Bayesian inference of nuclear symmetry energy from measured and imagined neutron skin thickness in , and
Abstract
The neutron skin thickness Δrnp in heavy nuclei has been known as one of the most sensitive terrestrial probes of the nuclear symmetry energy Esym(ρ) around $$\frac{2}{3}$$ of the saturation density ρ0 of nuclear matter. Existing neutron skin data mostly from hadronic observables suffer from large uncertainties and their extraction from experiments are often strongly model dependent. While waiting eagerly for the promised model-independent and high-precision neutron skin data for 208Pb and 48Ca from the parity-violating electron scattering experiments (PREX-II and CREX at JLab as well as MREX at MESA), within the Bayesian statistical framework using the Skyrme-Hartree-Fock model we infer the posterior probability distribution functions (PDFs) of the slope parameter L of the nuclear symmetry energy at ρ0 from imagined Δrnp(208Pb)=0.15, 0.20, and 0.30 fm with a 1σ error bar of 0.02, 0.04, and 0.06 fm, respectively, as well as Δrnp(48Ca)=0.12, 0.15, and 0.25 fm, with different 1σ error bar of 0.01 and 0.02 fm, respectively. The results are compared with the PDFs of L inferred using the same approach from the available Δrnp data for 116, 118, 120, 122, 124, 130, 132Sn from hadronic probes. They are also compared with results from a recent Bayesian analysis of the radius and tidal deformability data of canonical neutron stars from GW170817 and NICER. The neutron skin data for Sn isotopes gives L = 45.5 $$^{+ 26.5}_{-21.6}$$ MeV surrounding its mean value or L = 53 . 4 $$^{+ 18.6}_{ -29.5}$$ MeV surrounding its maximum a posteriori value, respectively, with the latter smaller than but consistent with the L = 66 $$^{+ 12}_{-20}$$ MeV from the neutron star data within their 68% confidence intervals. We found that Δrnp = 0.17 –0.18 fm in 208Pb with an error bar of about 0.02 fm leads to a PDF of L compatible with that from analyzing the Sn data. To provide additionally useful information on L extracted from the Δrnp of Sn isotopes, the experimental error bar of Δrnp in 208Pb should be at least smaller than 0.06 fm aimed by some current experiments. In addition, the Δrnp (48Ca) needs to be larger than 0.15 fm but smaller than 0.25 fm to be compatible with the Sn and/or neutron star results. To further improve our current knowledge about L and distinguish its PDFs in the examples considered, even higher precisions leading to significantly less than ±20 MeV error bars for L at 68% confidence level are necessary.
- Authors:
-
- Chinese Academy of Sciences (CAS), Shanghai (China)
- Yuncheng University (China)
- Texas A & M Univ., Commerce, TX (United States)
- Publication Date:
- Research Org.:
- Texas A & M Univ., Commerce, TX (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC); National Natural Science Foundation of China (NSFC)
- OSTI Identifier:
- 1837897
- Grant/Contract Number:
- SC0013702; SC0009971
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Physical Review C
- Additional Journal Information:
- Journal Volume: 102; Journal Issue: 4; Journal ID: ISSN 2469-9985
- Publisher:
- American Physical Society (APS)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 73 NUCLEAR PHYSICS AND RADIATION PHYSICS
Citation Formats
Xu, Jun, Xie, Wen-Jie, and Li, Bao-An. Bayesian inference of nuclear symmetry energy from measured and imagined neutron skin thickness in Sn 116 , 118 , 120 , 122 , 124 , 130 , 132 , Pb 208 , and Ca 48. United States: N. p., 2020.
Web. doi:10.1103/physrevc.102.044316.
Xu, Jun, Xie, Wen-Jie, & Li, Bao-An. Bayesian inference of nuclear symmetry energy from measured and imagined neutron skin thickness in Sn 116 , 118 , 120 , 122 , 124 , 130 , 132 , Pb 208 , and Ca 48. United States. https://doi.org/10.1103/physrevc.102.044316
Xu, Jun, Xie, Wen-Jie, and Li, Bao-An. Wed .
"Bayesian inference of nuclear symmetry energy from measured and imagined neutron skin thickness in Sn 116 , 118 , 120 , 122 , 124 , 130 , 132 , Pb 208 , and Ca 48". United States. https://doi.org/10.1103/physrevc.102.044316. https://www.osti.gov/servlets/purl/1837897.
@article{osti_1837897,
title = {Bayesian inference of nuclear symmetry energy from measured and imagined neutron skin thickness in Sn 116 , 118 , 120 , 122 , 124 , 130 , 132 , Pb 208 , and Ca 48},
author = {Xu, Jun and Xie, Wen-Jie and Li, Bao-An},
abstractNote = {The neutron skin thickness Δrnp in heavy nuclei has been known as one of the most sensitive terrestrial probes of the nuclear symmetry energy Esym(ρ) around $\frac{2}{3}$ of the saturation density ρ0 of nuclear matter. Existing neutron skin data mostly from hadronic observables suffer from large uncertainties and their extraction from experiments are often strongly model dependent. While waiting eagerly for the promised model-independent and high-precision neutron skin data for 208Pb and 48Ca from the parity-violating electron scattering experiments (PREX-II and CREX at JLab as well as MREX at MESA), within the Bayesian statistical framework using the Skyrme-Hartree-Fock model we infer the posterior probability distribution functions (PDFs) of the slope parameter L of the nuclear symmetry energy at ρ0 from imagined Δrnp(208Pb)=0.15, 0.20, and 0.30 fm with a 1σ error bar of 0.02, 0.04, and 0.06 fm, respectively, as well as Δrnp(48Ca)=0.12, 0.15, and 0.25 fm, with different 1σ error bar of 0.01 and 0.02 fm, respectively. The results are compared with the PDFs of L inferred using the same approach from the available Δrnp data for 116, 118, 120, 122, 124, 130, 132Sn from hadronic probes. They are also compared with results from a recent Bayesian analysis of the radius and tidal deformability data of canonical neutron stars from GW170817 and NICER. The neutron skin data for Sn isotopes gives L = 45.5 $^{+ 26.5}_{-21.6}$ MeV surrounding its mean value or L = 53 . 4 $^{+ 18.6}_{ -29.5}$ MeV surrounding its maximum a posteriori value, respectively, with the latter smaller than but consistent with the L = 66 $^{+ 12}_{-20}$ MeV from the neutron star data within their 68% confidence intervals. We found that Δrnp = 0.17 –0.18 fm in 208Pb with an error bar of about 0.02 fm leads to a PDF of L compatible with that from analyzing the Sn data. To provide additionally useful information on L extracted from the Δrnp of Sn isotopes, the experimental error bar of Δrnp in 208Pb should be at least smaller than 0.06 fm aimed by some current experiments. In addition, the Δrnp (48Ca) needs to be larger than 0.15 fm but smaller than 0.25 fm to be compatible with the Sn and/or neutron star results. To further improve our current knowledge about L and distinguish its PDFs in the examples considered, even higher precisions leading to significantly less than ±20 MeV error bars for L at 68% confidence level are necessary.},
doi = {10.1103/physrevc.102.044316},
journal = {Physical Review C},
number = 4,
volume = 102,
place = {United States},
year = {Wed Oct 14 00:00:00 EDT 2020},
month = {Wed Oct 14 00:00:00 EDT 2020}
}
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