A macroscopic and kinetic relativistic description for a decoupled multi-fluid cosmology endowed with gravitationally induced particle production of all components is proposed. The temperature law for each decoupled particle species is also kinetically derived. The present approach points to the possibility of an exact (semi-classical) quantum-gravitational kinetic treatment by incorporating back reaction effects for an arbitrary set of dominant decoupled components. As an illustration we show that a cosmology driven by creation of cold dark matter and baryons (without dark energy) evolves like $$\Lambda $$Λ CDM. However, the complete physical emulation is broken when photon creation is added to the mixture thereby pointing to a crucial test in the future. The present analysis also open up a new window to investigate the Supernova-CMB tension on the values of $$H_0$$H 0 , as well as the $$S_8$$S 8 tension since creation of all components changes slightly the CMB results and the expansion history both at early and late times. Finally, it is also argued that cross-correlations between CMB temperature maps and the Sunyaev–Zeldovich effect may provide a crucial and accurate test confronting extended CCDM and $$\Lambda $$Λ CDM models.

Within the "gravitoelectromagnetism" formalism, starting from the "weak-field approximation", we derive "Type Maxwell" equations from Einstein's equations. This equations relate gravitational effects to electromagnetic ones. From this, we calculate the "gravitomagnetic" field generated by a spherical shell rotating at angular velocity ⃗ ω. Regarding the "Lense-Thirring effect", the spin ⃗ sm = Im⃗ ω of a particle of mass m orbiting a sphere of mass M and spin ⃗ SM = IM ⃗ Ω undergoes a deflection of its rotation axis ⃗ ω in the direction corresponding to the composition of the r × ⃗ sm and ⃗ Ω × ⃗ sm directions. The deflection in the axis of rotation of the body of mass m is identical to the value for the "gravitomagnetic" field associated with the same scenario involving a rotating spherical shell, as treated within the "gravitoelectromagnetic" formalism.

We discuss the gravitational collapse of a spherically symmetric massive core of a star in which the fluid component is suffering the influence of particle creation due to the temporal evolution of the system's gravity. The influence of the creation rate in the collapsing core is quantified by a phenomenological α parameter as predicted by dimensional arguments and the renormalization group approach. For all reasonable values of this free parameter, we find that the creation increases the collapsing time, but it cannot prevent the formation of a singular point. The condition for the generation of a BH is closely related to the creation's rate and is parameterized by inequality α >-1 + 2/[3(1 + ω)], where (ω) is the parameter describing the EoS of the fluid component.

A macroscopic and kinetic relativistic description for a decoupled multi-fluid cosmology endowed with gravitationally induced particle production of all components is proposed. The temperature law for each decoupled particle species is also kinetically derived. The present approach points to the possibility of an exact (semi-classical) quantum-gravitational kinetic treatment by incorporating back reaction effects for an arbitrary set of dominant decoupled components. As an illustration we show that a cosmology driven by creation of cold dark matter and baryons (without dark energy) evolves like $Λ$CDM. However, the complete physical emulation is broken when photon creation is added to the mixture thereby pointing to a crucial test in the future. The present analysis also open up a new window to investigate the Supernova-CMB tension on the values of $H_0$, as well as the $S_8$ tension since creation of all components changes slightly the CMB results and the expansion history both at early and late times. Finally, it is also argued that cross-correlations between CMB temperature maps and the Sunyaev-Zeldovich effect may provide a crucial and accurate test confronting extended CCDM and $Λ$CDM models.