Gravitational-wave constraints on the neutron-star-matter Equation of State - INSPIRE

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Gravitational-wave constraints on the neutron-star-matter Equation of State

Eemeli Annala
(
- Helsinki U. and
- Helsinki Inst. of Phys.
)
,
Tyler Gorda
(
- Helsinki U. and
- Helsinki Inst. of Phys.
)
,
Aleksi Kurkela
(
- CERN and
- Stavanger U.
)
,
Aleksi Vuorinen
(
- Helsinki U. and
- Helsinki Inst. of Phys.
)

Nov 7, 2017

5 pages

Published in:

Phys.Rev.Lett. 120 (2018) 17, 172703

Published: Apr 26, 2018

e-Print:

1711.02644 [astro-ph.HE]

DOI:

10.1103/PhysRevLett.120.172703

Report number:

CERN-TH-2017-236

View in:

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Abstract: (APS)

The detection of gravitational waves originating from a neutron-star merger, GW170817, by the LIGO and Virgo Collaborations has recently provided new stringent limits on the tidal deformabilities of the stars involved in the collision. Combining this measurement with the existence of two-solar-mass stars, we generate a generic family of neutron-star-matter equations of state (EOSs) that interpolate between state-of-the-art theoretical results at low and high baryon density. Comparing the results to ones obtained without the tidal-deformability constraint, we witness a dramatic reduction in the family of allowed EOSs. Based on our analysis, we conclude that the maximal radius of a 1.4-solar-mass neutron star is 13.6 km, and that the smallest allowed tidal deformability of a similar-mass star is Λ(1.4 M⊙)=120.

Note:

6 pages, 4 figures; v2: results and discussion updated, version accepted to PRL

star: mass
baryon: density: high
gravitational radiation
gravitational radiation: emission
gravitational radiation detector
gravitational radiation: direct detection
equation of state
numerical methods
data analysis method
neutron star

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Figures(4)

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