Kaon properties in (proto-)neutron star matter

Abstract

The modification on kaon and antikaon properties of in the interior of (proto-)neutron stars is investigated using a chiral SU(3) model. The parameters of the model are fitted to nuclear matter saturation properties, baryon octet vacuum masses, hyperon optical potentials and low energy a kaon-nucleon scattering lengths. We study the kaon/antikaon medium modification and explore the possibility of antikaon condensation in (proto-)neutron star matter at zero as well as finite temperature/entropy and neutrino content. The effect of hyperons on kaon and antikaon optical potentials is also investigated at different stages of the neutron star evolution.

Dmesons in asymmetric nuclear matter

“…Within the effective chiral model considered in the present investigation, the D(D) energies are modified due to a vectorial Weinberg-Tomozawa, due to scalar exchange terms (σ, ζ, δ) as well as range terms [39,40]. The isospin asymmetric effects among D 0 and D…”

“…These interactions were considered within the SU(3) chiral model to investigate the modifications of K-mesons in the dense (asymmetric) hadronic medium [38,39,40].…”

“…[38,39] and have been extended to include the effects from hyperons in the asymmetric strange hadronic matter in ref. [40].…”

“…We organize the paper as follows: We briefly recapitulate the SU(3)-flavor chiral model adopted for the description of the asymmetric hadronic matter [39,40] in Section II. The properties then are studied within this approach.…”

Many-body Forces in Magnetic Neutron Stars

“…In particular, it has been extensively discussed in the literature whether exotic degrees of freedom might populate the core of neutron stars. On the one hand, it is more energetically favorable for the system to populate new degrees of freedom, such as hyperons (Dexheimer & Schramm 2008;Ishizuka et al 2008;Bednarek et al 2012;Fukukawa et al 2015;Gomes et al 2015;Maslov et al 2015;Oertel et al 2015;Lonardoni et al 2015Lonardoni et al , 2016; Biswal et al 2016;Burgio & Zappalà 2016;Chatterjee & Vidana 2016;Mishra et al 2016;Vidaña 2016;Yamamoto et al 2016;Tolos et al 2017); Torres et al 2017), delta isobars (Fong et al 2010;Schurhoff et al 2010;Drago et al 2014;Cai et al 2015;Zhu et al 2016), and meson condensates (Ellis et al 1995;Menezes et al 2005;Takahashi 2007;Ohnishi et al 2009;Alford et al 2010;Fernandez et al 2010;Mesquita et al 2010;Mishra et al 2010;Lim et al 2014;Muto et al 2015), in order to lower its Fermi energy (starting at about two times the saturation density). On the other hand, the EoS softening due to the appearance of exotica might turn some nuclear models incompatible with observational data, in particular with the recently measured massive neutron stars.…”