Search for correlated high energy cosmic ray events with CHICOS

Carlson, B. E.; Brobeck, E.; Jillings, C.; Larson, Michelle B.; Lynn, T. W.; McKeown, R. D.; Hill, J.; Falkowski, Barbara J.; Seki, Ryoichi; Sepikas, J.; Yodh, G.

doi:10.1088/0954-3899/31/5/011

Cited by 16 publications

(14 citation statements)

References 10 publications

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“…(25)), we obtain ∆E 1S = 0.0814 − 0.0029 = 0.0785 meV (31) ∆E 2S = 0.0102 − 0.0005 = 0.0097 meV (32) (the first term is ∆E a , and the second is ∆E b ). Comparing this with the leading proton size contribution [8],…”

Section: Implications For the Proton Radius Puzzlementioning

confidence: 96%

“…[6] suggest that the meson exchange contribution strongly grows at Q 2 → 0, which may be interesting in connection with so-called "proton radius puzzle". The values of the proton charge radius, obtained from the elastic electron-proton scattering and from the measurements of the Lamb shift in muonic hydrogen, are in serious disagreement [8]. Potentially, any effect, which makes a difference between muon and electron, could be responsible for the discrepancy and should be checked; the meson exchange is one of them.…”

Section: Introductionmentioning

confidence: 99%

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Meson exchange in lepton-nucleon scattering and the proton radius puzzle

Borisyuk

2017

Phys. Rev. C

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We study two-photon contribution to the elastic lepton-proton scattering, associated with σ meson exchange, with special attention paid to the low-Q 2 region. We show that the corresponding amplitude grows sharply but remains finite at Q 2 → 0. The analytical formula for the amplitude at Q 2 = 0 is obtained. We also estimate the shift of the muonic hydrogen energy levels, induced by σ meson exchange. For the 2S level the shift is approximately 30 times smaller than needed to resolve the proton radius puzzle, but still exceeds the precision of the muonic hydrogen measurements.

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Section: Implications For the Proton Radius Puzzlementioning

confidence: 96%

Section: Introductionmentioning

confidence: 99%

Meson exchange in lepton-nucleon scattering and the proton radius puzzle

Borisyuk

2017

Phys. Rev. C

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“…Since attaining a microscopic understanding of the EoS of dense matter constitutes an important objective of nuclear science [13], there have been ongoing experimental efforts to constrain the EoS at various densities in nuclear structure and reaction experiments [14][15][16][17][18][19][20][21][22][23][24][25][26] and to describe, with various success, using ab initio [27,28], microscopic [29,30] and phenomenological [31][32][33] models. However the EoS from nuclear experiments using nuclei with similar number of neutrons and protons must be extrapolated to neutron star environments where the density of neutrons greatly exceeds the density of protons.…”

Section: Constraints From Nucleus-nucleus Collisionsmentioning

confidence: 99%

Symmetry energy constraints from GW170817 and laboratory experiments

et al. 2019

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The LIGO-Virgo collaboration detection of the binary neutron-star merger event, GW170817, has expanded efforts to understand the Equation of State (EoS) of nuclear matter. These measurements provide new constraints on the overall pressure, but do not elucidate its origins, by not distinguishing the contribution to the pressure from symmetry energy which governs much of the internal structure of a neutron star. By combining the neutron star EoS extracted from the GW170817 event and the EoS of symmetric matter from nucleus-nucleus collision experiments, we extract the symmetry pressure, which is the difference in pressure between neutron and nuclear matter over the density region from 1.20 to 4.50. While the uncertainties in the symmetry pressure are large, they can be reduced with new experimental and astrophysical results.

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“…Understanding the nature of dense nuclear matter and neutron stars is a compelling objective of nuclear science [1]. The recent observation of the neutron-star merger event,…”

Section: Introductionmentioning

confidence: 99%

Insights on Skyrme parameters from GW170817

Tsang

Danielewicz

et al. 2019

Physics Letters B

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The binary neutron-star merger event, GW170817, has cast a new light on nuclear physics research. Using a neutron-star model that includes a crust equation of state (EoS), we calculate the properties of a 1.4 solar-mass neutron star. The model incorporates more than 200 Skyrme energy density functionals, which describe nuclear matter properties, in the outer liquid core region of the neutron star. We find a power-law relation between the neutron-star tidal deformability, Λ, and the neutron-star radius, R. Without an explicit crust EoS, the model predicts smaller R and the difference becomes significant for stars with large radii. To connect the neutron star properties with nuclear matter properties, we confront the predicted values for Λ, against the Taylor expansion coefficients of the Skyrme interactions. There is no pronounced correlation between Skyrme parameters in symmetric nuclear matter and neutron star properties.However, we find the strongest correlation between Λ and Ksym, the curvature of the density dependence of the symmetry energy at saturation density. At twice the saturation density, our calculations show a strong correlation between Λ and total pressure providing guidance to laboratory nucleus-nucleus collision experiments.

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Search for correlated high energy cosmic ray events with CHICOS

Cited by 16 publications

References 10 publications

Meson exchange in lepton-nucleon scattering and the proton radius puzzle

Meson exchange in lepton-nucleon scattering and the proton radius puzzle

Symmetry energy constraints from GW170817 and laboratory experiments

Insights on Skyrme parameters from GW170817

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