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

@article{49285,
   author = {Chirenti, Cecilia and Posada Aguirre, Nelson Camilo and Guedes, Victor},
   article_location = {GB - Spojené království Velké Británie a},
   article_number = {19},
   doi = {http://dx.doi.org/10.1088/1361-6382/abb07a},
   keywords = {compact stars; tidal deformability; gravitational waves; analytical solutions},
   language = {eng},
   issn = {0264-9381},
   journal = {Classical and Quantum Gravity},
   title = {Where is Love? Tidal deformability in the black hole compactness limit},
   url = {https://iopscience.iop.org/article/10.1088/1361-6382/abb07a},
   volume = {37},
   year = {2020}
}

TY  - JOUR
ID  - 49285
AU  - Chirenti, Cecilia - Posada Aguirre, Nelson Camilo - Guedes, Victor
PY  - 2020
TI  - Where is Love? Tidal deformability in the black hole compactness limit
JF  - Classical and Quantum Gravity
VL  - 37
IS  - 19
SP  - "195017-1"-"195017-15"
EP  - "195017-1"-"195017-15"
SN  - 02649381
KW  - compact stars
KW  - tidal deformability
KW  - gravitational waves
KW  - analytical solutions
UR  - https://iopscience.iop.org/article/10.1088/1361-6382/abb07a
N2  - 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.
ER  - 

CHIRENTI, Cecilia, Nelson Camilo POSADA AGUIRRE a Victor GUEDES. Where is Love? Tidal deformability in the black hole compactness limit. \textit{Classical and Quantum Gravity}. GB - Spojené království Velké Británie a, 2020, roč.~37, č.~19, s.~''195017-1''-''195017-15'', 15 s. ISSN~0264-9381. Dostupné z: https://dx.doi.org/10.1088/1361-6382/abb07a.