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.
Categories: astro-ph.HE nucl-th