Dynamical systems analysis of a cosmological model with interacting Umami Chaplygin fluid in adiabatic particle creation mechanism: Some bouncing features

The present work aims to investigate an interacting Umami Chaplygin gas in the background dynamics of a spatially flat Friedmann-Lemaitre-Robertson-Walker (FLRW) universe when adiabatic particle creation is allowed. Here, the universe is taken to be an open thermodynamical model where the particle is created irreversibly and consequently, the creation pressure comes into the energy-momentum tensor of the material content. The rate at which the particle created is assumed to have a linear relation with the Hubble parameter and the created particle is dark matter (pressureless). The Umami Chaplygin gas is considered dark energy, pressureless dust is taken as dark matter and a phenomenological interaction term is taken for mathematical simplicity. Dynamical analysis is performed to obtain an overall evolution of the model we consider. The autonomous system is obtained by considering dimensionless variables in terms of cosmological variables. The local stability of the critical points and the classical stability of the model are also performed at each critical point. This study explores some cosmologically viable scenarios when we constrain the model parameters. Some critical points exhibit the accelerated de Sitter expansion of the universe at both the early phase as well as the late phase of evolution which is characterized by completely Umami Chaplygin fluid equation of state. Scaling solutions are also described by some other critical points showing late-time accelerated attractors in phase space satisfying present observational data, and solving the coincidence problem. A unified cosmic evolution is also achieved within this model describing the evolution of the universe starting from inflation to late time acceleration connecting through a matter-dominated intermediate phase. Finally, the non-singular bouncing behavior of the universe is also investigated for this model numerically.