Effective field theory with genuine many-body forces and tidal effects on neutron stars

被引：0

作者：

Razeira, M. ^{[1
]}

Hadjimichef, D. ^{[2
]}

Machado, M. V. T. ^{[2
]}

Kopp, F. ^{[2
]}

Volkmer, G. ^{[2
]}

Bodmann, B. ^{[2
,3
]}

Degrazia, G. A. ^{[3
]}

Vasconcellos, C. A. Z. ^{[2
]}

机构：

[1] Univ Fed Pampa UNIPAMPA, Phys Dept, Cacapava Do Sul, Brazil

[2] Univ Fed Rio Grande do Sul, Phys Dept, Porto Alegre, RS, Brazil

[3] Univ Fed Santa Maria, Phys Dept, Santa Maria, RS, Brazil

来源：

ASTRONOMISCHE NACHRICHTEN | 2019年 / 340卷 / 1-3期

关键词：

gravitational waves; neutron stars; tidal parameter;

D O I：

10.1002/asna.201913590

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 the neutron star undergoes a deformation measured in terms of the ratio between the quadrupole moment induced in the star and the field , 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.

引用

页码：209 / 212

页数：4

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