Matter
ghost-matter astrophysics.3 :
The
radiative era : The problem of the "origin" of the universe.
The problem of
the homogeneity of the early universe.(p5)
Fig. 4 : Evolution
of the Planck constant during radiative era.
If we plot the curve together :
Fig. 5**: Radiative era.**
...This
is a new description of the radiative era. The era (t < tcr)
corresponds to the primeval universe and nucleosynthesis phenomena. As the
energies are assumed to be constant during this period, all associated processes
(nucleosynthesis) should be rephrased in terms of "variable constants".
...What
about the dezionization ? Call td the value of time when desionization
occurs (in the standard model »105 yrs).
Assume tcr � td /10 . Then,
when t > 10 tcr the constants behave like absolute constants. The individual
energies of particles are no longer constant and the mixture temperature become
less than 3000°. Then desionization occurs, matter and radiation are discoupled,
etc.
What about the cosmic background
radiation ?
...In
that new description of the radiative era, the photon energy is constant when
t < tcr. But the cosmic background radiation photons are not
"primeval photons" but "secondary ones", emitted at the desionization time.
For t > td their energy falls down and Tr
tends to 2,7°K.
...In
order to compare the standard model to that new one, call Rcr the
value of the space scale factor when t = tcr and Rd its value when
t = td (desionization).
Fig. 6 : Compared evolutions
: matter and radiation densities.
Similar curves, for matter dominated
era and ghost universe
(r*m
»
1/R*3 and r*r
»
1/R*4).
Fig. 7
: This figure is identical
to figure 1
except R »
t2/3 during the (short) radiative era (insteadt1/2).
...After
the transition, before ghost matter clumps formation (see paper [7]) ,matter
temperature Tm » 1/R2, (while T*m »
1/R*2) . If we assume an isentropic expansion :
(76)
