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16 results for “Core-Collapse Supernovae”
Constraining properties of the next nearby core-collapse supernova with multi-messenger signals: multi-messenger signals
<p>1D FLASH simulations with STIR, for alpha_lambda = 1.23, 1.25, and 1.27. Run with SFHo EOS, M1 with 12 energy groups.</p> <p>For more information on these simulations, see Warren, Couch, O'Connor, & Morozova (arXiv:1912.03328) and Couch, Warren, & O'Connor (2020).</p> <p>Includes the multi-messenger data from the STIR simulations. The filename indicates the turbulent mixing parameter a and progenitor mass m of the simulation. Columns are time [s], shock radius [cm], explosion energy [ergs], electron neutrino mean energy [MeV], electron neutrino rms energy [MeV], electron neutrino luminosity [10^51 ergs/s], electron antineutrino mean energy [MeV], electron antineutrino rms energy [MeV], electron antineutrino luminosity [10^51 ergs/s], x neutrino mean energy [MeV], x neutrino rms energy [MeV], x neutrino luminosity [10^51 ergs/s], gravitational wave frequency from eigenmode analysis of the protoneutron star structure [Hz]. Note that the x neutrino luminosity is for <strong>one</strong> neutrino flavor - to get the total mu/tau neutrino and antineutrino luminosities requires multiplying this number by 4.</p> <p>v1.1 - removed unnecessary duplicate files</p> <p>v1.2 - upload failed. Obsolete.</p> <p>v1.3 - packaging alpha values as separate tar files for easy download.</p>
Stellar Mass Black Hole Formation and Multimessenger Signals from Three-dimensional Rotating Core-collapse Supernova Simulations
<p>Gravitational waveforms from <a href="https://ui.adsabs.harvard.edu/abs/2021ApJ...914..140P/abstract">Pan et al. (2021) .</a></p> <p>They are the 40 solar mass model from Woosley & Heger 2007 with different<br>initial rotational speeds:</p> <p>Model NR: Omega_0 = 0.0 rad/sec<br>Model SR: Omega_0 = 0.5 rad/sec<br>Model FR: Omega_0 = 1.0 rad/sec</p> <p>/* File content */</p> <p>They are 5 files for each simulation.</p> <p>Files "data_s40_[model]_d3_[Cross/Plus][Equator/Pole].d" are GW strains for different<br>mode of polarization [h_plus or h_cross] and viewing angles [equator or pole].</p> <p>1st column is time [s] in postbounce. <br>2nd column s the GW strain, assuming d=10 kpc.<br> <br>Files "data_s40_[model]_d3_Idotdot.d" are the second time derivative of the<br>quadruple moments.</p> <p>1st: postbounce time [s] <br>2nd: Idd_xx [cgs]<br>3rd: Idd_xy = Idd_yx [cgs]<br>4th: Idd_yy = Idd_yy [cgs]<br>5th: Idd_zx = Idd_zx [cgs]<br>6th: Idd_zy = Idd_zy [cgs]<br>7th: Idd_zz = Idd_zz [cgs]</p> <p> </p>
Stellar Evolution Models from "Finding the Fuse: Prospects for the Detection and Characterization of Hydrogen-Rich Core-Collapse 5 Supernova Precursor Emission with the LSST"
<p>These data consist of all runs from the Modules for Experiments in Stellar Astrophysics (MESA; Paxton et al. 2011, 2013, 2015, 2018, 2019) code, used to construct radius priors for modeling supernova precursor emission in<em> <a href="https://arxiv.org/abs/2408.13314">Finding the Fuse: Prospects for the Detection and Characterization of Hydrogen-Rich Core-Collapse 5 Supernova Precursor Emission with the LSST</a></em> (Gagliano+2024, submitted). </p> <p>The contents of the data files are detailed in the file <strong>ReadmeMESA.txt</strong>. Additional detail concerning the simulations can be found in Section 2.2 of the linked publication. </p>
Emission line models for the lowest mass core-collapse supernovae - I. Case study of a 9 M⊙ one-dimensional neutrino-driven explosion
<p>Model spectra of the 9 Msun iron-core model, and the pure H toy model, 200-600d. Distance 10 Mpc assumed.</p>
Core-Collapse Supernova
<p>Collection of certified trajectories, covering a wide range of<sup> </sup>core-collapse supernova nucleosynthesis conditions. Every trajectory comes with the selected initial abundances and other key information, such as the reference of the publication, the stellar region from where it was extracted, the mass of the progenitor star and its metallicity.</p>
Constraining properties of the next nearby core-collapse supernova with multi-messenger signals: gravitational wave frequency fits
<p>1D FLASH simulations with STIR, for alpha_lambda = 1.23, 1.25, and 1.27. Run with SFHo EOS, M1 with 12 energy groups.</p> <p>For more information on these simulations, see Warren, Couch, O'Connor, & Morozova (arXiv:1912.03328) and Couch, Warren, & O'Connor (2020).</p> <p>Includes fit to the gravitational wave peak frequency versus time post-bounce, for a functional fit of the form f = A*sqrt(t) + B*t + C, where the frequency f is in Hz and the time t is in seconds. The columns are: progenitor mass [M_sun], fit coefficient A, fit coefficient B, fit coefficient C, and the R^2 of the fit.</p>
Equation of state for simulations of core-collapse supernovae and neutron-star mergers
<p>We construct a new equation of state (EOS) for numerical simulations of core-collapse supernovae and neutron-star mergers based on an extended relativistic mean-field model with a small symmetry energy slope L, which is compatible with both experimental nuclear data and recent observations of neutron stars. The new EOS table (EOS4) based on the extended TM1 (TM1e) model with L=40 MeV is designed in the same tabular form as the commonly used Shen EOS (EOS2) based on the original TM1 model with L=110.8 MeV. This is convenient and useful for performing numerical simulations and examining the influences of symmetry energy and its density dependence on astrophysical phenomena. </p> <p> </p>
A Detailed Comparison of Multi-Dimensional Boltzmann Neutrino Transport Methods in Core-Collapse Supernovae
<p>This dataset contains results of 1D and 2D static neutrino transport calculations using discrete ordinates and Monte Carlo methods, as described in the 2017 paper by the same name. The results include the neutrino momentum space grids used for the simulations, the full spectral and angular distribution functions, energy-dependent angular moments of the distribution functions, and neutrino heating rates. The HDF5 dataset name corresponds to the simulation of the same name in the 2017 paper, Table 1. Also included are the fluid backgrounds and opacities. See the readme for a description of all quantities in the datasets.</p> <p>There are also two simulation setups including all initial conditions and parameters for 1D and 2D Monte Carlo calculations using the open-source code Sedonu. This accompanies Sedonu commit 8bd509b27aa0461df26b194df65b4526d6c153fe.</p>
The Impact of Nuclear Reaction Rate Uncertainties on the Evolution of Core-collapse Supernova Progenitors
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/#abs/2018ApJS..234...19F/abstract">Fields et al. (2018)</a>. MESA version 7624.</p> <p>Publication DOI: <a href="https://doi.org/10.3847/1538-4365/aaa29b">10.3847/1538-4365/aaa29b</a></p>
Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2017MNRAS.466.2085M">Moriya et al. (2017)</a>. MESA version 7624.</p> <p>Publication DOI: <a href="https://doi.org/10.1093/mnras/stw3225">10.1093/mnras/stw3225</a></p>
Three-dimensional simulations of rapidly rotating core-collapse supernovae: finding a neutrino-powered explosion aided by non-axisymmetric flows
<p>Those are movies of numerical supernova models, which appear in Takiwaki, Kotake, and Suwa 2016 Monthly Notices of the Royal Astronomical Society: Letters, Volume 461, Issue 1, p.L112-L116.</p> <p> </p> <p> </p>
Measuring the distance and mass of galactic core-collapse supernovae using neutrinos
<p>This is the dataset and analysis scripts for the manuscript "Measuring the distance and mass of galactic core-collapse supernovae using neutrinos" (submitted to PRL, arXiv link to follow). </p>
The Nucleosynthetic Yields of Core-collapse Supernovae: Prospects for the Next Generation of Gamma-Ray Astronomy Dataset
<p>Models used in "The Nucleosynthetic Yields of Core-collapse Supernovae: Prospects for the Next Generation of Gamma-Ray Astronomy"</p>
On The Development of Multidimensional Progenitor Models For Core-collapse Supernovae
<p>Eight multi-dimensional core-collapse supernova progenitor models from work, 'On The Development of Multidimensional Progenitor Models For Core-collapse Supernovae'. Works that utilize these progenitor models are required to cite article. All models are given at 424 seconds, less than a second before iron core-collapse. The 3D 4pi models were evolved to 424.31 seconds, the collapse time according to the 1D MESA model. All data are in FLASH4 format using the HDF5 data structure. </p>
{Core-Collapse Supernovae in Binaries as the Origin of Galactic Hyper-Runaway Stars
<p>Several stars detected moving at velocities near to or exceeding the Galactic escape speed likely originated in the Milky Way disc. We quantitatively explore the `binary supernova scenario' hypothesis, wherein these stars are ejected at large peculiar velocities when their close, massive binary companions undergo a core-collapse supernova and the binary is disrupted. We perform an extensive suite of binary population synthesis simulations evolving massive systems to determine the assumptions and parameters which most impact the ejection rate of fast stars. In a simulation tailored to eject fast stars, we find hyper-runaway star progenitor binaries composed of a massive (~30 M<sub>sun</sub>) primary and a ~3-4 M<sub>sun</sub> companion on an orbital period that shrinks to <1 day prior to the core collapse following a common envelope phase. The black hole remnant formed from the primary must receive a natal kick >1000 km/s to disrupt the binary and eject the companion at a large velocity. We compare the fast stars produced in these simulations to a contemporary census of early-type Milky Way hyper-runaway star candidates. We find that these rare objects may be produced in sufficient number only when poorly-constrained binary evolution parameters related to the strength of post-core collapse black hole natal kicks and common envelope efficiency are adjusted to values currently unsupported -- but not excluded -- by the literature. We discuss observational implications that may constrain the existence of these putative progenitor systems.</p>
On The Development of Realistic Multi-Dimensional Progenitor Models For Core-Collapse Supernovae
<p>Seven multi-dimensional core-collapse supernova progenitor models from work, 'On The Development of Realistic Multi-Dimensional Progenitor Models For Core-Collapse Supernovae'. Works that utilize these progenitor models are required to cite article [fields 2019]. All models are given at 424 seconds, less than a second before iron core-collapse. The 3D 4pi model was evolved to 424.31 seconds, the collapse time according to the 1D MESA model. All data are in FLASH4 format using the HDF5 data structure. </p>
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