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5 results for “dense matter”

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zenodo48/100

Relativistic description of dense matter equation of state and compatibility with neutron star observables: a Bayesian approach

<p>The general behavior of the nuclear equation of state (EOS), relevant for the description of neutron stars (NS), is studied within a Bayesian approach applied to a set of models based on a density-dependent relativistic mean-field description of nuclear matter&nbsp;<a href="https://arxiv.org/abs/2201.12552">Malik et al 2022</a>. The EOS is subjected to a minimal number of constraints based on nuclear saturation properties and the low-density pure neutron matter EOS obtained from a precise next-to-next-to-next-to-leading order (N$^{3}$LO) calculation in chiral effective field theory ($\chi$EFT). The number of final sample parameters corresponding to the posterior sets is around fourteen&nbsp;thousand. We present five EOSs among them, namely DDBl, DDBm, DDBu1, DDBu2, and DDBx. The DDBl, DDBm, DDBu2 were chosen so that the radius of the 1.4$M_\odot$ star has the lower limit, a medium value, and the upper limit of the 90% CI for the conditional probabilities $P(R|M)$. We have also included DDBu1 that has a slightly lower $R_{1.4}$ than the upper limit but lies completely inside the 90% CI for the conditional probabilities $P(R|M)$. The DDBx is the one that predicts a maximum mass of 2.5$M_\odot$ and has the following nuclear matter properties, $K_0=300$ MeV, $J_{sym,0}=30$ MeV and $L_{sym,0}=39$ MeV.</p> <p>We also release our entire sets of ~14K NS matter EOS. All the EOSs are for NS core and starting baryon density is 0.04 fm$^{-3}$. One needs to add their own choice of crust EOS for the star properties calculation. The uncertainty in star properties for the choice of the different crust has been discussed in Section 2.1 of the manuscript (arxiv: 2201.12552).&nbsp;</p> <pre> To extract the entire sets of ~14K NS matter EOS files, one needs to follow the steps, 1) unzip DDB_EOS_14K.zip ----------------------------Note------------------------------------- All the eos files have three columns baryon density (fm-3), energy density (MeV.fm-3), and pressure (MeV.fm-3). The starting density is 0.04 fm-3, as it is NS core eos. One needs to add their own choice of crust eos in order to calculate NS properties. ---------------------------------------------------------------</pre> <p>&nbsp;</p> <p>&nbsp;</p>

opencc-by-4.0Mar 2022View details →
zenodo40/100

Constraining the dense matter equation of state with joint analysis of NICERand LIGO/Virgo measurements: Data for generating plots

<p>In this repository you will find a Jupyter&nbsp;notebook with code to generate the plots from the paper <em>Constraining the dense matter equation of state with joint analysis of NICER and LIGO/Virgo measurements</em>&nbsp;by&nbsp;Raaijmakers et al. (2020).</p>

opencc-by-4.0Mar 2020View details →
zenodo40/100

Constraining the dense matter equation of state with new NICER mass-radius measurements and new chiral effective field theory constraints: prior and posterior samples and scripts for generating plots

<p>Full reproduction package accompanying the paper: <em>Constraining the dense matter equation of state with new NICER mass-radius measurements and </em><em>new chiral effective field theory inputs</em></p> <p>&nbsp;</p> <p><em>*Note, the changes made from version to version are made visible in the CHANGELOG.rst file</em></p>

opencc-by-4.0Jul 2024View details →
zenodo40/100

Constraining the Neutron Star Mass-Radius Relation and Dense Matter Equation of State with NICER. I. The Millisecond Pulsar X-Ray Data Set

<p>This deposit includes the cleaned, filtered and phase folded NICER event data set for the millisecond pulsar (MSP) PSR J0030+0451 in the 0.25-3 keV band. The data processing and filtering was performed using HEASoft 6.251 and NICERDAS version 5.0; the specific parameters and filtering criteria used are detailed in the ApJ Letter listed above. This event list was used to produce what is shown for PSR J0030+0451 in Figures 2, 3, and 4 in the accepted ApJ Letter listed above and was also used for the neutron star mass-radius and equation of state inference analyses presented in the companion papers (Miller et al. 2019, Riley et al. 2019, and Raaijmakers et al. 2019).</p> <p>The event file and its MD5 checksum is:<br> J0030+0451_merged_phase_0.25-3keV.fits (463bbac7203bb45bb02ea0deed49f083)<br> &nbsp;</p>

opencc-by-4.0Oct 2019View details →
zenodo40/100

Bayesian inference of the dense matter equation of state built upon extended Skyrme interactions [Data Set]

<pre>&nbsp;</pre> <p>We provide the posterior distributions of the input parameters of the five main runs considered in the article "Bayesian inference of the dense matter equation of state built upon extended Skyrme interactions" (accepted to Phys. Rev. C, arXiv: 2403.19325).</p> <p>Each row in each file corresponds to one equation of state. It contains 13 input parameters of the extend Skyrme interaction that define the effective interaction and that can be used in order to construct equations of state. The input parameters (columns, from left to right) and their dimensions are:&nbsp;</p> <p>C_0 (MeV*fm^3); D_0 (MeV*fm^3); C_3 (MeV*fm^{3+3*sigma}); D_3 (MeV*fm^{3+3*sigma}); C_eff (MeV*fm^5); D_eff (MeV*fm^5); t_4 (MeV*fm^{5+3*beta}); t_5 (MeV*fm^{5+3*gamma}); x_4; x_5; sigma; beta; gamma.</p> <p>See the article for more details.</p>

opencc-by-4.0Aug 2024View details →

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