The Effects of Gravitational Wave Recoil on Black Holes

Abstract

In space, a black hole is a region where gravity is so strong that even light cannot escape. Because the substance is compressed into such a small area, the gravity is extremely intense. While a star is dying, this may take place. Furthermore, the asymmetric emission of gravitational waves that results from the merger of two black holes gives the merged system an impulse; this gravitational-wave recoil velocity can reach up to 4000 km/s, which is more than fast enough for the black hole to leave its host galaxy. After doing vast quantities of systematic literature research, one can see that much more research is required on the effects of gravitational wave recoil and its impact on the growth of the supermassive black hole (SMBH). Most research makes the assumption that the black hole is stationary, which is problematic since recoil can be altered by the black hole moving in an opposite, identical, or parallel direction. The shape of the primordial globular cluster, the amount of mass in low metallicity systems, the impact of few body-black hole interactions on the emergence of the early globular structure, and other factors are all the subject of extensive research on the current methods for determining the characteristics of a black hole. In addition to considering the growth and evolution of the host galaxies of the host black hole, this review paper investigates the effects of gravitational recoil on three different types of black holes, namely Massive Black Holes (MBH), Intermediate Black Holes (IBH), and SMBH. This paper suggests future research and identifies knowledge gaps, such as the knowledge gap regarding non-stationary black holes and the structure of the primordial globular cluster, where the current research methodologies and procedures regarding gravitational recoil in different black holes would require study.