4.7 Article

Bayesian Nonparametric Inference of the Neutron Star Equation of State via a Neural Network

期刊

ASTROPHYSICAL JOURNAL
卷 919, 期 1, 页码 -

出版社

IOP Publishing Ltd
DOI: 10.3847/1538-4357/ac11f8

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资金

  1. NSFC [11921003, 11525313]
  2. United States National Science Foundation (NSF)
  3. Science and Technology Facilities Council (STFC) of the United Kingdom
  4. Max Planck Society (MPS)
  5. State of Niedersachsen/Germany
  6. Australian Research Council
  7. European Gravitational Observatory (EGO)
  8. French Centre National de Recherche Scientifique (CNRS)
  9. Italian Istituto Nazionale di Fisica Nucleare (INFN)

向作者/读者索取更多资源

A new nonparametric method utilizing neural networks is developed to reconstruct the equation of state of neutron stars, successfully fitting theoretical EoS and analyzing real data to obtain posterior probabilities for radius and tidal deformability. Additionally, findings suggest the conformal limit may not always hold true in neutron stars' high-density regions.
We develop a new nonparametric method to reconstruct the equation of state (EoS) of a neutron star with multimessenger data. As a universal function approximator, the feed-forward neural network (FFNN) with one hidden layer and a sigmoidal activation function can approximately fit any continuous function. Thus, we are able to implement the nonparametric FFNN representation of the EoSs. This new representation is validated by its capability of fitting the theoretical EoSs and recovering the injected parameters. Then, we adopt this nonparametric method to analyze the real data, including the mass-tidal deformability measurement from the binary neutron star merger gravitational-wave event GW170817 and mass-radius measurement of PSR J0030+0451 by NICER. We take the publicly available samples to construct the likelihood and use the nested sampling to obtain the posteriors of the parameters of the FFNN according to the Bayesian theorem, which in turn can be translated to the posteriors of the EoS parameters. Combining all of these data for a canonical 1.4 M-circle dot neutron star, we get a radius R-1.4 = 11.83(-1.08)(+1.25) km and tidal deformability Lambda(1.4) = 323(-165)(+334) (90% confidence interval). Furthermore, we find that in the high-density region (>= 3 rho(sat)), the 90% lower limits of c(s)(2)/c(2) (where c(s) is the sound speed and c is the velocity of light in vacuum) are above 1/3, which means that the so-called conformal limit (i.e., c(s)(2)/c(2) < 1/3) is not always valid in the neutron stars.

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