Aneeza Ijaz2025-11-252025-11-252025-07-16https://escholar.umt.edu.pk/handle/123456789/12715In this study, we explore the dynamics of relativistic fluids with axial symmetry, focusing on scenarios characterized by the presence of vorticity, the absence of dissipative processes, and shear-free but non-geodesic flow. Traditional views, particularly those stemming from Bondi conjecture, suggest that under specific ideal conditions—such as zero dissipation and geodesic motion—the emission of gravitational radiation is prohibited. However, our analysis introduces a modified framework that challenges this notion. We specifically consider fluid configurations where dissipation is absent, but the fluid possesses intrinsic rotation (vorticity) and the flow deviates from geodesic paths. Through this approach, we examine whether gravitational radiation can still emerge under these circumstances. Our findings reveal that the presence of vorticity, coupled with non-geodesic motion, facilitates the generation of gravitational waves, even in the absence of dissipative mechanisms and shear stress. This outcome implies that vorticity alone is a significant contributor to the emission of gravitational radiation, independent of the dissipative properties of the medium. Consequently, our results offer a broader understanding of the conditions that can give rise to gravitational wave phenomena in relativistic fluids. This insight is particularly relevant for astrophysical environments, such as rotating stellar interiors, neutron stars, or other compact objects, where non-dissipative, rotational fluid motion is expected to play a dominant role. Ultimately, our work highlights the essential influence of fluid rotation and non-geodesic behavior on gravitational wave production, challenging the restrictive interpretation of Bondi conjecture and contributing to the ongoing efforts to understand the complex mechanisms underlying gravitational radiation in relativistic astrophysical systems.enThesis