twin universe cosmology Matter ghost matter astrophysics. 4 : Joint gravitational instabilities. 7 - Matter ghost matter astrophysics. 4 : Joint gravitational instabilities. Jean-Pierre Petit and Pierre Midy Observatory of Marseille.
Abstract :
Starting from the two coupled field equations and assuming separate conservation equations, due to zero divergence conditions, the subsequent coupled Euler equations systems are analyzed, which gives two coupled Jeans equations. A solution is given, which evidences the joint gravitational instabilities effect.
1) Building a coupled Jeans equations system.
In references [1] to [9] we have developed a model based on the two coupled field equations system.
(1) S = c ( T - T*)
(2) S* = c ( T* - T)
We assume these equations to be divergenceless, which gives : (3)
¶ ( T - T* ) = 0
It gives conservation equations. In the general case it means that the energy-matter is conserved over the two folds, if one admits that some material can be transferred from a fold to the other, through some hypertoric bridge. At the present time we do not deal with such process and shift to the more restrictive form :> (4)
¶ T = 0 ¶ T* = 0
which means that the energy-matter is conserved in the two folds, in the two sub-systems : matter and ghost matter. Then we separate conservation equations. We write the equations in a common system of coordinates { t , x , y , z }, of an observer located in the fold F.
Matter and ghost matter obey distinct sets of Euler equations :
(5)
(6)
(7)
(8)
We can add : (9)
Starting from steady initial conditions : (10)
r = ro
r* = r*o
T = To
T* = T*o
V = V* = 0
we use a perturbation method, with the perturbed Poisson equation : (11)
D d Y = 4 p G ( dr - dr* )
Introducing the Jeans lengths : (12)
we get two coupled Jeans equations : (13)
(14)
which describe the joint gravitational instabilities phenomenon.
Imagine now that we deal with a spherically symmetric steady state system, corresponding to a final state.
We can describe it by two Maxwellian distribution functions f and f* (thermodynamic equilibrium). Then we know that the mass-densities obey : (15)
that are introduced in the Poisson equation.
Write it in an adimensional form, with : (16)
we get : (17)
which is solved numerically on figure 1, for l = m = 1 ( ro = r*o )
**Fig.**1 : Steady spherically symmetric non-linear Maxwellian solution.
