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Improved spin and density correlation simulations give researchers clearer insights on neutron stars
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</p> <p> <span class="tick-mark"></span> peer-reviewed publication </p> <p> <span class="tick-mark"></span> trusted source </p> <p> <span class="tick-mark"></span> proofread </p> </div> </div> </div> <h1 class="text-extra-large line-low mb-2">Improved spin and density correlation simulations give researchers clearer insights on neutron stars</h1> <p class="article-byline text-low"> by <a class="article-byline__link" href="http://www.energy.gov/" target="_blank">US Department of Energy</a> </p> <div class="mt-4 article-main"> <div class="article-gallery lightGallery"> <div data-thumb="https://scx1.b-cdn.net/csz/news/tmb/2024/improved-spin-and-dens.jpg" data-src="https://scx2.b-cdn.net/gfx/news/2024/improved-spin-and-dens.jpg" data-sub-html="A neutrino moves through a gas of neutrons and is sensitive to correlations in spin and density in the neutron matter. These correlations determine how much energy transfers from the neutrino to the neutrons. Credit: Dean Lee"> <figure class="article-img"> <img src="https://scx1.b-cdn.net/csz/news/800a/2024/improved-spin-and-dens.jpg" alt="Improved spin and density correlation simulations give researchers clearer insights on neutron stars" title="A neutrino moves through a gas of neutrons and is sensitive to correlations in spin and density in the neutron matter. These correlations determine how much energy transfers from the neutrino to the neutrons. Credit: Dean Lee" width="800" height="465"> <figcaption class="text-darken text-low-up text-truncate-js text-truncate mt-3"> A neutrino moves through a gas of neutrons and is sensitive to correlations in spin and density in the neutron matter. These correlations determine how much energy transfers from the neutrino to the neutrons. Credit: Dean Lee </figcaption> </figure> </div> </div><p>When a star dies in a supernova, one possible outcome is for the remains to become a neutron star. Inside a neutron star, the protons and electrons combine into uncharged neutrons. This substance is called neutron matter.</p> <div class="ads d-print-none text-center mb-4 w-100"> <!-- /4988204/Phys_Story_InText_TextOnly --> <div id='div-gpt-ad-1449240174198-2'> <script type='text/javascript'> googletag.cmd.push(function() { googletag.display('div-gpt-ad-1449240174198-2'); }); </script> </div> </div> <p>A team of researchers from the United States, China, Turkey, and Germany has performed <a href="https://phys.org/tags/ab+initio/" rel="tag" class="textTag">ab initio</a> (i.e., from the most fundamental principles) simulations to calculate spin and density correlations in <a href="https://phys.org/tags/neutron/" rel="tag" class="textTag">neutron</a> matter. They used realistic nuclear interactions at higher densities of neutrons than previously explored. Spin and density are the probability of finding a neutron in a particular position with a particular direction of <a href="https://phys.org/tags/spin/" rel="tag" class="textTag">spin</a>. These correlations determine key aspects of how neutrinos scatter and heat up in a core-collapse supernova.</p> <p>The research is <a href="https://link.aps.org/doi/10.1103/PhysRevLett.132.232502" target="_blank">published</a> in the journal <i>Physical Review Letters</i>.</p> <p>To perform the calculations, the researchers introduced a new algorithm called the "rank-one operator method" that greatly reduces the computational effort needed to calculate observables involving several particles. The rank-one operator method exploits a simplification in the complicated mathematics used in computing neutrino transport through dense nuclear matter, resulting in much more efficient computation. The rank-one operator method has since been applied to calculations of other observables in <a href="https://phys.org/tags/nuclear+physics/" rel="tag" class="textTag">nuclear physics</a> as well as other fields.</p> <p>Researchers can use the results of this new study in realistic simulations of supernova explosions. Nearly all the energy released in a core-collapse supernova is carried away by neutrinos. The outward flow of neutrinos energizes the neutron-rich matter in the supernova. This increases the likelihood of an explosion.</p> <div class="article-main__more p-4"> <p><strong>More information:</strong> Yuan-Zhuo Ma et al, Structure Factors for Hot Neutron Matter from Ab Initio Lattice Simulations with High-Fidelity Chiral Interactions, <i>Physical Review Letters</i> (2024). <a data-doi="1" href="https://dx.doi.org/10.1103/PhysRevLett.132.232502" target="_blank">DOI: 10.1103/PhysRevLett.132.232502</a>. On <i>arXiv</i>: <a data-doi="1" href="https://dx.doi.org/10.48550/arxiv.2306.04500" target="_blank">DOI: 10.48550/arxiv.2306.04500</a> <div class="mt-3"> <p> <strong>Journal information:</strong> <a href="https://phys.org/journals/physical-review-letters/"><cite>Physical Review Letters</cite></a> <a class="icon_open" href="http://prl.aps.org/" target="_blank" rel="nofollow"> <svg> <use href="https://phys.b-cdn.net/tmpl/v6/img/svg/sprite.svg#icon_open" x="0" y="0"/> </svg> </a>, <a href="https://phys.org/journals/arxiv/"><cite>arXiv</cite></a> <a class="icon_open" href="http://arxiv.org/" target="_blank" rel="nofollow"> <svg> <use href="https://phys.b-cdn.net/tmpl/v6/img/svg/sprite.svg#icon_open" x="0" y="0"/> </svg> </a> </p> </div> </div> <div class="d-inline-block text-medium mt-4"> <p> Provided by <a href="https://phys.org/partners/us-department-of-energy/">US Department of Energy</a> <a class="icon_open" href="http://www.energy.gov/" target="_blank" rel="nofollow"> <svg> <use href="https://phys.b-cdn.net/tmpl/v6/img/svg/sprite.svg#icon_open" x="0" y="0"/> </svg> </a> </p> </div> <!-- print only --> <div class="d-none d-print-block"> <div class="mb-4"> <strong>Citation</strong>: Improved spin and density correlation simulations give researchers clearer insights on neutron stars (2024, November 27) retrieved 1 December 2024 from https://phys.org/news/2024-11-density-simulations-clearer-insights-neutron.html </div> <div class="border text-muted p-3"> This document is subject to copyright. 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