pith. sign in

arxiv: 1511.05859 · v1 · pith:AO6T7QYEnew · submitted 2015-11-18 · ⚛️ nucl-th

Strangeness S=-2 baryon-baryon interaction at next-to-leading order in chiral effective field theory

classification ⚛️ nucl-th
keywords interactionsymmetryorderbaryon-baryonchiralcontacteffectivefield
0
0 comments X
read the original abstract

The strangeness $S=-2$ baryon-baryon interaction is studied in chiral effective field theory up to next-to-leading order. The potential at this order consists of contributions from one- and two-pseudoscalar-meson exchange diagrams and from four-baryon contact terms without and with two derivatives. SU(3) flavor symmetry is imposed for constructing the interaction in the $S=-2$ sector. Specifically, the couplings of the pseudoscalar mesons to the baryons are fixed by SU(3) symmetry and, in general, also the contact terms are related via SU(3) symmetry to those determined in a previous study of the $S=-1$ hyperon-nucleon interaction. The explicit SU(3) symmetry breaking due to the physical masses of the pseudoscalar mesons ($\pi$, $K$, $\eta$) is taken into account. It is argued that the $\Xi N$ interaction has to be relatively weak to be in accordance with available experimental constraints. In particular, the published values and upper bounds for the $\Xi^- p$ elastic and inelastic cross sections apparently rule out a somewhat stronger attractive $\Xi N$ force and, specifically, disfavor any near-threshold deuteron-like bound states in that system.

This paper has not been read by Pith yet.

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Symmetry Energy Expansion with Strange Dense Matter

    nucl-th 2025-04 unverdicted novelty 7.0

    A redefinition of the symmetry energy expansion that incorporates finite strangeness consistent with SU(3) flavor symmetry and remains valid beyond typical neutron-star central densities.