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dc.contributor.author
B.P. Abbott et al.
dc.contributor.author
강궁원
dc.contributor.author
배상욱
dc.date.accessioned
2019-08-28T07:42:18Z
dc.date.available
2019-08-28T07:42:18Z
dc.date.issued
2018-10-15
dc.identifier.issn
0031-9007
dc.identifier.uri
https://repository.kisti.re.kr/handle/10580/14779
dc.identifier.uri
http://www.ndsl.kr/ndsl/search/detail/article/articleSearchResultDetail.do?cn=NART90642184
dc.description.abstract
On 17 August 2017, the LIGO and Virgo observatories made the first direct detection of gravitational
waves from the coalescence of a neutron star binary system. The detection of this gravitational-wave signal,
GW170817, offers a novel opportunity to directly probe the properties of matter at the extreme conditions
found in the interior of these stars. The initial, minimal-assumption analysis of the LIGO and Virgo data
placed constraints on the tidal effects of the coalescing bodies, which were then translated to constraints on
neutron star radii. Here, we expand upon previous analyses by working under the hypothesis that both bodies
were neutron stars that are described by the same equation of state and have spins within the range observed in
Galactic binary neutron stars. Our analysis employs two methods: the use of equation-of-state-insensitive
relations between various macroscopic properties of the neutron stars and the use of an efficient
parametrization of the defining function pðρÞ of the equation of state itself. From the LIGO and Virgo
data alone and the first method, we measure the two neutron star radii as R1
¼ 10.8
þ2.0
−1.7 km for the heavier
star and R2
¼ 10.7
þ2.1
−1.5 km for the lighter star at the 90% credible level. If we additionally require that the
equation of state supports neutron stars with masses larger than 1.97 M⊙ as required from electromagnetic
observations and employ the equation-of-state parametrization, we further constrain R1
¼ 11.9
þ1.4
−1.4 km and
R2
¼ 11.9
þ1.4
−1.4 km at the 90% credible level. Finally, we obtain constraints on pðρÞ at supranuclear densities,
with pressure at twice nuclear saturation density measured at 3.5
þ2.7
−1.7 × 1034 dyn cm−2 at the 90% level.
dc.language
eng
dc.relation.ispartofseries
PHYSICAL REVIEW LETTERS
dc.title
GW170817: Measurements of Neutron Star Radii and Equation of State
dc.citation.number
16
dc.citation.startPage
091102
dc.citation.volume
121
dc.subject.keyword
GW170817
dc.subject.keyword
Neutro star
dc.subject.keyword
Equation of state
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