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Effective field theory with genuine many‐body forces and tidal effects on neutron stars
Author(s) -
Razeira M.,
Hadjimichef D.,
Machado M. V. T.,
Köpp F.,
Volkmer G.,
Bodmann B.,
Degrazia G. A.,
Vasconcellos C. A. Z.
Publication year - 2019
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.201913590
Subject(s) - neutron star , physics , quadrupole , moment of inertia , equation of state , tidal force , astrophysics , gravitation , stars , gravitational wave , field (mathematics) , classical mechanics , atomic physics , quantum mechanics , mathematics , pure mathematics
Neutron stars are characterized by their masses, radii, spinning speeds (associated with their moments of inertia), and degree of deformation. Under the action of an external static tidal quadrupole field ℰ ij , the neutron star undergoes a deformation measured in terms of the ratio between the quadrupole moment induced in the star and the field ℰ ij , which defines, in turn, the tidal deformability parameter. In this contribution, we combine our recent predictions for the neutron stars' tidal parameter with recent gravitational wave observations of merging the binary system GW170817 with quasiuniversal relations between the maximum mass of rotating and nonrotating neutron stars. Our results indicate that predictions of the tidal parameter represent a useful constraint of the Equation of State (EoS) of neutron stars.