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5 results for “binary population synthesis”
Dataset from: Rapid stellar and binary population synthesis with COMPAS
<p>This data set is used to produce Figure 16 of the COMPAS Paper (<a href="https://arxiv.org/abs/2109.10352">Team COMPAS et al. 2021</a>).</p> <p>The file contains the output of 10,000,000 binaries evolved using COMPAS v02.21.00, using adaptive importance sampling (STROOPWAFEL) , sampling from a metallicity uniform in <span class="math-tex">\(\log(Z) \in [10^{-4},0.03]\)</span>. More details can be found in the `Run_Details` group.</p> <p>*****************************<br> Contents<br> *****************************</p> <ol> <li>COMPAS simulation output:<br> The hdf5 file Includes necessary information about the simulated binaries in the following groups:<br> <br> <strong>BSE_Double_Compact_Objects<br> BSE_Common_Envelopes<br> BSE_RLOF<br> BSE_Supernovae<br> BSE_System_Parameters<br> Run_</strong><strong>Details</strong><br> <br> We point the reader to the documentation at <a href="https://compas.science/docs">https://compas.science/docs</a>, for information and instructions regarding the contained data.<br> </li> <li><strong>Rate Data</strong><br> The hdf5 file contains 1 groups with BBH merger rate data for every BBH with an inspiral time that is smaller than the age of the Universe. This group contains a dataset "DCOmask" which can be used to point from the "DoubleCompactObjects" to the data contained in the respective rates datasets.<br> <br> We include the rates for one realization of the metallicity-dependent SFRD as discussed in the manuscript.<br> The metallicity-dependent SFRD used is the phenomenological metallicity-dependent SFRD as described in Neijssel et al. 2019, this contained in:<br> <strong>'Rates_mu00.035_muz-0.23_alpha0.0_sigma00.39_sigmaz0.0'</strong></li> </ol> <p>*****************************</p> <p>The rates were calculated by running ```FastCosmicIntegration.py``` from COMPAS's post-processing tools.<br> For a more detailed explanation of the workings of COMPAS's post-processing tools, please the docs <a href="https://compas.science/docs">https://compas.science/docs</a></p>
Dataset from: Binary population synthesis with probabilistic remnant mass and kick prescriptions
<p>This contains the data behind the paper "<a href="https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.1380M">Binary population synthesis with probabilistic remnant mass and kick prescriptions</a>"<br> <br> See<a href="https://github.com/TeamCOMPAS/COMPAS"> https://github.com/TeamCOMPAS/COMPAS</a> for code information and instructions on parsing the data.</p>
Towards a Realistic Explosion Landscape for Binary Population Synthesis
<p>Data from:</p> <p> Towards a Realistic Explosion Landscape for Binary Population Synthesis</p> <p> by</p> <p> Patton, Rachel A. and Sukhbold, Tuguldur<br> (2020).</p> <p> (Submitted to MNRAS)</p> <p>- Detailed descriptions of calculations are provided in the paper, but<br> please feel free to get in touch with any of us with questions, or<br> if you need something that is not provided here.</p> <p>Contacts:<br> Rachel Patton = patton[dot]502[at]osu[dot]edu<br> Tuguldur Sukhbold = tuguldur[dot]s[at]gmail[dot]com<br> - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - - -</p> <p>Below are brief descriptions of each dataset. More details can be found in the paper.</p> <p>kepler_table.tar.gz (1.0GB)<br> -These are tables for our entire set of 3496 KEPLER CO-core models, containing the final presupernova structure and composition quantities for each zone. Core masses range from 2.5 to 10.0 in increments of 0.1 Msun and the initial composition ranges from 5% carbon and 95% oxygen to 50% carbon and oxygen, in incrmeents of 1%. Each file has the naming convention "mA_B.ktbl" where A is the core mass in Msun (2.5, 2.6, etc.) and B represents the initial carbon mass fraction as the number of increments of 0.01 taken from 0.05 (5%). For example, the file 'm8.0_27.ktbl' would be for an 8 Msun core with an initial carbon mass fraction of 0.32 (= 0.05 + 27*0.01).</p> <p>kepler_datatset.tar.gz (30.4KB)<br> -This folder contains four tables listing the presupernova parameters evaluated from all of our KEPLER CO-cores: M_fe, the iron core mass, M4, the mass enclosed where the entropy per baryon reaches 4 Kb, mu_4, the radial gradient of mass at the location of M4, and xi_2.5, the compactness parameter. See section#3 of our paper for details on how these were evaluated. Columns represent each CO-core mass and rows represent starting carbon mass fraction.</p> <p>inlist (2.8KB)<br> -This is the inlist used to create 760 MESA (version 7624) CO-core models, presented in section#4.1. The only thing that changes between models is the CO-core mass, set by 'initial_mass' and the composition, set by 'accretion_species_xa(1)' and 'accretion_species_xa(2)'. In our grid, we covered the same mass and composition range as the KEPLER models, keeping the same mass increment but increasing the carbon mass increment from 0.01 to 0.05.</p>
Investigating the Lower Mass Gap with Low Mass X-ray Binary Population Synthesis
<p>Title: Investigating the Lower Mass Gap with Low Mass X-ray Binary Population Synthesis </p> <p>Authors: Jared C. Siegel, Ilia Kiato, Vicky Kalogera, Christopher P. L. Berry,<br> Thomas J. Maccarone, Katelyn Breivik, Jeff J. Andrews, Simone S. Bavera,<br> Aaron Dotter, Tassos Fragos, Konstantinos Kovlakas, Devina Misra,<br> Kyle A. Rocha, Philipp M. Srivastava, Meng Sun, Zepei Xing,<br> and Emmanouil Zapartas<br> <br> Table: Summary of Population Synthesis Models</p> <p>Columns:<br> Population parameters:<br> CE: efficiency of common envelope unbinding, either:<br> * 1 or 5<br> CE merge: stars without a distinct core-envelope boundary that instigate a CE <br> event are either assumed to survive the CE (Optimistic) or are <br> assumed to merge (Pessimistic).<br> QMIN: minimum ZAMS ratio, either:<br> * 0.01<br> * Lifetime limited (pre-main-sequence lifetime of the secondary is shorter<br> than the main-sequence lifetime of the primary)<br> BRK: prescription for magnetic braking of a tidally coupled magnetic wind, either:<br> * H02: Hurley et al. 2002<br> * IT03: Ivanova & Taam 2003<br> ACC: amount of mass accreted during Roche-lobe overflow, either:<br> * 50% efficiency<br> * State dependent: (i) limited to ten-times the thermal rate if the accretor is a main-sequence, <br> Hertzsprung gap or core helium burning star, or (ii) unlimited if the accretor is a giant branch, <br> early asymptotic giant branch or asymptotic giant branch star. <br> Compact objects also experience conservative mass transfer, provided the <br> mass-transfer rate is sub-Eddington.<br> <br> Selection effect parameters:<br> weighting: logs what selection effects were considered for the detection weighted results, either:<br> *prob_occ: the probability that an outburst occurs and turns off during the survey<br> *prob_see: the probability that the outburst is bright enough to be detected<br> *prob: the product of prob_occ and prob_see<br> <br> RIA_nu: determines when the transition to radiatively inefficient accretion occurs, either:<br> *0 (no transition) or 0.05<br> <br> Results:<br> f_gap_N: fraction of LMXB systems with a mass gap BH (M<4.5Msol)<br> f_AIC_N: fraction of LMXB systems where the BH formed through accretion induced collapse of a NS<br> f_AIC_gap_N: fraction of LMXB systems where the BH formed through accretion induced collapse of a NS and<br> the BH is in the mass gap<br> fw_X_N: detection weighted fraction of X (e.g., gap, AIC, AIC_gap)<br> <br> Notes:<br> Each quantity is calculated for 5000 snapshots of the evolution tracks. <br> Here we report the Nth percentiles (e.g., 16, 50, 84) of each quantity.</p>
Population synthesis data of massive binaries: NS/BH-core mergers and double compact objects formation and mergers
<p><span>Binary population synthesis data generated using the rapid population synthesis code COMPAS.</span></p> <p><span>Contains:</span></p> <p><span>1. Full COMPAS output in (.csv format) for running massive binaries varying the common envelope efficiency parameter and the metallicity.</span></p> <p><span>2. Identifying seeds of systems that result in neutron star (NS)/black hole (BH)-core mergers, binary NSs, binary BHs and NS-BH binaries. </span></p>
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