PaperPanorama

Nuclear Theory·nucl-th

Wednesday·November 8, 2017

8 papers6 primary·2 cross-listed

  1. 07

    Anomalous effects of dense matter under rotation

    Xu-Guang Huang🇨🇳 · Kentaro Nishimura🇯🇵 · Naoki Yamamoto🇯🇵

    We study the anomaly induced effects of dense baryonic matter under rotation. We derive the anomalous terms that account for the chiral vortical effect in the low-energy effective theory for light Nambu-Goldstone modes. The anomalous terms lead to new physical consequences, such as the anomalous Hall energy current and spontaneous generation of angular momentum in a magnetic field (or spontaneous magnetization by rotation). In particular, we show that, due to the presence of such anomalous terms, the ground state of the quantum chromodynamics (QCD) under sufficiently fast rotation becomes the "chiral soliton lattice" of neutral pions that has lower energy than the QCD vacuum and nuclear matter. We briefly discuss the possible realization of the chiral soliton lattice induced by a fast rotation in noncentral heavy ion collisions.

    hep-phcond-mat.mes-hallhep-thnucl-thJHEP(2018)·91 citations
  2. 08

    Gravitational-wave constraints on the neutron-star-matter Equation of State

    Eemeli Annala🇫🇮 · Tyler Gorda🇫🇮 · Aleksi Kurkela🇨🇭 · Aleksi Vuorinen🇫🇮

    The LIGO/Virgo detection of gravitational waves originating from a neutron-star merger, GW170817, has recently provided new stringent limits on the tidal deformabilities of the stars involved in the collision. Combining this measurement with the existence of two-solar-mass stars, we generate a generic family of neutron-star-matter Equations of State (EoSs) that interpolate between state-of-the-art theoretical results at low and high baryon density. Comparing the results to ones obtained without the tidal-deformability constraint, we witness a dramatic reduction in the family of allowed EoSs. Based on our analysis, we conclude that the maximal radius of a 1.4-solar-mass neutron star is 13.6 km, and that smallest allowed tidal deformability of a similar-mass star is .

    astro-ph.HEhep-phnucl-thPRL(2018)·1022 citations

Affiliations

first authorsco-authorsvia INSPIRE