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Nuclear Theory·nucl-th

Wednesday·June 27, 2018

6 papers—2 primary·4 cross-listed

All6Primary2Cross-lists4
  1. 03

    Universal magnetoresponse in QCD and SYM

    Gergely Endrodi🇩🇪 · Matthias Kaminski🇺🇸 · Andreas Schafer🇩🇪 · Jackson Wu🇺🇸 · Laurence Yaffe🇺🇸

    Using recent lattice data on the thermodynamics of QCD in the presence of a background magnetic field, we show that the ratio of transverse to longitudinal pressure exhibits, to good accuracy, a simple scaling behavior over a wide range of temperature and magnetic field, essentially depending only on the ratio . We compare this QCD response to the corresponding magnetoresponse in maximally supersymmetric Yang Mills theory. Given suitable calibrations defining the comparison, we find excellent agreement. This may be viewed as a further test of the applicability of holographic models for hot QCD.

    ↳ hep-thhep-latnucl-thJHEP(2018)·25 citations
  2. 04

    Californium-254 and kilonova light curves

    Y. Zhu🇺🇸 · R. T. Wollaeger🇺🇸 · N. Vassh🇺🇸 · R. Surman🇺🇸 · T. M. Sprouse🇺🇸 · M. R. Mumpower🇺🇸 · P. Moller🇺🇸 · G. C. McLaughlin🇺🇸 · O. Korobkin🇺🇸 · T. Kawano🇺🇸 · P. J. Jaffke🇺🇸 · E. M. Holmbeck🇺🇸 and 4 other authors

    Neutron star mergers offer unique conditions for the creation of the heavy elements and additionally provide a testbed for our understanding of this synthesis known as the -process. We have performed dynamical nucleosynthesis calculations and identified a single isotope, Cf, which has a particularly high impact on the brightness of electromagnetic transients associated with mergers on the order of 15 to 250 days. This is due to the anomalously long half-life of this isotope and the efficiency of fission thermalization compared to other nuclear channels. We estimate the fission fragment yield of this nucleus and outline the astrophysical conditions under which Cf has the greatest impact to the light curve. Future observations in the middle-IR which are bright during this regime could indicate the production of actinide nucleosynthesis.

    ↳ astro-ph.HEastro-ph.SRnucl-thApJL(2018)·102 citations
  3. 05

    Neutron star properties from optimized chiral nuclear interactions

    Domenico Logoteta🇮🇹 · Ignazio Bombaci🇮🇹

    We adopt two- and three-body nuclear forces derived at the next-to-next-to-leading-order (N2LO) in the framework of effective chiral perturbation theory (ChPT) to calculate the equation of state (EOS) of -stable neutron star matter using the Brueckner--Hartree--Fock many-body approach. We use the recent optimized chiral two-body nuclear interaction at N2LO derived by \cite{ekstrom1} and two different parametrizations of the three-body N2LO interaction: the first one is fixed to reproduce the saturation point of symmetric nuclear matter while the second one is fixed to reproduce the binding energies of light atomic nuclei. We show that in the second case the properties of nuclear matter are not well determined whereas in the first case various empirical nuclear matter properties around the saturation density are well reproduced. We also calculate the nuclear symmetry energy as a function of the nucleonic density and compare our results with the empirical constraints obtained using the excitation energies of isobaric analog states in nuclei and the experimental data on the neutron skin thickness of heavy nuclei. We next calculate various neutron star properties and in particular the mass-radius and mass-central density relations. We find that the adopted interactions based on a fully microscopic framework, are able to provide an EOS which is consistent with the present data of measured neutron star masses and in particular with the mass of the neutron star in PSR J0348+0432. We finally consider the possible presence of hyperons in the stellar core and we find a softening of the EOS and a substantial reduction of the stellar maximum mass in agreement with similar calculations present in the literature.

    ↳ astro-ph.HEnucl-th0 citations
  4. 06

    QCD determination of the magnetic field dependence of QCD and hadronic parameters

    C. A. Dominguez🇿🇦 · M. Loewe🇿🇦 · Cristian Villavicencio🇨🇱

    A set of four Finite Energy QCD sum rules are used to determine the magnetic field dependence of the sum of the up- and down-quark masses of QCD, , the pion decay constant , the pion mass , the gluon condensate, , and the squared energy threshold for the onset of perturbative QCD, , related to the Polyakov loop of lattice QCD.

    ↳ hep-phnucl-thPRD(2018)·29 citations

Affiliations

first authorsco-authorsvia INSPIRE