J 2020

Where is Love? Tidal deformability in the black hole compactness limit

CHIRENTI, Cecilia, Nelson Camilo POSADA AGUIRRE and Victor GUEDES

Basic information

Original name

Where is Love? Tidal deformability in the black hole compactness limit

Authors

CHIRENTI, Cecilia, Nelson Camilo POSADA AGUIRRE (170 Colombia, belonging to the institution) and Victor GUEDES

Edition

Classical and Quantum Gravity, GB - Spojené království Velké Británie a, 2020, 0264-9381

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Country of publisher

United Kingdom of Great Britain and Northern Ireland

Confidentiality degree

není předmětem státního či obchodního tajemství

References:

RIV identification code

RIV/47813059:19630/20:A0000064

Organization unit

Institute of physics in Opava

UT WoS

000570861000001

Keywords in English

compact stars; tidal deformability; gravitational waves; analytical solutions

Tags

Tags

International impact, Reviewed
Změněno: 19/4/2021 12:50, Mgr. Pavlína Jalůvková

Abstract

V originále

One of the macroscopically measurable effects of gravity is the tidal deformability of astrophysical objects, which can be quantified by their tidal Love numbers. For planets and stars, these numbers measure the resistance of their material against the tidal forces, and the resulting contribution to their gravitational multipole moments. According to general relativity, nonrotating deformed black holes, instead, show no addition to their gravitational multipole moments, and all of their Love numbers are zero. In this paper we explore different configurations of nonrotating compact and ultracompact stars to bridge the compactness gap between black holes and neutron stars and calculate their Love number k(2). We calculate k(2) for the first time for uniform density ultracompact stars with mass M and radius R beyond the Buchdahl limit (compactness M/R > 4/9), and we find that k(2) -> 0(+) as M/R -> 1/2, i.e., the Schwarzschild black hole limit. Our results provide insight on the zero tidal deformability limit and we use current constraints on the binary tidal deformability (Lambda) over tilde from GW170817 (and future upper limits from binary black hole mergers) to propose tests of alternative models.