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46 results for “stars: evolution”
Reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution: V. Models at low metallicity" by Keszthelyi et al. 2024
<p>This is a reproduction package for the paper "The effects of surface fossil magnetic fields on massive star evolution: V. Models at low metallicity" by <a href="https://ui.adsabs.harvard.edu/abs/2024MNRAS.tmp.1818K/abstract">Keszthelyi et al. 2024</a></p>
FRB Mock Catalog and Reproduction Package for "Birth and Evolution of Fast Radio Bursts: Strong Population-Based Evidence for a Neutron-Star Origin"
<h3>Quickstart: FRB Mock Catalog</h3> <p>A simulated 1-day catalog of one-off FRBs, that allows users to access the FRB population without installing the entire frbpoppy package. Download and unzip 1_Day_FRB_Sky_on_Earth.txt.zip (175 MB). This human and machine readable file contains 3.5E6 FRBs that are brighter than 0.01 Jy ms, the best limit in one-off FRB detection currently. The simulated catalog is produced by the perfect telescope in frbpoppy, free of selection effects, that observed 4pi of sky for 24 hrs, with minimum detectable fluence 0.01 Jy ms, for the best-fit no-delay SFR model. This file can be read using the accompanying jupyter notebook "starting_with_mock_catalog.ipynb".</p> <p>If you use this, please cite Wang & van Leeuwen 2024 (A&A), <a href="https://doi.org/10.1051/0004-6361/202450673">https://doi.org/10.1051/0004-6361/202450673</a></p> <h3>Reproduction package for the paper "Birth and Evolution of Fast Radio Bursts: Strong Population-Based Evidence for a Neutron-Star Origin"</h3> <p>ReproductionPackage.zip is a basic reproduction package for the paper "Birth and Evolution of Fast Radio Bursts: Strong Population-Based Evidence for a Neutron-Star Origin" by Wang & van Leeuwen (2024).</p> <p> * arXiv: [<a href="https://arxiv.org/abs/2405.06281">2405.06281</a>] <br> * DOI: [<a href="https://doi.org/10.1051/0004-6361/202450673">10.1051/0004-6361/202450673</a>] </p> <h3>Installation</h3> <p>First pull or download and `frbpoppy` from <https://github.com/TRASAL/frbpoppy>.<br>Then download `ReproductionPackage.zip` and extract it starting in the frbpoppy/ base directory.<br>The scripts to produce the Figures are found in folder `frbpoppy/tests/markov_chain_monte_carlo/`.<br>The data used for these Figures resides in folder `frbpoppy/data/populations/mcmc/`.</p> <h3>Software</h3> <p>The methods and software packages used to produce the results are listed in the paper (including links to the relevant publications and/or packages):<br> FRBPOPPY: <https://github.com/TRASAL/frbpoppy><br> TRASAL: <https://github.com/TRASAL></p> <h3>Raw Data</h3> <p>The data are publicly available at<br> https://www.wis-tns.org/</p> <p> </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>
The Evolution of Intermediate Mass Stars
<p>Intermediate mass stars (M ~ 2.0 - 3.0 Msun) provide interesting constraints on stellar rotation and evolution because they live in an important transitional regime. Like massive stars, they rotate rapidly on the main sequence and have convective cores. However, they evolve to become secondary clump stars, where their structure and internal rotation can be measured with the tools of red giant asteroseismology developed for lower mass stars. We have used these tools to track these stars as they evolve, and measured their rotation, activity, and chemical mixing in various phases. I will demonstrate that the slow rotation rates of these stars provide conclusive evidence for some combination of strong post-main-sequence angular momentum loss and differential rotation with depth in convective envelopes, and discuss their core-envelope coupling as a function of time. Finally, I will discuss the relationships between rotation, activity, and mixing in these stars, and their implications for the broader population of massive stars.</p>
Exploring uncertainties in the evolution of massive stars with METISSE
<p>In the era of advanced electromagnetic and gravitational wave detectors, it has become increasingly important to effectively combine and study the impact of stellar evolution on binaries and star clusters. Systematic studies dedicated to exploring uncertain parameters in stellar evolution are required to account for the recent observations of the stellar populations. While fitting formulae to stellar tracks in the form of Single Star Evolution (SSE) code remain a popular choice for modelling stellar evolution in population synthesis codes, they are less adaptable to changes in the stellar tracks. Hence, we have developed a Method of Interpolation for Single Star Evolution (METISSE) as an alternative to SSE. It makes use of interpolation between sets of pre-computed stellar tracks to approximate evolution parameters for a population of stars. METISSE is comparable to SSE in performance and can reproduce tracks from different stellar evolution codes quite accurately. In this work, we apply METISSE with detailed stellar tracks computed by the Modules for Experiments in Stellar Astrophysics (MESA), Bonn Evolutionary Code (BEC), to study the impact of uncertainties in stellar evolution on a population of massive stars. We find that different physical ingredients used in the evolution of stars, such as the treatment of radiation dominated envelopes, can impact their evolutionary outcome, including remnant masses and maximal radial expansion. The differences in the predictions of different stellar models can help us account for the present day observations of stellar populations.</p>
State-of-the-art evolution models for single, binary and magnetic massive stars
<p>The Universe is threaded by magnetic fields on all scales, from planetary systems to galaxy clusters. In massive stars, they play a pivotal and multifaceted role. They are thought to be crucial in transporting angular momentum throughout the stellar interior and maintaining the overall angular-momentum budget. They may also contribute to chemical mixing, can interact with convective fluid motions and may give rise to distinct seismic signatures. For example, the spin rates of white dwarfs, neutron stars and black holes are strongly determined by the coupling of a star’s core to its envelope. In this talk, I will discuss recent progress in our understanding of how magnetic fields affect single and binary stars, and what are possible origins of the different types of magnetic fields in massive stars. In particular, I will highlight connections to observations and how these can be used to further our understanding of how magnetic fields influence the evolution and final fates of stars.</p>
General-Relativistic Hydrodynamics Simulation of a Neutron Star — Sub-Solar-Mass Black Hole Merger - Kilonova Luminosity Evolution Visualization
<p>Evolution of luminosity maps as seen by observers from the pole with Θ = 0° and from the four angles Φ = 0°, Φ = 90°, Φ = 180° and Φ = 270° in the equatorial plane with Θ = 90°. The maps show the luminosity from each region of the ejecta integrated along the line of sight and are calculated in (6000 − 8000) Å band at 1 day after the merger.</p> <p>Visualization: Ivan Markin (University of Potsdam), Mattia Bulla (University of Ferrara); Data: Anna Neuweiler (University of Potsdam), Swami Vivekanandji Chaurasia (Stockholm University)</p> <p>Simulations for the project have been performed on the national supercomputer HPE Apollo Hawk at the High Performance Computing (HPC) Center Stuttgart (HLRS) under the grant number GWanalysis/44189, on the GCS Supercomputer SuperMUC NG at the Leibniz Supercomputing Centre (LRZ) [project pn29ba], and on the HPC systems Lise/Emmy of the North German Supercomputing Alliance (HLRN) [project bbp00049] for the final production runs. The particular simulation shown here has been run on HLRN.</p>
A calibration point for stellar evolution from massive star asteroseismology: supplementary dataset
<p>Dataset related to the article "A calibration point for stellar evolution from massive star asteroseismology" by Burssens et al. 2022 published in Nature Astronomy on the 22nd of June 2023. </p> <p>This dataset contains:</p> <p>1) The frequency list derived from the cycle 2 TESS data set of HD192575 in machine-readable format. Units are provided in the article. </p> <p>2) The MESA/GYRE inlists needed to reproduce models and figures. </p> <p>See the article for more detailed information.</p> <p> </p> <p> </p> <p> </p> <div> </div>
Data from: A pulsar-helium star compact binary system formed by common envelope evolution
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Functional characterization of luciferase in a brittle star indicates parallel evolution influenced by genomic availability of haloalkane dehalogenase
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Properties of OB star−black hole systems derived from detailedbinary evolution models
<p>Input files to reproduce the MESA simulations used in <a href="https://arxiv.org/abs/1912.09826">Langer et al. (2020)</a></p> <p>MESA version 8845</p> <p>For instructions, refer to the README.md file included.</p>
The evolution of massive binary stars
<p>Input files and data to reproduce the figures of the review paper "The Evolution of Massive Binary Stars".</p><p>Simulations shown in the paper were computed using the Modules for Experiments in Stellar Astrophysics code (MESA), with version r23.05.1 and compiled with the MESA SDK version x86_64-linux-22.6.1.</p><p>Figures were produced using the julia programming language version 1.9.2 together with Makie.jl. A Project.toml and Manifest.toml file are provided to reproduce the environment used to produce the figures.</p>
Reproduction package for the paper "Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): The SPHERE view of the Orion star-forming region"
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Simulating the onset of grazing envelope evolution of binary stars
<p>MESA files associated with <a href="https://ui.adsabs.harvard.edu/#abs/2017MNRAS.465L..54S/abstract">Simulating the onset of grazing envelope evolution of binary stars</a></p>
Exploring Stellar Evolution Models of sdB Stars using MESA
<p>MESA inlists associated with <a href="https://ui.adsabs.harvard.edu/?#abs/2015ApJ...806..178S">Exploring Stellar Evolution Models of sdB Stars using MESA</a></p>
Online material to publication "Exploring the dynamical evolution of Cepheid multiplicity in star clusters and its implications for B-star multiplicity at birth"
<p>The description of the movie can be found in the file movie_description.pdf.</p> <p>The full paper can be found here: https://ui.adsabs.harvard.edu/abs/2024arXiv240907530D/abstract</p>
Data from: Positive selection on sperm ion channels in a brooding brittle star: consequence of life-history traits evolution
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Data from: Structure and evolution of the sea star egg receptor for sperm bindin
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Animation of MS evolution in young star clusters
<p>The video shows the evolution of binary and single stellar models from 1Myr to 100Myr. </p>
Online material to paper "On the dynamical evolution of Cepheids in star clusters"
<p>The description of the movies can be found in the file movie_description.pdf.</p>
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.