High-density kaonic-proton matter (KPM) composed of Lambda* equiv K-p multiplets and its astrophysical connections

TL;DR

This paper proposes a new high-density baryonic matter called Kaonic Proton Matter (KPM), formed from Lambda* multiplets, which could have formed in the early universe or neutron stars, and exhibits unique stability and density properties.

Contribution

It introduces the concept of KPM composed of Lambda* multiplets, predicting its stability and potential formation during the early universe and in astrophysical objects, with implications for QCD and baryogenesis.

Findings

KPM is predicted to be more stable and lower in energy than neutron ensembles at large m.

Formation of KPM could have occurred during the Big Bang QGP phase.

KPM may be produced in neutron star environments.

Abstract

We propose and examine a new high-density composite of $\Lambda^* \equiv K^-p = (s \bar{u}) \otimes (uud)$, which may be called {\it Kaonic Proton Matter (KPM)}, or simply, {\it $\Lambda^* $-Matter}, where substantial shrinkage of baryonic bound systems originating from the strong attraction of the $(\bar{K}N)^{I=0}$ interaction takes place, providing a ground-state neutral baryonic system with a huge energy gap. The mass of an ensemble of $(K^-p)_m$, where $m$, the number of the $K^-p$ pair, is larger than $m \approx 10$, is predicted to drop down below its corresponding neutron ensemble, $(n)_m$, since the attractive interaction is further increased by the Heitler-London type molecular covalency, as well as by chiral symmetry restoration of the QCD vacuum. Since the seed clusters ($K^-p$, $K^-pp$ and $K^-K^-pp$) are short-lived, the formation of such a stabilized relic ensemble, $(K^-p)_m$, may be conceived during the Big-Bang Quark Gluon Plasma (QGP) period in the early universe before the hadronization and $quark$-$anti$-$quark$ annihilation proceed. At the final stage of baryogenesis a substantial amount of primordial ($\bar{u},\bar{d}$)'s are transferred and captured into {\it KPM}, where the anti-quarks find places to survive forever. The expected {\it KPM} state may be {\it cold, dense and neutral $\bar{q} q$-hybrid ({\it Quark Gluon Bound (QGB)}) states, $[s(\bar{u} \otimes u) ud]_m$,} to which the relic of the disappearing anti-quarks plays an essential role as hidden components. The {\it KPM} may also be produced during the formation and decay of neutron stars.