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10 results for “magnetar”
Supporting data and scripts for Nature Astronomy article "Detection of two bright radio bursts from magnetar SGR 1935+2154" by Kirsten et al.
<p>This data set contains scripts and data used to analyze the observations described in Nature Astronomy article "Detection of two bright radio bursts from magnetar SGR 1935+2154" by Kirsten et al. 2020. The scripts used to create the plots therein also included.</p>
Onset of electron captures and shallow heating in magnetars
<p>The loss of magnetic pressure accompanying the decay of the magnetic field in a magnetar may trigger exothermic electron captures by nuclei in the shallow layers of the outer crust. The threshold density and pressure, as well as the maximum amount of heat that can be possibly released were calculated for different nuclei. The Landau-Rabi quantization of electron motion was taken into account using approximate analytical formulas. Results were obtained using experimental atomic masses and the <span class="math-tex">\(Q_\beta\)</span> values (included recommended ones) from the <a href="http://amdc.in2p3.fr/web/masseval.html">2016 Atomic Mass Evaluation</a> supplemented with the atomic mass model <a href="https://link.aps.org/doi/10.1103/PhysRevC.88.024308">HFB-24</a> available on the <a href="http://www.astro.ulb.ac.be/bruslib/">BRUSLIB</a> database.</p> <p>Each file contains data for electron captures by nuclei with the specified charge number Z and mass number A. The columns are as follows: </p> <ul> <li>magnetic field strengh in units of <span class="math-tex">\(B_{\rm rel}=\dfrac{m_e^2 c^3}{e \hbar}\approx 4.41\times 10^{13}\, \rm G\)</span></li> <li>the pressure in dyn cm<sup>-2</sup></li> <li>the mass density in g cm<sup>-3</sup></li> <li>the heat per nucleon in MeV.</li> </ul> <p>The files with (without) label 'ex' contain results for ground state to excited state (ground state) transitions.</p>
Is a number of strongly magnetised OB stars enough to produce all known magnetars?
<p>According to stellar evolution models, massive OB stars form neutron stars after the end of their life. But does the initial magnetic field of a neutron star depend on the magnetic field of a predecessor star? Some pulsar population synthesis (e.g. Gullón et al. 2015) which included thermally emitting neutron stars showed that magnetars (and for example the group of young cooling neutron stars called "the Magnificent Seven") could originate from a peculiar subpopulation of massive stars. Moreover, we can see that massive stars also can be divided into two groups: magnetic stars with average magnetic fields from several hundreds of Gauss to tens of kilogauss (only 5-7% of all) and nonmagnetic or weakly magnetic stars whose magnetic fields can not yet be measured accurately. Therefore, we want to check the hypothesis if magnetic OB stars in the Milky Way could be progenitors of magnetars. We also aim to explain how the magnetic fields depend on the stellar radii, binarity, and other parameters using modern observational data for various values (NARVAL measurements, Magnetar Outburst Online Catalog, Gaia DR2, etc). To do so, we study the distribution of magnetic fields of massive stars using the maximum likelihood technique and run a new pulsar population synthesis code. As a result of our analysis, we can claim that normal pulsars seem to be plausible descendants of the weakly magnetic OB stars and the precursors of magnetars are magnetic OB stars.</p>
Reproduction package for the paper "Multi-dimensional population modelling using frbpoppy: Magnetars can produce the observed fast radio burst sky"
<p>This is a basic reproduction package for the paper "Multi-dimensional population modelling using frbpoppy: Magnetars can produce the observed fast radio burst sky" by David Gardenier & Joeri van Leeuwen (2021).</p> <p>* arXiv: <a href="https://arxiv.org/abs/2012.06396">arXiv:2012.06396</a><br> * DOI: <a href="https://doi.org/10.1051/0004-6361/202040119">10.1051/0004-6361/202040119</a></p> <p> </p>
Magnetar+Bump Modeling of Superluminous Supernovae
<p>These data files are associated with the article <a href="https://ui.adsabs.harvard.edu/abs/2021arXiv210909743H">"Bumpy Declining Light Curves are Common in Hydrogen-poor Superluminous Supernovae."</a> This repository contains four directories, described below.</p> <p><strong>MOSFiT Output Files</strong></p> <p>The "mosfit" directory contains the raw output files from the Modular Open-Source Fitter for Transients (Guillochon et al. <a href="https://doi.org/10.3847/1538-4365/aab761">2017</a>). See its <a href="https://mosfit.readthedocs.io">documentation</a> for the output format. Keep in mind that some detections have been converted into nondetections in these files (see the paper for a full explanation), so you should not use them as a source for the photometry.</p> <p><strong>Magnetar Models</strong></p> <p>The "models" directory contains the range of models for each supernova. These are stored as <a href="https://docs.astropy.org/en/latest/io/ascii/ecsv.html">ECSV</a> files, which can be read using Astropy tables. The columns are MJD, filter, apparent magnitude (median, minimum, maximum), and absolute magnitude (median, minimum, maximum). The metadata contains the median and standard deviation of each parameter discussed in the paper, as well as the supernova name, distance modulus, and extinction.</p> <p><strong>Magnetar Parameters</strong></p> <p>The "params" directory contains the magnetar model parameters corresponding to each model realization, also stored as <a href="https://docs.astropy.org/en/latest/io/ascii/ecsv.html">ECSV</a> files. In other words, you can use these files to reproduce the posterior for each parameter. The metadata contains the units for each parameter and a LaTeX representation of each variable name.</p> <p><strong>Bump Models</strong></p> <p>The "bumps" directory contains the raw output for the bump modeling. These are stored as compressed Numpy files (.npz) and can be read using np.load. The keywords are as follows:</p> <ul> <li>"chain": the flattened MCMC chain, stored as a 2D array. The 0th dimension corresponds to the number of walkers times the number of steps. The 1st dimension corresponds to the parameters: amplitude, center (MJD), and FWHM (observed days). In the case of 2 bumps, the parameters are amplitude 1, center 1, FWHM 1, amplitude 2, center 2, FWHM 2.</li> <li>"pmed": the median of each parameter, followed by the median absolute deviation for each parameter (converted to a standard deviation).</li> <li>"energies": the integrated energy in each model realization (in watt-days).</li> <li>"energy": the median of the “energies” array.</li> <li>"denergy": the median absolute deviation of the “energies” array (converted to a standard deviation).</li> <li>"integral": the integral of the magnetar residuals before modeling (in watt-days). This is not used in the paper.</li> <li>"t0" and "t1": the range of MJDs used in the bump fitting.</li> </ul> <p>If you have any questions about this dataset, feel free to contact the author, <a href="mailto:griffin0@arizona.edu">Griffin Hosseinzadeh</a>.</p>
Supplemental data: possible Sn126 decay gamma-ray fluxes from known SNRs and magnetars
<p>The tar file contains two separate data files.</p> <p>The file SNR_flux.txt contains the list of supernova remnants and their gamma-ray line fluxes from the decay of nucleus 126Sn at 666.3 keV (100% intensity). Fluxes are calculated by assuming a ejecta mass of 0.01 solar mass, containing number fraction of 126Sn of 1.7*10^-4. Note that this list only contains those SNRs with both the age and distance information available from http://www.physics.umanitoba.ca/snr/SNRcat/.</p> <p>The file magnetar_flux.txt contains instead the gamma-ray line fluxes from known magnetars with both the characteristic age and distance information available from http://www.physics.mcgill.ca/~pulsar/magnetar/main.html.</p>
Data and Codes used in the study: Very high frequency oscillations in the main peak of a magnetar giant flare
<p>Description is given in the uploaded pdf document: Data_codes_description.pdf</p>
Toward nebular spectral modeling of magnetar-powered supernovae
<p>The set of models analyzed in Omand and Jerkstrand (2023). The zip files contain all data for the corresponding epoch and composition. All the outputs for each model are contained in the folder with the model's ID, using the system explained in the paper.</p>
A magnetar model for the hydrogen-rich super-luminous supernova iPTF14hls
<p>Model spectra from <a href="https://ui.adsabs.harvard.edu/abs/2018A%26A...610L..10D">Dessart 2018, A&A, 610, 10</a>.</p>
Simulations of light curves and spectra for superluminous Type Ic supernovae powered by magnetars
<p>Model spectra from <a href="https://ui.adsabs.harvard.edu/abs/2019A%26A...621A.141D">Dessart 2019, A&A, 621, 141</a>.</p>
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