The Birth of a Ghost Star.

Area of Science:

• Theoretical astrophysics
• Cosmology
• Fluid dynamics

Background:

• Self-gravitating fluid distributions are fundamental to understanding cosmic structures.
• Previous models often simplify fluid evolution, limiting exploration of exotic end-states.
• The concept of a 'ghost star' presents a unique theoretical challenge in astrophysics.

Purpose of the Study:

• To develop an analytical model for a spherically symmetric dissipative self-gravitating fluid.
• To investigate the asymptotic behavior of such a system towards a 'ghost star' state.
• To explore the physical conditions and implications of forming a ghost star.

Main Methods:

• Constructed a model based on quasi-homologous fluid evolution with a vanishing complexity factor.
• Modified the initial solution to achieve asymptotic behavior towards a ghost star.
• Imposed a condition on radial distance variation to introduce a central cavity.

Main Results:

• An analytical model was successfully derived, demonstrating the emergence of a ghost star.
• The end state is a static fluid distribution with vanishing total mass.
• The energy density distribution exhibits negative regions within the fluid.

Conclusions:

• The study provides a viable analytical framework for modeling ghost star formation.
• The model incorporates dissipative processes and specific conditions leading to this exotic state.
• Potential observational consequences of ghost stars warrant further investigation.