Nuclear Pairing Gaps and Neutron Star Cooling

Wei, Jin-Biao; Burgio, G. F.; Schulze, H.-J.

doi:10.3390/universe6080115

Cited by 10 publications

(5 citation statements)

References 83 publications

(134 reference statements)

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“…We notice that the proton fraction with the V18 EOS is relatively large, and at T = 0 it exceeds at relatively low density ∼ 0.37 fm −3 the threshold value x DU ≈ 0.13 for the opening of the direct Urca cooling reactions [23,92]. Therefore mediummass NSs can cool down very rapidly, in agreement with NS mass distributions, as illustrated in our recent works [93][94][95].…”

Section: Resultssupporting

confidence: 83%

Microscopic nuclear equation of state at finite temperature and stellar stability

Li¹,

Zhang²,

Li³

et al. 2022

Preprint

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Section: Resultssupporting

confidence: 83%

Microscopic nuclear equation of state at finite temperature and stellar stability

Li¹,

Zhang²,

Li³

et al. 2022

Preprint

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“…In fact, the constraints on neutron star thermal evolution -or more specifically the cooling speed -were also recently taken into account in Refs. [191] and [192], while in [193,194] the effects of three-body forces were taken into account in BHF theory at finite temperature. Finally, we note that a complete treatment of Fock terms within the QMC model at finite temperature has recently been reported by Stone and collaborators [97].…”

Section: Many-body Forcesmentioning

confidence: 99%

The Role of Baryon Structure in Neutron Stars

Motta,

Thomas

2022

Preprint

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The current state of neutron star mass measurements is depicted in Fig. 1. We see that the only measurements of heavy neutron stars with reasonably small errors are those of PSR J1614-2230 [29] and PSR J0348+0432 [2], along with PSR J0740+6620 [30] which is the newest member of the heavy neutron star club. Nevertheless, the uncertainties on the aforementioned pulsars still make them all comparable with each other within two standard deviations. Therefore, a conservative lower estimate for the maximum mass of neutron stars is that of PSR J1614-2230, namely, 1.908±0.016M . RadiiOther than their masses, the radii of neutron stars are extremely sensitive to different models for the equations of state. However, the experimental constraints on radii are less numerous and until recently the systematic errors were quite large. The first new source of a constraint came on August 17th 2017, with the first gravitational wave measurement [4] of the merger of two neutron stars. This yielded the result that the radii of the neutron stars involved in the merger both lie within R = 11.9 +1.4 −1.4 , at the 90% confidence level.More recently, the NICER mission, with its X-ray telescope on the space station, obtained results [5,37] for PSR J0030+0451. The collaboration applied different analyses on the data and obtained values of (all at 68% credibility) 12.71 +1.14 −1.19 km and mass 1.34 +0.15 −0.16 M in Ref.[5] and 13.02 +1.24 −1.06 km in Ref.[37] with the mass estimated at 1.44 +0.15 −0.14 M . Another recent measurement by the NICER collaboration was that of pulsar PSR J0740+6620 which by virtue of being much heavier, is of considerable interest to nuclear physicists. They measured a radius of 12.39 +1.3 −0.98 km for a mass of 2.07 ± 0.06M [38]. Modelling Dense MatterHistorically, studies of the properties of nuclear matter were primarily aimed at understanding finite nuclei. They were based primarily on using two-body and three-body potentials with standard techniques in quantum many-body theory, such as Brueckner-Hartree-Fock (BHF) [39], Bethe-Brueckner-Goldstone (BBG) [40]. The two-body potentials were derived from phenomenological fits to nucleonnucleon scattering [41]. The quantum Monte Carlo variational approach has had considerable success with light nuclei [42], with parameters of the phenomenological three-body force tuned to nuclear data. In recent years there has been a great deal of activity using chiral effective field theory [43,44,45,46,47,48], with its systematic expansion in powers of momentum. This approach builds in the constraints of chiral symmetry within a Lagrangian theory built upon pion and nucleon degrees of freedom, plus counterterms. With a similar number of parameters to those needed for phenomenological potentials (typically 25-30), it yields a good description of nucleon-nucleon scattering data. Within the same framework, one also has a systematic expansion of a three-nucleon force, with counterterms again tuned to nuclear data. Once again one finds excellent agreement with data for light nuc...

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“…Today, the presence of superfluidity in NSs is a widely accepted fact (for a more detailed account on the history of NSs, see Refs. [2,10], as well as other contributions to this special issue [11][12][13]).…”

Section: Introductionmentioning

confidence: 99%

Superfluid Neutron Matter with a Twist

Palkanoglou

Gezerlis

2021

Universe

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Superfluid neutron matter is a key ingredient in the composition of neutron stars. The physics of the inner crust are largely dependent on those of its S-wave neutron superfluid, which has made its presence known through pulsar glitches and modifications in neutron star cooling. Moreover, with recent gravitational-wave observations of neutron star mergers, the need for an equation of state for the matter of these compact stars is further accentuated and a model-independent treatment of neutron superfluidity is important. Ab initio techniques developed for finite systems can be guided to perform extrapolations to the thermodynamic limit and attain this model-independent extraction of various quantities of infinite superfluid neutron matter. To inform such an extrapolation scheme, we performed calculations of the neutron 1S0 pairing gap using model-independent odd–even staggering in the context of the particle-conserving, projected Bardeen–Cooper–Schrieffer (BCS) theory under twisted boundary conditions. While the practice of twisted boundary conditions is standard in solid-state physics and has been used repeatedly in the past to reduce finite-size effects, this is the first time that it has been employed in the context of pairing. We find that a twist-averaging approach results in a substantial reduction of the finite-size effects, bringing systems with N⪆50 within a 2% error margin from the infinite system. This can significantly reduce extrapolation-related errors in the extraction of superfluid neutron matter quantities.

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Nuclear Pairing Gaps and Neutron Star Cooling

Cited by 10 publications

References 83 publications

Microscopic nuclear equation of state at finite temperature and stellar stability

Microscopic nuclear equation of state at finite temperature and stellar stability

The Role of Baryon Structure in Neutron Stars

Superfluid Neutron Matter with a Twist

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