We consider consequences of hypothetical existence of baryo-dense stars created in the very early universe within an extension of Affleck-Dine scenario of baryogenesis. New constraints on the possible number of compact antimatter objects are derived.
The contemporary observational data do not exclude significant amount of antimatter in the Galaxy (and in other galaxies) in the form of the baryo-dense low-massive stars.
A mechanism of creation of stellar-like objects in the very early universe, from the QCD phase transition till BBN and somewhat later, is studied. It is argued that in the considered process primordial black holes with masses above a few solar masses
up to super-heavy ones could be created. This may explain an early quasar creation with evolved chemistry in surrounding medium and the low mass cutoff of the observed black holes. It is also shown that dense primordial stars can be created at the considered epoch. Such stars could later become very early supernovae and in particular high redshift gamma-bursters. In a version of the model some of the created objects can consist of antimatter.
We demonstrate the applicability of our new method (the Dense Shell Method or DSM) for the determination of astronomical distances by calculating the distance to SN2009ip. The distance to this supernova has been accurately determined in the standard
approach via the cosmic distance ladder and has been found to be 20.4 Mpc. Our direct method, assuming the most reasonable parameter values, gives a very close result, namely 20.1+/-0.8 (68% CL) Mpc to SN2009ip.
The equation of state and composition of matter are calculated for conditions typical for pre-collapse and early collapse stages in core collapse supernovae. The composition is evaluated under the assumption of nuclear statistical equilibrium, when t
he matter is considered as an `almost ideal gas with corrections due to thermal excitations of nuclei, to free nucleon degeneracy, and to Coulomb and surface energy corrections. The account of these corrections allows us to obtain the composition for densities a bit below the nuclear matter density. Through comparisons with the equation of state (EOS) developed by Shen et al. we examine the approximation of one representative nucleus used in most of recent supernova EOSs. We find that widely distributed compositions in the nuclear chart are different, depending on the mass formula, while the thermodynamical quantities are quite close to those in the Shens EOS.
