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1. Strong enhancement of electromagnetic shower development induced by high-energy photons in a thick oriented tungsten crystal

   https://doi.org/10.1140/epjc/s10052-023-11247-x  

   Soldani, M. ; Bandiera, L. ; Moulson, M. ; Ballerini, G. ; Baryshevsky, V. G. ; Bomben, L. ; Brizzolari, C. ; Charitonidis, N. ; D’Alessandro, G. L. ; De Salvador, D. ; et al ( January 2023 , The European Physical Journal C)

   We have observed a significant enhancement in the energy deposition by 25–$$100~\textrm{GeV}$$$100\text{GeV}$photons in a$$1~\textrm{cm}$$$1\text{cm}$thick tungsten crystal oriented along its$$\langle 111 \rangle $$$⟨111⟩$lattice axes. At$$100~\textrm{GeV}$$$100\text{GeV}$, this enhancement, with respect to the value observed without axial alignment, is more than twofold. This effect, together with the measured huge increase in secondary particle generation is ascribed to the acceleration of the electromagnetic shower development by the strong axial electric field. The experimental results have been critically compared with a newly developed Monte Carlo adapted for use with crystals of multi-$$X_0$$$X_0$thickness. The results presented in this paper may prove to be of significant interest for the development of high-performance photon absorbers and highly compact electromagnetic calorimeters and beam dumps for use at the energy and intensity frontiers.

    

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2. On the rigorous derivation of the incompressible Euler equation from Newton’s second law

   https://doi.org/10.1007/s11005-023-01630-w  

   Rosenzweig, Matthew ( January 2023 , Letters in Mathematical Physics)

   A long-standing problem in mathematical physics is the rigorous derivation of the incompressible Euler equation from Newtonian mechanics. Recently, Han-Kwan and Iacobelli (Proc Am Math Soc 149:3045–3061, 2021) showed that in the monokinetic regime, one can directly obtain the Euler equation from a system ofNparticles interacting in$${\mathbb {T}}^d$$$T^d$,$$d\ge 2$$$d\ge 2$, via Newton’s second law through asupercritical mean-field limit. Namely, the coupling constant$$\lambda $$$\lambda$in front of the pair potential, which is Coulombic, scales like$$N^{-\theta }$$$N^{-\theta }$for some$$\theta \in (0,1)$$$\theta \in (0,1)$, in contrast to the usual mean-field scaling$$\lambda \sim N^{-1}$$$\lambda \sim N^{-1}$. Assuming$$\theta \in (1-\frac{2}{d(d+1)},1)$$$\theta \in (1-\frac{2}{d(d+1)},1)$, they showed that the empirical measure of the system is effectively described by the solution to the Euler equation as$$N\rightarrow \infty $$$N\to \infty$. Han-Kwan and Iacobelli asked if their range for$$\theta $$$\theta$was optimal. We answer this question in the negative by showing the validity of the incompressible Euler equation in the limit$$N\rightarrow \infty $$$N\to \infty$for$$\theta \in (1-\frac{2}{d},1)$$$\theta \in (1-\frac{2}{d},1)$. Our proof is based on Serfaty’s modulated-energy method, but compared to that of Han-Kwan and Iacobelli, crucially uses an improved “renormalized commutator” estimate to obtain the larger range for$$\theta $$$\theta$. Additionally, we show that for$$\theta \le 1-\frac{2}{d}$$$\theta \le 1-\frac{2}{d}$, one cannot, in general, expect convergence in the modulated energy notion of distance.

    

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3. Inferring the Energy and Distance Distributions of Fast Radio Bursts Using the First CHIME/FRB Catalog

   https://doi.org/10.3847/1538-4357/acaf06  

   Shin, Kaitlyn ; Masui, Kiyoshi W. ; Bhardwaj, Mohit ; Cassanelli, Tomas ; Chawla, Pragya ; Dobbs, Matt ; Dong, Fengqiu Adam ; Fonseca, Emmanuel ; Gaensler, B. M. ; Herrera-Martín, Antonio ; et al ( February 2023 , The Astrophysical Journal)

   Fast radio bursts (FRBs) are brief, energetic, typically extragalactic flashes of radio emission whose progenitors are largely unknown. Although studying the FRB population is essential for understanding how these astrophysical phenomena occur, such studies have been difficult to conduct without large numbers of FRBs and characterizable observational biases. Using the recently released catalog of 536 FRBs published by the Canadian Hydrogen Intensity Mapping Experiment/Fast Radio Burst (CHIME/FRB) collaboration, we present a study of the FRB population that also calibrates for selection effects. Assuming a Schechter function, we infer a characteristic energy cut-off of$E_{\mathrm{char}}={2.38}_{-1.64}^{+5.35}\times {10}^{41}$erg and a differential power-law index ofγ=$-{1.3}_{-0.4}^{+0.7}$. Simultaneously, we infer a volumetric rate of [${7.3}_{-3.8}^{+8.8}$(stat.)${}_{-1.8}^{+2.0}(\mathrm{sys}.)]\times {10}^4$Gpc⁻³yr⁻¹above a pivot energy of 10³⁹erg and below a scattering timescale of 10 ms at 600 MHz, and find we cannot significantly constrain the cosmic evolution of the FRB population with star-formation rate. Modeling the host’s dispersion measure (DM) contribution as a log-normal distribution and assuming a total Galactic contribution of 80 pc cm⁻³, we find a median value of${\mathrm{DM}}_{\mathrm{host}}={84}_{-49}^{+69}$pc cm⁻³, comparable with values typically used in the literature. Proposed models for FRB progenitors should be consistent with the energetics and abundances of the full FRB population predicted by our results. Finally, we infer the redshift distribution of FRBs detected with CHIME, which will be tested with the localizations and redshifts enabled by the upcoming CHIME/FRB Outriggers project.

    

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4. Electromagnetic Precursors to Black Hole–Neutron Star Gravitational Wave Events: Flares and Reconnection-powered Fast Radio Transients from the Late Inspiral

   https://doi.org/10.3847/2041-8213/acfdae  

   Most, Elias R. ; Philippov, Alexander A. ( October 2023 , The Astrophysical Journal Letters)

   The presence of magnetic fields in the late inspiral of black hole–neutron star binaries could lead to potentially detectable electromagnetic precursor transients. Using general-relativistic force-free electrodynamics simulations, we investigate premerger interactions of the common magnetosphere of black hole–neutron star systems. We demonstrate that these systems can feature copious electromagnetic flaring activity, which we find depends on the magnetic field orientation but not on black hole spin. Due to interactions with the surrounding magnetosphere, these flares could lead to fast-radio-burst-like transients and X-ray emission, with${\mathit{}}_{\mathrm{EM}}\lesssim {10}^{41}{\left(B_{*}/{10}^{12}\mathrm{G}\right)}^2\mathrm{erg}{\mathrm{s}}^{-1}$as an upper bound on the luminosity, whereB_*is the magnetic field strength on the surface of the neutron star.

    

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5. Neutrino emission from binary neutron star mergers: characterising light curves and mean energies

   https://doi.org/10.1140/epja/s10050-022-00743-5  

   Cusinato, Marco ; Guercilena, Federico Maria ; Perego, Albino ; Logoteta, Domenico ; Radice, David ; Bernuzzi, Sebastiano ; Ansoldi, Stefano ( May 2022 , The European Physical Journal A)

   Neutrinos are copiously emitted by neutron star mergers, due to the high temperatures reached by dense matter during the merger and its aftermath. Neutrinos influence the merger dynamics and shape the properties of the ejecta, including the resultingr-process nucleosynthesis and kilonova emission. In this work, we analyse neutrino emission from a large sample of binary neutron star merger simulations in Numerical Relativity, covering a broad range of initial masses, nuclear equation of state and viscosity treatments. We extract neutrino luminosities and mean energies, and compute quantities of interest such as the peak values, peak broadnesses, time averages and decrease time scales. We provide a systematic description of such quantities, including their dependence on the initial parameters of the system. We find that for equal-mass systems the total neutrino luminosity (several$$10^{53}{\hbox {erg}~{\hbox {s}}^{-1}}$$${10}^{53}\text{erg}{\text{s}}^{-1}$) decreases as the reduced tidal deformability increases, as a consequence of the less violent merger dynamics. Similarly, tidal disruption in asymmetric mergers leads to systematically smaller luminosities. Peak luminosities can be twice as large as the average ones. Electron antineutrino luminosities dominate (initially by a factor of 2-3) over electron neutrino ones, while electron neutrinos and heavy flavour neutrinos have similar luminosities. Mean energies are nearly constant in time and independent on the binary parameters. Their values reflect the different decoupling temperature inside the merger remnant. Despite present uncertainties in neutrino modelling, our results provide a broad and physically grounded characterisation of neutrino emission, and they can serve as a reference point to develop more sophisticated neutrino transport schemes.

    

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