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8 results for “binaries: close”
Pulsational pair-instability supernovae in very close binaries
<p>Models of pulsational pair-instability supernovae arising from the evolution of metal poor helium stars. These simulations have been made with the MESA software instrument for stellar evolution, and are used in the paper <a href="https://ui.adsabs.harvard.edu/abs/2019ApJ...882...36M/abstract">"Pulsational pair-instability supernovae in very close binaries"</a>. Data includes machine-readable tables, both history and profile files from the simulations, as well as the terminal output and a movie for each. All MESA output files have been post-processed to reduce their size. All the code used to process the MESA simulations and produce figures is provided in a jupyter-notebook.</p> <p>WARNING: Simulations were done using a development MESA version (11123) rather than an official release. </p> <p>List of files:</p> <p>- template.tar.xz: MESA work folder to reproduce the simulations.</p> <p>- xxx_xx.tar.xz: Each of these files contains stellar profiles at different moments of evolution for one simulation.</p> <p>- histories.tar.xz: MESA history files for each simulation, containing the time evolution of quantities that are single-valued at each moment in time.</p> <p>- preSN.tar.xz: profiles for stars before the onset of pulsations (see paper for definition).</p> <p>- movies.tar: Movies for all simulations, produced using MESAs pgstar.</p> <p>- terminal_output.tar.xz: Terminal output from the simulations.</p> <p>- masses_table.txt: Machine readable version of Table 1 in the paper.</p> <p>- pulse_tables.tar.xz: machine readable tables containing mass lost, time, and kinetic energy of each pulse.</p> <p>- notebook.tar.xz: jupyter-notebook plus complementary files used to post-process the data and produce Figures.</p> <p>This version of the files has an updated notebook.tar.xz to produce the figures in the published version of the paper.</p>
Ultra-luminous X-ray sources and neutron-star-black-hole mergers from very massive close binaries at low metallicity
<p>MESA inlists, run_star_extras, and data associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017A&A...604A..55M">Marchant et al. (2017)</a>. MESA version 8118.</p> <p>Publication DOI: <a href="https://doi.org/10.1051/0004-6361/201630188">10.1051/0004-6361/201630188</a></p> <p>Files are also available in a gihub repository <a href="https://github.com/orlox/mesa_input_data/tree/master/2016_ULX">here</a></p> <p>Upload includes post-processed simulation output in the files Z-XX.tar.xz, where XX represents the metallicity (Z-25.tar.gz is for a metallicity of log10(Z)=-2.5). Each folder inside the archive corresponds to a single MESA simulation, with the name indicating the value of log10(M_1), q=M2/M1 and the orbital period in days. For example, the directory 1.600_0.500_0.900 corresponds to the simulation with log10(M1/Msun)=1.6, M2/M1=0.5 and Porb=0.9 days. Each folder is also a MESA template folder, containing all input files neccesary to reproduce that individual simulation.</p> <p>The file summary_tables.tar.gz contains summarized information for each simulation in ascii format.</p>
Animations for "Remnants of Subdwarf Helium Donor Stars Ejected from Close Binaries with Thermonuclear Supernovae"
<p>Movies showing time evolution of the density in the z=0 plane for each of the seven Athena++ models in the paper. Each movie file corresponds to one model, labeled according to donor model number and the kinetic energy of the explosion in units of 10<sup>51</sup> ergs.</p>
Tidally perturbed g-mode pulsations in a sample of close eclipsing binaries
<p>Description:<br> Reduced Kepler and TESS light curves of KIC 3228863, KIC 3341457, KIC 4947528, KIC 9108579, and<br> KIC 12785282, as well as various data products obtained at different steps of the analysis presented in Van Reeth<br> et al. (2023): the residual pulsation light curves (after subtracting the harmonic model for the binarity), the<br> optimised prewhitened (Kepler) frequency lists, measured g-mode patterns, and detected tidal g-mode<br> perturbations (both measured directly from orbital-phase-binned data and reconstructed using detected<br> orbital-frequency-spaced multiplets).</p> <p>Abstract:<br> Context. Thanks to the high-precision photometry from space missions such as Kepler and TESS, tidal<br> perturbations and tilting of pulsations have been detected in more than a dozen binary systems. However, only<br> two of these were gravity-mode (g-mode) pulsators.<br> Aims. We aim to detect tidally perturbed g modes in additional binary systems and characterise them<br> observationally.<br> Methods. We perform a custom data reduction of the available Kepler and TESS photometry of a well-studied,<br> published sample of 35 binary systems with gamma Doradus (gamma Dor) pulsators. For each target, we model<br> the binary signal using a sum of 100 sine waves, with frequencies at orbital harmonics, and measure significant<br> pulsation frequencies in an iterative prewhitening analysis of the residual light curve. Pulsations are<br> labelled as tidally perturbed g modes if they are part of both period-spacing patterns and multiplets spaced by<br> integer multiples of the orbital frequency. After visual inspection and confirmation, the properties of these<br> targets and g modes are characterised.<br> Results. We detect tidally perturbed g-mode pulsations for five short-period binaries that are circularised and<br> (almost) synchronously rotating: KIC 3228863, KIC 3341457, KIC 4947528, KIC 9108579, and KIC 12785282.<br> Tidally perturbed g modes that occur within the same star and have the same mode identification (k,m), are found<br> to have near-identical relative amplitude and phase modulations, which are within their respective 1-sigma<br> uncertainties also identical for the Kepler and TESS photometric passbands. By contrast, pulsations with<br> different mode identification (k,m) are found to exhibit different modulations. Moreover, the observed<br> amplitude and phase modulations are correlated, indicating that the binary tides primarily distort the g-mode<br> amplitudes on the stellar surface. The phase modulations are then primarily a geometric effect of the<br> integration of the stellar flux over the visible stellar surface. All selected binaries also exhibit signal<br> that resembles rotational modulation in the Fourier domain. In the case of KIC 3228863, this is caused by the<br> presence of the known tertiary component, and for the other systems we hypothesise that it is caused by<br> temperature variations on the stellar surface. Alternatively, the signal can be overstable convective modes in<br> the stellar core or belong to the non-pulsating companion.<br> Conclusions. While g-mode pulsation periods are known to be a direct probe of the deep interior stellar<br> structure, the binary tides which cause the pulsation modulations are dominant in the outer stellar layers.<br> Hence, in future tidally perturbed g modes may allow us to do core-to-surface asteroseismic modelling of<br> tidally distorted stars.</p>
Binary Fate Choice Between Closely Related Interneuronal Types is Determined by a Fezf1-Dependent Postmitotic Transcriptional Switch
GEO Series GSE132555. Mus musculus. 27 samples. Type: Expression profiling by high throughput sequencing.
The data for a catalog of newly discovered close binary open clusters in the Milky Way from Gaia DR3
<p>The database for a catalog of newly discovered close binary open clusters in the Milky Way from Gaia DR3.</p> <p>It corresponds to the study of Zhongmu Li, Zhanpeng Zhu in 2024, which was submitted to AJ. When one use these data, please cite to that work. </p> <p>The database contains four parts, i.e., a parameter file and four directories. They are explained as follows.</p> <p>The file of ''data_tableI.csv'' gives the spatial positions and parallaxs of 13 newly discovered close binary open clusters (CBOCs).</p> <p>There are 11 columns in this file. The colums are for Name1, RA1, DEC1, Parallax1, Rtidal1, Name2, RA2, DEC2, Parallax2, Rtidal2 respectively. </p> <p>They correspond to the contents of a manuscript that was submitted to AJ.</p> <p>The file of ''data_tableII.csv'' contains the data of the fundamental parameters of 13 newly discovered CBOCs, together with their astrometric information. PBOC means primordial binary open cluster member. Distance modulus, color excess, age, and metal abundance of the clusters were obtained by fitting Parsec isochrones and Powerful CMD code. Proper motion data for the clusters were provided by HR23.</p> <p>Columns 3-14 show the basic parameters (distance modulus, color excess, age, and metal abundance) and errors of the cluster. Columns 15-16 are the proper motion data for the clusters. Column 17 is the number of member stars of the cluster.</p> <p>The file of ''data_tableIII.csv'' contains the data of Parameters for checking gravitationally bound and unbound cluster pairs. The subscripts 1 and 2 indicate the first and second sub-clusters respectively. Rroche is the Roche radius. RV 1, RV 2 and ΔRV denote the radial velocities of two member clusters and their difference. Porb and Vorb denote orbital period and orbital velocity.</p> <p>There are 13 columns in this file. The colums are for Name1, Name2, d12, r1, r2, Rroche, Mass1, Mass2, Porb, RV1, RV2, ΔRV, Vorb respectively. </p> <p>The file of ''memeber_allp.txt'' gives the list of member stars of 13 pairs of clusters. Data provided by HR23.</p> <p>If you have any problems with using these data, send an email to zhongmuli@126.com.</p>
Effects of close binary evolution on the main-sequence morphology of young star clusters
<p>Star cluster animation to show their evolution in the Hertzsprung-Russell diagram.</p>
Data for "A binary system in the S cluster close to the supermassive black hole Sagittarius A*"
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