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34 results for “core collapse”
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>
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>
Implications of large binding energies of massive stripped core collapse supernova progenitors on the explosion mechanism
<p>Inlist files (r15140) used for the creation of the core-collapse progenitor models in the paper "The implications of large binding energies of massive, stripped, core-collapse supernova progenitors on the explosion mechanism". Based on the ‘20M pre ms to core collapse’ example from MESA r22.05, adapted for use in r15140, and include several variations as detailed in the paper appendix A. See README.txt for running details and example script.</p> <p>Also included are the full simulation list and the profiles of the 52 simulated cases, including the pre-collapse profiles at the point of termination for the 27 models that reached collapse. Profiles are at central oxygen depletion (5% abundance at center), central silicon depletion (5% abundance at center) and collapse, as defined in the paper.</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>
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>
MESA files for: "Progenitor stars calculated with small reaction networks should not be used as initial conditions for core collapse"
<p>Reproduction package for RNAAS [TBD].<br><br>Use MESA r24.03.1 and the provided template folder in `MESA_template.tar.xz` to reproduce the MESA models. Resolution tests can be done changing in `inlist1` the parameters `mesh_delta_coeff`, `mesh_time_coeff`, and `mesh_delta_coeff_for_highT` (see commented option).<br>Use the provided `environment.yml` and the script `compare_two_models.py` provided in `scripts.tar.xz` with a few dependencies to reproduce the figure in the research note.</p>
The rotational shear in pre-collapse cores of massive stars
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2018MNRAS.474.1194Z">The rotational shear in pre-collapse cores of massive stars</a></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>
Thermal runaway during the evolution of ONeMg cores towards accretion-induced collapse
<p>MESA inlists associated with <a href="http://adsabs.harvard.edu/abs/2015MNRAS.453.1910S">Schwab et al. (2015)</a>. MESA version r5118.</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>
Hyperbaric Oxygen Therapy Versus Core Decompression Augmented With Bone Substitute in Pre Collapse of Avascular Necrosis of Femoral Head
ClinicalTrials.gov study NCT04657653. IPD Sharing: UNDECIDED. Countries: 1. Publications: 0.
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>
Z=0.04 core collapse helium star models
<p>Core collapse models of helium stars at Z=0.04</p>
ScienceDex guides
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
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International Brain Laboratory public data
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OpenNeuro
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