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Constraints on neutron stars equation of state using the tidal deformability derived from BNS mergers

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Constraints on neutron stars equation of state using the tidal deformability derived from BNS mergers (EN)
Kanakis-Pegios, Alkiviadis
Moustakidis, Charalampos
info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Theoretical; Computational (EN)
2020-04-17
The purpose of this work is the study of neutron stars (NS) equation of state (EOS) using constraints on tidal deformability derived from observation of binary neutron star (BNS) mergers, such as GW170817. The mathematical formalism is introduced, and then for a variety of EOS the system is solved numerically, allowing us to determine the mass, the radius, the tidal love number and the tidal deformability of the NS, each one of them unique for each EOS. Moreover, for a fixed value of chirp mass under the assumption that m2 (EN)
equation of state (EN)
neutron stars (EN)
tidal deformability (EN)
gw170817 (EN)
Annual Symposium of the Hellenic Nuclear Physics Society
English
Hellenic Nuclear Physics Society (HNPS) (EN)
2654-0088
2654-007X
Annual Symposium of the Hellenic Nuclear Physics Society; Τόμ. 27 (2019): HNPS2019; 95-100 (EL)
HNPS Advances in Nuclear Physics; Vol. 27 (2019): HNPS2019; 95-100 (EN)
Πνευματική ιδιοκτησία (c) 2020 Alkiviadis Kanakis-Pegios, Charalampos Moustakidis (EL)
Hellenic Nuclear Physics Society
Annual Symposium of the Hellenic Nuclear Physics Society
Oral contributions



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