Constraining the dense matter equation of state with new NICER mass-radius measurements and new chiral effective field theory inputs - Archive ouverte HAL Accéder directement au contenu
Article Dans Une Revue Astrophys.J.Lett. Année : 2024

Constraining the dense matter equation of state with new NICER mass-radius measurements and new chiral effective field theory inputs

Nathan Rutherford
  • Fonction : Auteur
Melissa Mendes
  • Fonction : Auteur
Isak Svensson
  • Fonction : Auteur
Achim Schwenk
  • Fonction : Auteur
Anna L Watts
  • Fonction : Auteur
Kai Hebeler
  • Fonction : Auteur
Jonas Keller
  • Fonction : Auteur
Chanda Prescod-Weinstein
  • Fonction : Auteur
Devarshi Choudhury
  • Fonction : Auteur
Geert Raaijmakers
  • Fonction : Auteur
Tuomo Salmi
  • Fonction : Auteur
Patrick Timmerman
  • Fonction : Auteur
Serena Vinciguerra
  • Fonction : Auteur
James M Lattimer
  • Fonction : Auteur

Résumé

Pulse profile modeling of X-ray data from NICER is now enabling precision inference of neutron star mass and radius. Combined with nuclear physics constraints from chiral effective field theory ($\chi$EFT), and masses and tidal deformabilities inferred from gravitational wave detections of binary neutron star mergers, this has lead to a steady improvement in our understanding of the dense matter equation of state (EOS). Here we consider the impact of several new results: the radius measurement for the 1.42$\,M_\odot$ pulsar PSR J0437$-$4715 presented by Choudhury et al. (2024), updates to the masses and radii of PSR J0740$+$6620 and PSR J0030$+$0451, and new $\chi$EFT results for neutron star matter up to 1.5 times nuclear saturation density. Using two different high-density EOS extensions -- a piecewise-polytropic (PP) model and a model based on the speed of sound in a neutron star (CS) -- we find the radius of a 1.4$\,M_\odot$ (2.0$\,M_\odot$) neutron star to be constrained to the 95% credible ranges $12.28^{+0.50}_{-0.76}\,$km ($12.33^{+0.70}_{-1.34}\,$km) for the PP model and $12.01^{+0.56}_{-0.75}\,$km ($11.55^{+0.94}_{-1.09}\,$km) for the CS model. The maximum neutron star mass is predicted to be $2.15^{+0.14}_{-0.16}\,$$M_\odot$ and $2.08^{+0.28}_{-0.16}\,$$M_\odot$ for the PP and CS model, respectively. We explore the sensitivity of our results to different orders and different densities up to which $\chi$EFT is used, and show how the astrophysical observations provide constraints for the pressure at intermediate densities. Moreover, we investigate the difference $R_{2.0} - R_{1.4}$ of the radius of 2$\,M_\odot$ and 1.4$\,M_\odot$ neutron stars within our EOS inference.
Fichier principal
Vignette du fichier
Rutherford_2024_ApJL_971_L19.pdf (1.84 Mo) Télécharger le fichier
Origine Fichiers éditeurs autorisés sur une archive ouverte

Dates et versions

hal-04644848 , version 1 (30-08-2024)

Licence

Identifiants

Citer

Nathan Rutherford, Melissa Mendes, Isak Svensson, Achim Schwenk, Anna L Watts, et al.. Constraining the dense matter equation of state with new NICER mass-radius measurements and new chiral effective field theory inputs. Astrophys.J.Lett., 2024, 971 (1), pp.L19. ⟨10.3847/2041-8213/ad5f02⟩. ⟨hal-04644848⟩
13 Consultations
0 Téléchargements

Altmetric

Partager

Gmail Mastodon Facebook X LinkedIn More