Wed·Jul 20, 2016Wednesday·July 20, 2016

1. 01*

   Review of anisotropic flow correlations in ultrarelativistic heavy-ion collisions

   You Zhou🇩🇰

   Anisotropic flow phenomena is a key probe of the existence of Quark-Gluon Plasma. Several new observable associated with correlations between anisotropic flow harmonics are developed, which are expected to be sensitive to the initial fluctuations and transport properties of the created matter in heavy ion collisions. I review recent developments of correlations of anisotropic flow harmonics. The experimental measurements, together with the comparisons to theoretical model calculations, open up new opportunities of exploring novel QCD dynamics in heavy-ion collisions.

   nucl-exnucl-thAdv.High Energy Phys.(2016)·23 citations
2. 02*

   Nuclear constraints on gravitational waves from deformed pulsars

   Plamen G. Krastev🇺🇸 · Bao-An Li🇺🇸

   The recent direct detection of gravitational waves (GWs) from binary black hole mergers (2016, Phys. Rev. Lett. 116, no. 6, 061102; no. 24, 241103) opens up an entirely new non-electromagnetic window into the Universe making it possible to probe physics that has been hidden or dark to electromagnetic observations. In addition to cataclysmic events involving black holes, GWs can be triggered by physical processes and systems involving neutron stars. Properties of neutron stars are largely determined by the equation of state (EOS) of neutron-rich matter, which is the major ingredient in calculating the stellar structure and properties of related phenomena, such as gravitational wave emission from elliptically deformed pulsars and neutron star binaries. Although the EOS of neutron-rich matter is still rather uncertain mainly due to the poorly known density dependence of nuclear symmetry energy at high densities, significant progress has been made recently in constraining the symmetry energy using data from terrestrial nuclear laboratories. These constraints could provide useful information on the limits of GWs expected from neutron stars. Here after briefly reviewing our previous work on constraining gravitational radiation from elliptically deformed pulsars with terrestrial nuclear laboratory data in light of the recent gravitational wave detection, we estimate the maximum gravitational wave strain amplitude, using an optimistic value for the breaking strain of the neutron star crust, for 15 pulsars at distances 0.16 kpc to 0.91 kpc from Earth, and find it to be in the range of $\sim [0.2-31.1]\times 10^{-24}$, depending on the details of the EOS used to compute the neutron star properties. Implications are discussed.

   ↳ nucl-thastro-ph.HEastro-ph.SRnucl-ex2 citations
3. 03*

   Improved Measurement of the Reactor Antineutrino Flux and Spectrum at Daya Bay

   F.P. An · A.B. Balantekin · H.R. Band · M. Bishai · S. Blyth · D. Cao · G.F. Cao · J. Cao · W.R. Cen · Y.L. Chan · J.F. Chang · L.C. Chang and 210 other authors

   A new measurement of the reactor antineutrino flux and energy spectrum by the Daya Bay reactor neutrino experiment is reported. The antineutrinos were generated by six 2.9~GW${}_{\mathrm{th}}$ nuclear reactors and detected by eight antineutrino detectors deployed in two near (560~m and 600~m flux-weighted baselines) and one far (1640~m flux-weighted baseline) underground experimental halls. With 621 days of data, more than 1.2 million inverse beta decay (IBD) candidates were detected. The IBD yield in the eight detectors was measured, and the ratio of measured to predicted flux was found to be $0.946\pm 0.020$ ($0.992\pm 0.021$) for the Huber+Mueller (ILL+Vogel) model. A 2.9~$\sigma$ deviation was found in the measured IBD positron energy spectrum compared to the predictions. In particular, an excess of events in the region of 4-6~MeV was found in the measured spectrum, with a local significance of 4.4~$\sigma$. A reactor antineutrino spectrum weighted by the IBD cross section is extracted for model-independent predictions.

   ↳ hep-exnucl-exphysics.ins-detCPC(2017)·242 citations
4. 04*

   Detecting supernova neutrinos with iron and lead detectors

   Abhijit Bandyopadhyay (RKMVU)🇮🇳 · Pijushpani Bhattacharjee (SINP)🇮🇳 · Sovan Chakraborty (IIT-Guwahati)🇩🇪 · Kamales Kar (RKMVU)🇮🇳 · Satyajit Saha (SINP)🇮🇳

   Supernova (SN) neutrinos can excite the nuclei of various detector materials beyond their neutron emission thresholds through charged current (CC) and neutral current (NC) interactions. The emitted neutrons, if detected, can be a signal for the supernova event. Here we present the results of our study of SN neutrino detection through the neutron channel in lead (${}^{208}\mathrm{Pb}$) and iron (${}^{56}\mathrm{Fe}$) detectors for realistic neutrino fluxes and energies given by the recent Basel/Darmstadt simulations for a 18 solar mass progenitor SN at a distance of 10 kpc. We find that, in general, the number of neutrons emitted per kTon of detector material for the neutrino luminosities and average energies of the different neutrino species as given by the Basel/Darmstadt simulations are significantly lower than those estimated in previous studies based on the results of earlier SN simulations. At the same time, we highlight the fact that, although the total number of neutrons produced per kTon in a iron detector is more than an order of magnitude lower than that for lead, the dominance of the flavor blind NC events in the case of iron, as opposed to dominance of ${\nu }_e$ induced CC events in the case of lead, offers a complementarity between the two detector materials so that simultaneous detection of SN neutrinos in a lead and a sufficiently large iron detector suitably instrumented for neutron detection may allow estimating the fraction of the total $\mu$ and $\tau$ flavored neutrinos in the SN neutrino flux and thereby probing the emission mechanism as well as flavor oscillation scenarios of the SN neutrinos.

   ↳ astro-ph.HEhep-phnucl-exPRD(2017)·14 citations
5. 05*

   Prediction for a four-neutron resonance

   A. M. Shirokov🇺🇸 · G. Papadimitriou🇺🇸 · A. I. Mazur · I. A. Mazur · R. Roth🇩🇪 · J. P. Vary🇺🇸

   We utilize various {\em ab initio} approaches to search for a low-lying resonance in the four-neutron ($4n$) system using the JISP16 realistic $NN$ interaction. Our most accurate prediction is obtained using a $J$-matrix extension of the No-Core Shell Model and suggests a $4n$ resonant state at an energy near $E_r=0.8$ MeV with a width of approximately $\Gamma =1.4$ MeV.

   ↳ nucl-thnucl-exPRL(2016)·91 citations

* Reconstructed cohort: no mailing for this day survives in the archive. Papers are grouped by their submission times and arXiv's announcement cut-off, assuming announcement without delay; positions follow identifier order. Validated at ~91% exact-day agreement against the archived era.