutron Star and Neutron Star-Black Hole mergers in the HLVK-Configuration during O4, using 20 million CBC injections (July 2024 edition)
<p>We have conducted a simulation of the HLVK configuration deployed during the ongoing O4 run. This project supports the training of kilonova regression with machine learning processes, requiring thousands of BNS to pass the threshold cutoff. Here we have 17,009 BNS passing the SNR threshold, along with 3,148 NSBH and 121,718 BBH, from 20 million CBCs injected. The upper-lower limit between NS and BH is 3 sun masses.</p> <p>However, due to size constraints, this repository contains only the simulation data and sky maps of BNS and NSBH detections that have passed the cutoff threshold. For the complete dataset, including BBH, please refer to <a href="../doi/10.5281/zenodo.12693652">https://zenodo.org/doi/10.5281/zenodo.12693652</a> .</p>
Simulating the onset of grazing envelope evolution of binary stars
<p>MESA files associated with <a href="https://ui.adsabs.harvard.edu/#abs/2017MNRAS.465L..54S/abstract">Simulating the onset of grazing envelope evolution of binary stars</a></p>
Black-hole neutron-star binary simulation SXS:BHNS:0009
Simulation of a black-hole neutron-star binary system evolved by the <a href="https://www.black-holes.org/code/SpEC.html">SpEC code</a>.
Black-hole neutron-star binary simulation SXS:BHNS:0010
Simulation of a black-hole neutron-star binary system evolved by the <a href="https://www.black-holes.org/code/SpEC.html">SpEC code</a>.
binary_c output files to reproduce "Massive runaway and walkaway stars"
<p>Raw binary_c output for the paper "<a href="https://ui.adsabs.harvard.edu/abs/2019A%26A...624A..66R/abstract">Massive runaway and walkaway stars: A study of the kinematical imprints of the physical processes governing the evolution and explosion of their binary progenitors</a>" by Renzo et al. <br><br>The tarball is ~21GB zipped, and unzips to >250Gb file with all the parameter variations.<br><br></p>
Parameter estimation catalogs for binary neutron star mergers detected with next-generation gravitational wave detectors
<div> <p>Next-generation gravitational wave (GW) observatories, such as the Einstein Telescope (ET) and the Cosmic Explorer, will provide access to the population of binary neutron star (BNS) mergers throughout cosmic history and yield precise parameter estimates. Here, we publish the results of a comprehensive study evaluating BNS merger detection prospects using the ET alone or in a network of current or next-generation detectors up to redshift equal to 1. We publicly release all the parameter estimation for 10 years of observations of BNSs in the form of catalogs. These catalogs are made available to the community for multi-messenger studies, multi-probe cosmology, and nuclear study to constrain the neutron star (NS) equation of state (EOS). They can be used to focus on specific events (for example golden events with high signal-to-noise ratio) or for statistical studies on the BNS populations. </p> <p>Our simulations assessed the perspectives for detecting the optical emission of BNS mergers in the era of next-generation detectors, considering how uncertainties in BNS population properties, NS mass distribution, and the EOS might affect the detection rate and parameter estimation. The study is published in <a href="https://arxiv.org/abs/2411.02342" target="_blank" rel="noopener">Loffredo, Hazra, Dupletsa, Branchesi et al. 2024</a> arXiv:2411.02342 (submitted to A&A).</p> </div> <h3>BNS merger rate</h3> <p>As shown in <a href="https://ui.adsabs.harvard.edu/abs/2021MNRAS.502.4877S/abstract" target="_blank" rel="noopener">Santoliquido et al. (2021)</a>, the common envelope ejection efficiency parameter, α, determines one of the main sources of uncertainty for the number of BNS mergers per year. In order to evaluate the impact of the uncertainties of the BNS merger rate normalization on our results, we generate two catalogues of BNS mergers assuming α to be either <strong>0.5</strong> or <strong>1.0</strong>. </p> <h3>NS mass distribution</h3> <p>We draw the component masses of the NS binaries, M_1 and M_2, from two different mass distributions: <strong>Gaussian</strong> and<br><strong>uniform</strong> mass distributions. The Gaussian distribution is centred at 1.33 M⊙ with a standard deviation of 0.09 M⊙. The uniform mass distribution ranges in [1.1 M⊙, M_max], where M_max depends on the selected EOS.</p> <h3>Equation of state (EOS)</h3> <p>Since the NS EOS affects both the GW and EM signals expected from BNS mergers, we consider<br>two different EOSs, namely the <strong>APR4</strong> and <strong>BLh</strong> microscopic EOSs.</p> <h3>Detector configuration</h3> <p>Given the two values of α (0.5 and 1.0), the two mass distributions (uniform and Gaussian), and the two EOSs (BLh and APR4), we have a total of 8 different population sets, which constitute our injections for the gravitational signal analysis. For each of these datasets, we consider the following GW detector configurations:</p> <ul> <li>ET in its triangular design of 10 km arms, located in Sardinia, alone and operating together with (<strong>ET_delta_10_cryo</strong>): <ul> <li>the current ground-based network LIGO-Hanford, LIGO-Livingston, Virgo, KAGRA, LIGO-India (<strong>LVKI</strong>) </li> <li>one L-shaped CE with 40 km arms, located in the USA (<strong>1CE</strong>)</li> <li>2 CEs, both with 40 km arms, one in the USA and one in Australia (<strong>2CE</strong>)</li> </ul> </li> <li>ET in its 2L-shaped interferometer configuration of 15 km arms misaligned at 45 deg (one located in Sardinia and the other in the Netherlands); we consider the same networks as above, using the 2L-configuration instead of the triangular one (<strong>ET_2L_15_cryo_45deg</strong>). </li> </ul> <p>We thus have eight different detector networks giving a total of 64 simulations available in this repository. </p> <h3>Catalog description</h3> <p>The parameter estimation of the injected GW signals by the various detector networks is obtained through the Fisher matrix software <strong>GWFish</strong> (<a href="https://ui.adsabs.harvard.edu/abs/2023A%26C....4200671D/abstract" target="_blank" rel="noopener">Dupletsa et al. 2023</a>). The Fisher analysis method approximates the likelihood with a multivariate Gaussian distribution. All the parameters [M_1, M_2, dL, ι, RA, DEC, Ψ, phase, tc, Λ_1, Λ_2] are considered for the Fisher matrix derivation. The uncertainties on parameters coming from the covariance matrix (the inverse of the Fisher matrix) are given at 1σ. We implement a duty cycle of 85% for each of the L-shaped detectors, and for each of the three nested detectors composing the triangle. </p> <ul> <li><strong>Signals_<em>{BNS_merger_rate}</em>_<em>{EOS}</em>_<em>{NS_mass_distribution}</em>_<em>{Detector_configuration}</em>.txt </strong>contains the parameters describing a GW event and the corresponding network signal-to-noise ratio (SNR) <ul> <li><strong>mass_1: </strong>primary mass of the binary in [Msol] (in detector frame) (M_1)</li> <li><strong>mass_2:</strong> secondary mass of the binary in [Msol] (in detector frame) (M_2)</li> <li><strong>luminosity_distance:</strong> the luminosity distance of the merger in [Mpc]</li> <li><strong>dec:</strong> declination angle in [rad]. It varies in [−𝜋/2,+𝜋/2]</li> <li><strong>ra:</strong> right ascension in [rad]. It varies in [0,2/𝑝𝑖]</li> <li><strong>theta_jn:</strong> the angle between the line of observation and the total angular momentum (orbital, spin and GR corrections) of the binary [rad] (it reduces to the so-called inclination angle or <strong>iota</strong> if the spin component is absent); it ranges in [0,𝜋]</li> <li><strong>psi:</strong> the polarization angle in [rad]; it ranges in [0,𝜋]</li> <li><strong>geocent_time:</strong> merger time as GPS time in [s]</li> <li><strong>phase:</strong> the initial phase of the merger in [rad]; it ranges in [0,2𝜋]</li> <li><strong>redshift: </strong>the redshift of the merger</li> <li><strong>lambda_1: </strong>dimensionless tidal polarizabilty of primary component</li> <li><strong>lambda_2:</strong> dimensionless tidal polarizabilty of secondary component</li> <li><strong>network_SNR:</strong> network SNR for a the given event</li> </ul> </li> <li><strong>Errors_<em>{BNS_merger_rate}</em>_<em>{EOS}</em>_<em>{NS_mass_distribution}</em>_<em>{Detector_configuration}</em>.txt </strong>contains the <div> <div>parameter errors for each event. The first column is <strong>network_SNR</strong>, the following columns repeat the injected parameters as above and the relative errors <strong>err_<em>{parameter}</em></strong><em>. </em>The last column is the error on sky localisation (<strong>err_sky_location</strong>) at 90% credible interval. </div> </div> </li> </ul> <h3>Further details </h3> <p>Further details on the assumptions we made to produce these catalogs can be found in <a href="https://arxiv.org/abs/2411.02342" target="_blank" rel="noopener">Loffredo et al. 2024</a>, while further details on GWFish can be found on <a href="https://colab.research.google.com/github/janosch314/GWFish/blob/main/gwfish_tutorial.ipynb" target="_blank" rel="noopener">this tutorial</a>. We also provide the jupyter notebook <strong>paper_plots.ipynb</strong>, to reproduce Figs. 10, 11, 13, D.1, D.5, D.6. </p>
Evolutionary Origins of Binary Neutron Star Mergers
<p>Input and data files required to reproduce Figures 1 and 2 from Gallegos-Garcia et al 2022, Evolutionary Origins of Binary Neutron Star Mergers.</p>
Nucleosynthesis of binary-stripped stars.
<p>The cosmic origin of the elements, the fundamental chemical building blocks of the Universe, is still uncertain. Binary interactions play a key role in the evolution of many massive stars, yet their impact on chemical yields is poorly understood. Using the MESA stellar evolution code we predict the chemical yields ejected in wind mass loss and the supernovae of single and binary-stripped stars. We do this with a large 162 isotope nuclear network at solar-metallicity. We find that binary-stripped stars are more effective producers of the elements than single stars, due to their increased mass loss and an increased chance to eject their envelopes during a supernova. This increased production by binaries varies across the periodic table, with \fluorine[] and \potassium[] being more significantly produced by binary-stripped stars than single stars. We find that the \carbon[12]/\carbon[13] could be used as an indicator of the conservativeness of mass transfer, as \carbon[13] is preferentially ejected during mass transfer while \carbon[12] is preferentially ejected during wind mass loss. We identify a number of gamma-ray emitting radioactive isotopes that may be used to help constrain progenitor and explosion models of core-collapse supernovae with next-generation gamma-ray detectors. For single stars we find \vanadium[44] and \manganese[52] are strong probes of the explosion model, while for binary-stripped stars it is \chromium[48]. Our findings highlight that binary-stripped stars are not equivalent to two single stars and that detailed stellar modelling is needed to predict their final nucleosynthetic yields.</p><p> </p><p>MESA version: 12115</p><p> </p><p>This dataset contains the inlists, output from MESA, scripts, and data tables used in this publication.</p><p> </p><p>The tables folder contains the chemical yields for all models, isotopes, and mass loss processes.</p><p> </p><p>Accepeted for publication in ApJ</p>
Effects of Rotationally Induced Mixing in Compact Binary Systems with Low-mass Secondaries and in Single Solar-type Stars
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2012ApJ...755...95C/abstract">Chatzopoulos et al. (2012)</a>. MESA version 3647.</p> <p>Publication DOI: <a href="https://www.doi.org/10.1088/0004-637X/755/2/95">10.1088/0004-637X/755/2/95</a></p>
Stellar properties of observed stars stripped in binaries in the Magellanic Clouds - Spectral Models
<p>This Zenodo repository is one of three Zenodo repositories related to the article "Stellar properties of observed stars stripped in binaries in the Magellanic Clouds" by Y. Götberg, M.R. Drout, A.P. Ji, J.H. Groh, B.A. Ludwig, P.A. Crowther, N. Smith, A. de Koter, and S.E. de Mink. In the article, we analyze the optical spectra of ten stars and measure their stellar properties using spectral fitting. This repository contains the full spectral model grid computed using the 1D non-LTE radiative transfer code CMFGEN (see Hillier & Miller 1998 and http://kookaburra.phyast.pitt.edu/hillier/web/CMFGEN.htm). The grid spans three parameters: temperature, surface gravity, and surface hydrogen mass fraction (which also sets the surface helium mass fraction; Y = 1 - X - Z). See Section 4.1 for more details. Below, we describe the content presented here in more detail:</p> <ul> <li><strong>0_ReadMe.txt</strong>: A text file where we describe some more details regarding the content.</li> <li><strong>S41_spectral_model_grid_parameters.txt (95 KB):</strong> A table containing relevant parameter information for each model in the spectral model grid presented in Section 4.1.</li> <li><strong>S41_spectra_spectral_model_grid.tar.gz (479MB)</strong>: A .tar.gz containing the spectral energy distributions and normalized spectra in a text file for each model. The full CMFGEN models are provided as well (see below). This .tar.gz becomes 3.2 GB when inflated.</li> <li>Complete CMFGEN models for the full spectral model grid. Because of the size of these models, we group them into tarballs with one surface hydrogen mass fraction and one effective temperature, labeled for example <strong>XHs0.01_T40000.tar.gz</strong> (that is, this tarball contains a set of models with different surface gravity). Each of these have a size of ~1-3GB and when inflated the total content is ~5GB, and each model has about 500MB.</li> </ul>
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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)
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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.