E. T. A. Hoffmann's Musical Aesthetics. By Abigail Chantler.

Neutron star radii, deformabilities, and moments of inertia from experimental and ab initio theory constraints on the 208Pb neutron skin thickness

“…4 13.5 km on the radius of 1.4 M neutron stars [5,16,33]. More direct measurements of neutron star radii from x-ray pulse profiling [6][7][8][9] are consistent with inferences from GW170817, but statistically favor somewhat larger radii. In the case of the NICER x-ray measurements of PSR J0030+0451, two independent analyses found M = 1.44 +0.15 −0.14 M and R = 13.02 +1.…”

“…[22], the ab initio neutron skin thickness prediction from Ref. [24], the neutron star tidal deformability constraints from GW170817 [5], the simultaneous mass-radius measurement of PSR J0030+0451 [6,7], and the NICER-XMM radius measurement of PSR J0740+6620 [8,9].…”

“…Since the EDF employed in this work determines the tidal deformability Λ, it is not necessary to perform the Λ 1 and Λ 2 integrals. The results from NICER I [6,7] and NICER II [8,9] provide posterior samples from the joint mass-radius distribution f (M, R) that enters in the likelihood: (15) where M max stands for the maximum mass of a neutron star for a given EOS. We set the starting mass M start of a neutron star for the integration as 1M , since the mass distribution of observed neutron stars has no weight below this value.…”

“…Neutron stars have attracted a great deal of attention in recent years as new measurements of masses from radio pulsar timing [1][2][3], tidal deformabilities from gravitational wave analyses [4,5], and radii from x-ray pulse profiling [6][7][8][9] have begun to clarify the possible existence of novel states of matter in the dense inner cores of the heaviest neutron stars and the equation of state of dense matter [10][11][12]. At the same time, progress in nuclear effective field theories [13,14] have enabled similarly strong constraints [12,[15][16][17][18][19][20][21] on the dense matter equation of state and bulk properties of typical 1.4 M neutron stars.…”

“…The radius of this 2.08 M neutron star is predicted to be R 2.08 = 13.7 +2.6 −1.5 km from Miller et al [8] and R 2.08 = 12.39 +1. 30 −0.98 km from Riely et al [9]. One possibility to infer the existence of a phase transition at high density from radius measurements is to search for so called "twin stars", that is, two neutron stars with similar gravitational mass but different radii, which would provide strong evidence for a third stable branch of cold dense stars (after white dwarfs and neutron stars) [34].…”