2017 Margalit & Metzger 2017 Radice et al. 2017b), specifically a short gamma-ray burst and a kilonova (e.g. More stringent constraints have been obtained by combining information from the GW signal with the properties of the detected electromagnetic counterparts ( Abbott et al. The measurement of the tidal deformability in addition to the constraint represented by the maximum measured NS mass has allowed researchers to put constraints on the equation of state (EOS) of cold NSs ( Abbott et al. 2017a) opened a new window into the microphysics of microphysics of neutron stars (NSs). The detection of the gravitational wave (GW) event GW170817 from the inspiral phase of a binary neutron star (BNS) merger ( Abbott et al. Subscribe to A&A to support open access publication. This article is published in open access under the Subscribe to Open model. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License ( ), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. This work demonstrates that muons have a non-negligible effect on the outcome of BNS merger simulations, and they should be included to improve the accuracy of a simulation. Finally, muons and trapped neutrinos modify the neutron-to-proton ratio, affecting the remnant pressure by up to 7% when compared with calculations neglecting them.Ĭonclusions. Muons change the flavour hierarchy of trapped (anti-)neutrinos such that deep inside the remnant, muon anti-neutrinos are the most abundant, followed by electron anti-neutrinos. We find that depending on the baryonic EOS, the net fraction of muons is between 30% and 70% the net fraction of electrons. We compute the abundance of muons in the remnant and analyse how muons affect the trapped neutrino component and the fluid pressure. We post-process the outcome of four numerical relativity simulations of BNS mergers performed with three different baryonic EOSs and two mass ratios considering the first 15 milliseconds after merger. Our work is aimed at investigating the impact of muons on the merger remnant. However, muons are known to be relevant in the microphysics of cold NSs and are expected to have a significant role in mergers, where the typical thermodynamic conditions favour their production. State-of-the-art simulations of BNS mergers do not include muons. In this context, improving BNS merger numerical simulations is crucial to correctly interpret the data and constrain the equation of state (EOS) of neutron stars (NSs).Īims. In the upcoming years, present and next-generation gravitational wave observatories will detect a larger number of binary neutron star (BNS) mergers with increasing accuracy. INFN-TIFPA, Trento Institute for Fundamental Physics and Applications, Via Sommarive 14, 38123 Trento, Italyĭipartimento di Fisica, Universitá di Pisa, Largo B. Maggini snc, 64100 Teramo, Italyĭipartimento di Fisica, Universitá di Trento, Via Sommarive 14, 38123 Trento, Italy INAF – Osservatorio Astronomico d’Abruzzo, Via M. Acitelli 22, 67100 Assergi L’Aquila, Italy Gran Sasso Science Institute, Viale Francesco Crispi 7, 67100 L’Aquila, ItalyĮ-mail: – Laboratori Nazionali del Gran Sasso, Via G. Astronomical objects: linking to databasesĮleonora Loffredo 1 ,2 ,3, Albino Perego 4 ,5, Domenico Logoteta 6 ,7 and Marica Branchesi 1 ,2 ,3.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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