Tidal Deformability of Compact Stars

Zhou, Enbo

doi:10.1007/978-981-15-4151-3_2

Cited by 1 publication

(2 citation statements)

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“…We used the Numpyro probabilistic programming language [93] to implement the model (16). We inferred the values of the unknown parameters in our model (α, β, s m and s b ) by running MCMC using the No-U-Turn Sampler (NUTS) [94] for 10,000 warm-up samples and then collected 1000 posterior samples to represent our model parameter's posterior distribution.…”

Section: Bayesian Power Regression Model With Heteroscedastic Errorsmentioning

confidence: 99%

“…The association of the event with an electromagnetic (EM) counterpart led to the first joint GW-EM constraints on the NS EoS. Using the binary's tidal deformability parameter, which describes how much a body is deformed by tidal forces [6,[14][15][16], simulations of EM observations within numerical relativity and Kilonova models were performed, and extreme EoS models were ruled out: the stiffest and softest ones, e.g., see Figure 2 of Ref. [2].…”

Section: Introductionmentioning

confidence: 99%

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Bayesian Exploration of Phenomenological EoS of Neutron/Hybrid Stars with Recent Observations

et al. 2023

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The description of the stellar interior of compact stars remains as a big challenge for the nuclear astrophysics community. The consolidated knowledge is restricted to density regions around the saturation of hadronic matter ρ0=2.8×1014gcm−3, regimes where our nuclear models are successfully applied. As one moves towards higher densities and extreme conditions up to the quark/gluons deconfinement, little can be said about the microphysics of the equation of state (EoS). Here, we employ a Markov Chain Monte Carlo (MCMC) strategy to access the variability at high density regions of polytropic piecewise models for neutron star (NS) EoS or possible hybrid stars, i.e., a NS with a small quark-matter core. With a fixed description of the hadronic matter for low density, below the nuclear saturation density, we explore a variety of models for the high density regimes leading to stellar masses near to 2.5M⊙, in accordance with the observations of massive pulsars. The models are constrained, including the observation of the merger of neutrons stars from VIRGO-LIGO and with the pulsar observed by NICER. In addition, we also discuss the possibility of the use of a Bayesian power regression model with heteroscedastic error. The set of EoS from the Laser Interferometer Gravitational-Wave Observatory (LIGO) was used as input and treated as the data set for the testing case.

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Section: Bayesian Power Regression Model With Heteroscedastic Errorsmentioning

confidence: 99%