Precision Determination of the Neutral Weak Form Factor of 
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Adhikari, Dinesh; Al-Bataineh, H.; Androić, D.; Aniol, K.; Armstrong, David; Averett, T.; Gayoso, C. Ayerbe; Barcus, S.; Bellini, V.; Beminiwattha, R.; Benesch, J.; Bhatt, H.; Pathak, D. Bhatta; Bhetuwal, D.; Blaikie, B.; Boyd, James E.; Campagna, Quinn; Camsonne, A.; Cates, G. D.; Chen, Y.; Clarke, C.; Cornejo, J. C.; Dusa, S. Covrig; Dalton, M. M.; Datta, P.; Deshpande, A.; Dutta, D.; Feldman, Charles; Fuchey, E.; Gal, C.; Gaskell, D.; Gautam, T.; Gericke, Michael; Ghosh, C.; Halilovic, I.; Hansen, J. O.; Hassan, O.; Hauenstein, F.; Henry, W.; Horowitz, C. J.; Jantzi, Christopher; Jian, Siyu; Johnston, S.; Jones, D.; Kakkar, S.; Katugampola, Sumudu; Keppel, C. E.; P, King; King, David E.; Kumar, Krishna; Kutz, T.; Lashley-Colthirst, N.; Leverick, Graham; Liu, H.; Liyanage, N.; Mammei, J.; Mammei, R.; McCaughan, M.; McNulty, D.; Meekins, D.; Metts, C.; Michaels, R.; Mihovilovič, M.; Mondal, M. M.; Napolitano, J.; Narayan, A.; Nikolaev, D.; Owen, V.; Palatchi, C.; Pan, Jie; Pandey, B.; Park, S.; Paschke, K.; Petrusky, M.; Pitt, M.; Premathilake, S.; Quinn, B.; Radloff, Robert; Rahman, Sakib; Rashad, M. N. H.; Rathnayake, A.; Reed, Brendan; Reimer, P. E.; Richards, R. K.; Riordan, S.; Roblin, Y.; Seeds, S.; Shahinyan, A.; Souder, P. A.; Thiel, M.; Tian, Ye; Urciuoli, G. M.; Wertz, E. W.; Wojtsekhowski, B.; Yale, B.; Ye, T.; Yoon, A. S.; Xiong, Weizhi; Zec, A.; Zhang, W.; Zhang, J.; Zheng, X.

doi:10.1103/physrevlett.129.042501

Cited by 130 publications

(30 citation statements)

References 74 publications

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“…In the case of 48 Ca, the softening of the symmetry energy post-refinement moves the theoretical prediction in the direction of the experiment, but not nearly as much as it is required. That is, the neutron skin thickness of 48 Ca, goes down from R 48 skin = 0.231 fm to R 48 skin = 0.197 fm, which remains far from the quoted CREX value of R 48 skin = 0.121 (35) fm [25]. It is important to note that after refinement the theoretical uncertainty in both R 208 skin and R 48 skin is significantly reduced.…”

Section: Neutron Skinsmentioning

confidence: 75%

“…However, this correlation is in stark disagreement with experiment. The CREX collaboration has recently reported a neutron skin thickness in 48 Ca [25] that is significantly smaller than any theoretical prediction that reproduces the large value of the neutron skin in 208 Pb. Finally, the historic detection of gravitational waves by the LIGO-Virgo collaboration from the binary neutron star coalescence GW170817 suggests that the EOS is soft in the vicinity of 2ρ 0 [16], although a reanalysis [26] could accommodate a stiffer EOS that brings the radius of a 1.4 M neutron star into agreement with the NICER results [17,18] and with other constraints obtained from the analysis of the electromagnetic counterpart [27].…”

Section: Introductionmentioning

confidence: 83%

“…Given the strong correlation between L and the neutron skin thickness of 208 Pb [67][68][69][70], we expect that the significant lower value of L obtained after refinement will be in conflict with the PREX measurement [12], which instead favors a fairly stiff symmetry energy [13]. Indeed, an interesting tension has emerged when confronting the PREX [12] and CREX [25] measurements. Whereas the extracted neutron skin in 208 Pb is thick, CREX reported a very thin neutron skin in 48 Ca; see Table IV.…”

Section: Neutron Skinsmentioning

confidence: 99%

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Bayesian refinement of covariant energy density functionals

Salinas¹,

Piekarewicz²

2023

Preprint

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The last five years have seen remarkable progress in our quest to determine the equation of state of neutron rich matter. Recent advances across the theoretical, experimental, and observational landscape have been incorporated in a Bayesian framework to refine existing covariant energy density functionals previously calibrated by the properties of finite nuclei. In particular, constraints on the maximum neutron star mass from pulsar timing, on stellar radii from the NICER mission, on tidal deformabilities from the LIGO-Virgo collaboration, and on the dynamics of pure neutron matter as predicted from chiral effective field theories, have resulted in significant refinements to the models, particularly to those predicting a stiff symmetry energy. Still, even after these improvements, we find challenging to reproduce simultaneously the neutron skin thickness of both 208 Pb and 48 Ca recently reported by the PREX/CREX collaboration.

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Section: Neutron Skinsmentioning

confidence: 75%

Section: Introductionmentioning

confidence: 83%

Section: Neutron Skinsmentioning

confidence: 99%

See 1 more Smart Citation

Bayesian refinement of covariant energy density functionals

Salinas¹,

Piekarewicz²

2023

Preprint

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show abstract

“…Nevertheless, considering the large deviation in the L 0 distribution from PREX-II, different analyses from laboratory experiments and astrophysical data could be compatible with each other. For example, the joint analysis of PREX-II and the more recent CREX (Adhikari et al 2022) Figure 4 compares and contrasts the 90% confidence intervals of the EOSs for all the analyses. The contour of the GW170817/AT2017gfo + NICER analysis is denoted by the green-shaded region, while the other contours are denoted by the dashed lines.…”

Section: Parameters Of the Nuclear Eos And The Properties Of The Neut...mentioning

confidence: 99%

A Bayesian Inference of a Relativistic Mean-field Model of Neutron Star Matter from Observations of NICER and GW170817/AT2017gfo

Zhu

Liu

2023

ApJ

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Observations of optical and near-infrared counterparts of binary neutron star mergers not only enrich our knowledge about the abundance of heavy elements in the universe and help reveal the remnant object just after the merger, which is generally known, but can also effectively constrain the dense properties of the nuclear matter and the equation of state (EOS) in the interior of the merging stars. Following the relativistic mean-field description of nuclear matter, we perform a Bayesian inference of the EOS and the properties of the nuclear matter using the first multi-messenger event GW170817/AT2017gfo, together with the NICER mass–radius measurements of pulsars. The kilonova is described by a radiation-transfer model with the dynamical ejecta, and light curves connect with the EOS through the quasi-universal relations between the properties of the ejecta (the ejected mass, velocity, opacity, or electron fraction) and binary parameters (the mass ratio and reduced tidal deformability). It is found that the posterior distributions of the reduced tidal deformability from the AT2017gfo analysis display a bimodal structure, with the first peak enhanced by the GW170817 data, leading to slightly softened posterior EOSs, while the second peak cannot be achieved by a nuclear EOS with saturation properties in their empirical ranges. The inclusion of NICER data results in a stiffened EOS posterior because of the massive pulsar PSR J0740+6620. We provide the results at nuclear saturation density for the nuclear incompressibility, the symmetry energy, and its slope, as well as the nucleon effective mass, from our analysis of the observational data.

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“…combining the original Lead Radius EXperiment (PREX) result with the updated PREX2 result [2][3][4]. As for 48 Ca, the CREX group presented [5] r 48 skin (CREX) = 0.121 ± 0.026 (exp) ± 0.024 (model) = 0.071 ∼ 0.171 fm.…”

mentioning

confidence: 99%