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38 results for “binary systems”
Data for "Dynamic of binary molecular systems – advantages and limitations of NMR relaxometry"
<p>Raw data for "Dynamic of binary molecular systems – advantages and limitations of NMR relaxometry". DOI of article: https://doi.org/10.1063/5.0188257</p>
A Catalogue of All Known Mass-Transferring Ultracompact Binary Systems
<p>Introduction: I present a catalogue that collects all known mass-transferring ultracompact binary systems in one place. This includes AM CVn-type binaries, helium-enriched CVs and a variety of other objects.</p> <p>The goal of this catalogue is to prevent the duplicated effort of multiple researchers searching for known systems through the literature. Where applicable, the catalogue includes orbital periods, measured masses, Gaia cross-matches, as well as important references for each system. The catalogue includes 'confirmed' systems (usually means an orbital period measurement and/or a spectrum) and 'candidates' (may be selected based on other properties such as outburst shape).</p> <p>For full details and references see the associated paper (accepted to A&A). Preprint at https://arxiv.org/abs/2505.10535</p> <p>See the catalogue itself in the file 'amcvn_catalogue.fits'.</p> <p>Up to date as of 2025-04-01.</p>
A highly magnetized environment in a pulsar binary system
<p>A highly magnetized environment in a pulsar binary system</p> <p><strong>Data availability:</strong></p> <ul> <li>IPV and DM, RM variations used for Fig 1 (Demo how to read the code and plot: plot_Fig1.py) <p>DM_Icut_60s_140114.txt, DM_Icut_60s_200621.txt, </p> <p>RM_140114_20s_rmfit.txt,RM_200621_20s_rmfit.txt, </p> <p>ILV_140114_20s.npy, ILV_200621_20s.npy</p> </li> <li>A full table of DM and RM variations (duplicated with the txt files, but with better readability): Li_DM_RM_Ter5A.xlsx</li> <li>Calibrated full stokes data with frequency information for Fig 2 (in psrfit format, can be read in with standard psrchive commands): VEGAS_Ter5A_200621_0001.zap.E2.calib.rot.f32</li> </ul> <p><strong>Code availability</strong></p> <ul> <li><em>The basic process of the raw data and DM, RM fitting:</em></li> </ul> <p>DSPSR (http://dspsr.sourceforge.net) PSRCHIVE (http://psrchive.sourceforge.net)</p> <ul> <li><em>Modeling and fitting:</em></li> </ul> <p>https://github.com/dongzili/Pol_prop_fitting</p> <p>NOTICE: If there are updated data due to new demands, the information or new URL will be posted in https://github.com/dongzili/Pol_prop_fitting</p>
Gaia DR3 detectability of unresolved binary systems
<p>This upload contains the necessary data to construct the selection of unresolved binary systems in Gaia DR3 based on RUWE.</p> <p>The tutorial showing how to work with these data can be found here: </p> <p>https://gaiaunlimited.readthedocs.io/en/latest/notebooks/dr3-unresolved-binaries.html</p> <p>The paper describing the data and methods is:</p> <h2>Gaia DR3 detectability of unresolved binary systems</h2> <div>Alfred Castro-Ginard, Zephyr Penoyre, Andrew R. Casey, Anthony G.A. Brown, Vasily Belokurov, Tristan Cantat-Gaudin, Ronald Drimmel, Morgan Fouesneau, Shourya Khanna, Evgeny P. Kurbatov, Adrian M. Price-Whelan, Hans-Walter Rix and Richard L. Smart</div> <div> </div> <div>https://ui.adsabs.harvard.edu/abs/2024arXiv240414127C/abstract</div>
Surrogate waveform model data for black hole binary systems computed in point-particle black hole perturbation theory
<p>This repository contains all publicly available surrogate data for gravitational waveforms produced within the point-particle black hole perturbation theory framework and calibrated to numerical relativity simulations performed with the Spectral Einstein Code (SpEC). </p> <p>Several surrogate models are currently available in this catalog:</p> <ol> <li><strong>BHPTNRSur2dq1e3</strong>, for aligned spin black hole binary systems with mass-ratios varying from 3 to 1000 and spins from −0.8≤χ1≤0.8 on the larger black hole. This surrogate model is trained on waveform data generated by point-particle black hole perturbation theory (ppBHPT) with calibration to numerical relativity (NR) data. The waveforms include all spin-weighted spherical harmonic modes up to ℓ=4 except the (4,1) and m=0 modes. Model details can be found in <a href="https://arxiv.org/abs/2407.18319">Rink et al. 2024</a>. This data file is used to evaluate the surrogate model with either stand-alone Python code hosted by the <a href="https://bhptoolkit.org/BHPTNRSurrogate/">Black Hole Perturbation Toolkit</a> (Jupyter notebook <a href="https://github.com/BlackHolePerturbationToolkit/BHPTNRSurrogate/blob/main/tutorials/BHPTNRSur2dq1e3.ipynb">tutorial</a>) or the GWSurrogate Python package, which can be found on <a href="https://pypi.python.org/pypi/gwsurrogate/">PyPI</a> or <a href="https://anaconda.org/conda-forge/gwsurrogate">conda-forge</a>.</li> <li><strong>BHPTNRSur1dq1e4</strong>, an updated version of the <strong>EMRISur1dq1e4 </strong>model described below. The updated version includes better calibration to NR, a smoother transition to plunge model, and more harmonic modes. Model details can be found in <a href="https://arxiv.org/abs/2204.01972">Islam et al. 2022</a>. This data file is used to evaluate the surrogate model with either stand-alone Python code hosted by the <a href="https://bhptoolkit.org/BHPTNRSurrogate/">Black Hole Perturbation Toolkit</a> (Jupyter notebook <a href="https://github.com/BlackHolePerturbationToolkit/BHPTNRSurrogate/tree/main/tutorials/BHPTNRSur1dq1e4">tutorial</a>) or the GWSurrogate Python package, which can be found on <a href="https://pypi.python.org/pypi/gwsurrogate/">PyPI</a> or <a href="https://anaconda.org/conda-forge/gwsurrogate">conda-forge</a>.</li> <li><strong>EMRISur1dq1e4</strong>, for non-spinning black hole binary systems with mass-ratios varying from 3 to 10000. This surrogate model is trained on waveform data generated by point-particle black hole perturbation theory (ppBHPT), with the total mass rescaling parameter tuned to NR simulations. Available modes are [(2,2), (2,1), (3,3), (3,2), (3,1), (4,4), (4,3), (4,2), (5,5), (5,4), (5,3)]. The m<0 modes are deduced from the m>0 modes. Model details can be found in <a href="https://arxiv.org/abs/1910.10473">Rifat et al. 2019</a>. This data file is used to evaluate the surrogate model with either stand-alone Python code hosted by the <a href="http://github.com/BlackHolePerturbationToolkit/EMRISurrogate">Black Hole Perturbation Toolkit</a> (Jupyter notebook <a href="https://github.com/BlackHolePerturbationToolkit/EMRISurrogate/blob/master/EMRISur1dq1e4.ipynb">tutorial</a>) or the GWSurrogate Python package (Jupyter notebook <a href="https://github.com/sxs-collaboration/gwsurrogate/blob/master/tutorial/notebooks/nonspinning_nr_emri.ipynb">tutorial</a>), which can be found on <a href="https://pypi.python.org/pypi/gwsurrogate/">PyPI</a>.</li> </ol>
On the binary origin of Be stars and the nature of exotic Be binary systems
<p>Despite the large impact of massive stars on their environment, important questions concerning their formation, evolution, and final explosions remain unanswered. One of them is the origin of the Be phenomenon, which occurs in ~20% of the early-type OB star. Observationally, Be stars are defined as B-type stars with Balmer line emission, indicative of a circumstellar decretion disk. While the presence of a disk is thought to strongly correlate with rapid rotation of the star, the processes that lead to such high rotation rates are still widely debated. One of the proposed mechanisms for the spin up of Be stars is mass and angular momentum transfer from an initially more massive companion in previous binary interactions. If merging is avoided, the mass donor is now a He-burning stripped star or a compact object. If this is the predominant channel for Be star formation, there are two important implications: first, there should be no Be + main sequence binaries on tight orbits; and second, Be stars should have a stripped star or a compact object as companion (unless the system has been disrupted). Here, we present observational evidence that the binary channel is predominant in Be star formation. We report on a lack of main-sequence companions to massive Be stars, and argue that the few known Be binaries are indeed exotic systems with stripped star or compact companions. We further present new analyses that shed light on the nature and evolutionary status of the two famous Be systems LB-1 and HR 6819 who have recently been reported to contain a black hole companion.</p>
KU Car, a young massive eclipsing binary system in NGC 3324
<p>Massive stars are needed engines in the galactic clockwork for the chemical evolution of the Galaxy and the energetic input to the ISM. These stars suffer endemic multiplicity, and thus, studies of the origin and evolution of massive stars is tied to the study of binaries. Therefore, eclipsing binary systems are indispensable objects because absolute parameters (e.g. masses, radii, etc.) can be derived combining the study and modeling of radial velocity and light curves. Such absolute parameters derived from direct observations help to test models about the structure and evolution of massive stars. In this talk, we are presenting an analysis of the light and radial velocity curves of the eclipsing binary system KU Car (P=2.96 d). This binary, composed by a B0.5-0.7 V primary and an unseen companion, shows a remarkable light-curve with a sharp and deep primary minimum and a shallow secondary minimum with strong "reflection effect". Using PHOEBE 2.1 code for modeling, we have derived absolute parameters for both stars proposed the evolutionary stage. This Algol-like system dominated by a young early-B type star, is located in the center of NGC 3324, a bubble-like star-forming region also known as "Gabriela Mistral" Nebula. The photometric analysis is based on multi-band observations obtained using LCOGTN telescopes, and data gathered from ASAS-3, ASAS-SN, TESS, and GDS projects spanning a period of about 18 years. Radial velocities were determined using spectroscopic observations obtained at LCO/duPont and ESO-LSO/2p2 telescopes in the framework of "OWN Survey" and "B-SUGOS" projects.</p>
Ups!... I did it again: unveiling the hidden companion in Upsilon Sagittarii, a unique binary system at a second mass transfer stage
<p>Input files and simulation results for stellar evolution tracks computed for the paper "Ups!... I did it again: unveiling the hidden companion in Upsilon Sagittarii, a unique binary system at a second mass transfer stage". Version 15140 of MESA was used for the simulations. More details in the README.txt file and in the paper.</p>
Orbital Stability of Circumstellar Planets in Binary Systems
<p>Tar archives of simulations for circumstellar planets orbiting a range of host binary stars, where the archives are delineated by the mutual inclination in the filename. Each file in the archive has the assumed mass ratio, mu, and binary eccentricity, e_bin, in the file name as a tuple (mu,e_bin). Tools in python to manipulate and plot the data are provided through a GitHub repository, https://github.com/saturnaxis/ThreeBody_Stability. Inside each file contains a comma delimited text file, where the columns are the initial semimajor axis ratio, the initial phase of the planet, the maximum planetary eccentricity attained over the simulation time, the minimum planetary eccentricity attained over the simulation time, and the collision/escape time. Collisions are defined as collisions with either star, where the escape is when the radial distance of the planet exceeds 200 AU.</p>
Tagged original datasets for 'Genetically Optimized Massively Parallel Binary Neural Networks for Intrusion Detection Systems'
<p>Tagged, non-formatted, original datasets used in 'Genetically Optimized Massively Parallel Binary Neural Networks for Intrusion Detection Systems', T. Murovič, A. Trost.</p> <p>Available from the original authors:</p> <p>1. <a href="https://www.unsw.adfa.edu.au/unsw-canberra-cyber/cybersecurity/ADFA-NB15-Datasets/">https://www.unsw.adfa.edu.au/unsw-canberra-cyber/cybersecurity/ADFA-NB15-Datasets/</a> (UNWS-NB15 dataset)</p> <p>2. <a href="https://www.unb.ca/cic/datasets/nsl.html">https://www.unb.ca/cic/datasets/nsl.html</a> (NSL-KDD dataset)</p>
Eclipsing binary systems with beta Cephei components. V1216 Sco
<p>A set of files for MESA 23.05.1 and GYRE 7.1, used to compute a grid of binary evolutionary tracks and stellar oscillation models used in the paper "Eclipsing binary systems with beta Cephei components. V1216 Sco".</p>
Dataset: High-accuracy simulations of highly spinning binary neutron star systems
<p><strong>Dataset for Gravitational Waveforms for the work of Dudi et al., "High-accuracy simulations of highly spinning binary neutron star systems"; arXiv: 2108.10429 </strong></p> <p> </p> <p><strong>The naming of the files: </strong>EOS_SpinSetup_NumberOfPoints_Mode.dat<br> EOS: SLy<br> SpinSetup: dd - down down; ud - up, down; uu037 -- up, up with dimensionless spin of 0.37; uu057 -- up, up with dimensionless spin of 0.57<br> NumberOfPoints: Points inside the finest level: 96, 144, 192, 240<br> Mode: Only 2,2-mode available <br> </p>
The cosmic carbon footprint of massive stars stripped in binary systems
<p># Structure</p> <p>## Overview</p> <p>The folder data/ contains the inlists and mod files used in this work. Intermediate data (like history or profile) files must be regenerated from the provided files.</p> <p>The folder plots/ contains a jupyter notebook set-up to remake all plots (assuming the data is saved in the data/ folder). There are also additional scripts and files needed to reproduce this work.</p> <p>The griffith.txt file is the data from https://ui.adsabs.harvard.edu/abs/2021arXiv210309837G/abstract and was accessed from https://github.com/giganano/VICE/blob/master/vice/yields/ccsne/S16/W18F/FeH0/v0/explosive/c.dat</p> <p><br> ## Data folders</p> <p>corehedep - Evolution from ZAMS to end of core helium burning<br> coreodep - Evolution from end of core helium burning to end of core oxygen burning<br> cc - Evolution from end of core oxygen burning up to core collapse<br> ccsn - Evolution from core collapse to shock breakout</p> <p>engmc - Tests variations in the injection energy and mass cut of ccsn explosions<br> spacetime - Test variations in space/time resolution of ccsn explosions<br> ccsn_t_m - Test variations in injection time and injection mass of ccsn explosions</p> <p>## Sub-folders</p> <p>corehedep/base - Base folder with inlists for this set of models<br> corehedep/binary - Contains a folder for each mass for the binary-stripped stars (11-45)<br> corehedep/single - Contains a folder for each mass for the single stars (11-45)<br> corehedep/net/23 - A single star 23msun model ran with a larger nuclear network</p> <p>coreodep/base - Base folder with inlists for this set of models<br> coreodep/binary - Contains a folder for each mass for the binary-stripped stars (11-45)<br> coreodep/single - Contains a folder for each mass for the single stars (11-45)</p> <p>coreodep/mesh - Test variations with respect to space and time during carbon burning<br> coreodep/overshoot - Test variations with respect to overshoot during carbon burning<br> coreodep/net - A single star 23msun model ran with a larger nuclear network</p> <p>cc/base - Base folder with inlists for this set of models<br> cc/binary - Contains a folder for each mass for the binary-stripped stars (11-45)<br> cc/single - Contains a folder for each mass for the single stars (11-45)</p> <p><br> ccsn/base - Base folder with inlists for this set of models<br> ccsn/binary - Contains a folder for each mass for the binary-stripped stars (11-45)<br> ccsn/single - Contains a folder for each mass for the single stars (11-45)<br> ccsn/laplace_binary - Contains core collapse explosions of the binary-stripped models from Laplace et al 2021<br> ccsn/laplace_single - Contains core collapse explosions of the single star models from Laplace et al 2021</p> <p>spacetime/base - Base folder with inlists for this set of models<br> spacetime/binary - Test variations in space/time resolution of ccsn explosions</p> <p>ccsn_t_m/base - Base folder with inlists for this set of models<br> ccsn_t_m/binary - Test variations in injection time and injection mass of ccsn explosions</p> <p>engmc/base - Base folder with inlists for this set of models<br> engmc/binary - Tests variations in the injection energy and mass cut of ccsn explosions</p> <p><br> ## Notes</p> <p>Folders with the name '_k' have enhanced profile output for use in Kippenhan plots.</p> <p>Folders with the name '_v' have enhanced profile output for use in the video of the shock explosion.</p> <p>Each numbered folder contains a set of inlists used (which usually only vary one or two parameters), the rest of the inlists are stored in the base/ folders (See the submit.sh files for how to get MESA to read these files). They also contain a initial.mod file (which is the starting point for this phase of evolution), this is a softlink to the final.mod file from the previous phase (thus coreodep soft links to files in corehedep, corehdep uses MESA's built in ZAMS models to start).</p> <p>The folders that handle the core collapse explosions have additional .mod files that handle each phase of the explosion. See the base/ folders for details on the order.</p> <p>## Files</p> <p>cacheHist.py - Runs mesaplot code to turn history files into a python binary file for faster reading.<br> plotKip.py - Does a quick kippenhan plot for diagnostics</p> <p> </p>
Properties of Galactic B[e] supergiants. X. Refined orbit and fundamental parameters of the HD 327083 binary system.
<p>This dataset developed with MESA version r23.05.1 (May 30, 2023) and SDK version 23.7.3 (July 24, 2023), presents a comprehensive simulation of the binary system HD 327083, focusing on its evolution under specific initial conditions. </p>
Simulating a binary system that experiences the grazing envelope evolution
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.477.2584S/abstract">Simulating a binary system that experiences the grazing envelope evolution</a></p>
A window into δ Sct stellar interiors: understanding the eclipsing binary system TT Hor
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018MNRAS.480.1372S/abstract">A window into δ Sct stellar interiors: understanding the eclipsing binary system TT Hor</a></p>
AT 2021hdr: a candidate tidal disruption of a gas cloud by a binary super massive black hole system
<p>In this dataset we provide tables for the Zwicky Transient Facility (ZTF) and Swift observations presented in the paper "AT 2021hdr: a candidate tidal disruption of a gas cloud by a binary super massive black hole system", accepted for publication in the Astronomy and Astrophysics Journal (Hernández-García et al. 2024). </p> <p> </p> <p>Files description:</p> <p>-ztf_table:_zenodo.csv: Log of the ZTF forced photometry observations. Include the dates in MJD, filter, apparent magnitudes, and difference fluxes.</p> <p>- swift_table_zenodo.csv: Log of the Swift observations, including the observation ID, date (in MJD), exposure time, count-rate in the 0.5-10 keV energy band, and UV fluxes in the UVW2 and UVM2 filters. </p>
The variable evolution of accretor stars in binary systems due to accretion of increasingly helium-rich material
<p>Dataset for paper "The variable evolution of accretor stars in binary systems due to accretion of increasingly helium-rich material".</p> <p>You will need the <a href="https://github.com/Krytic/Kaitiaki">Kaitiaki code</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>
A massive binary system with a single magnetic star
<p>HD148937 is one of the three Galactic O-type sources belonging to the rare class of Of?p objects. These stars are characterised by recurrent spectral variations, the origin of which is found to be their strong magnetic fields. Originally thought to be a single star, long baseline near-IR interferometry with PIONIER has revealed HD148937 to be a binary system. In this presentation I will discuss our investigations into the source using a combination of multi-epoch GRAVITY and PIONIER data. These data reveal that the two components are of similar brightness but one star shows the BrG line in emission and the other in absorption, confirming that only one of the two stars is magnetic. Combining our data with existing spectroscopic measurements, a preliminary 3D orbit of the system can be obtained and subsequently absolute masses. We use these new constraints to discuss the evolutionary status of this unique object in the context of the origin of the magnetic star.</p>
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OpenNeuro
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