In the general accretion disk model theory, the accretion disk surrounding an astronomical object comprises fluid rings obeying Keplerian motion. However, we should consider relativistic and rotational effects as we close in toward the center of accretion disk surrounding spinning compact massive objects such as a black hole or a neutron star. In this study, we explore the geometry of the inner portion of the accretion disk in the context of Mukhopadhyay’s pseudo-Newtonian potential approximation for the full general relativity theory. We found that the shape of the accretion disk “puffs up” or becomes thicker and the luminosity of the disk could exceed the Eddington luminosity near the surface of the compact spinning black hole.

1. INTRODUCTION
2. METHODS
    2.1 Pseudo-Newtonian Potential
    2.2 Vertical Structure of the Thick Portion of the AccretionDisk
    2.3 Radiation and Luminosity of the Thick Portion of theAccretion Disk
3. RESULTS
    3.1 Analysis of Luminosity for an Accretion Disk
    3.2 Vertical Structure of the Thick Accretion Disk
4. CONCLUSIONS
REFERENCES

• Yu Yi(Department of Astronomy, Space Science and Geology, Chungnam National University) Corresponding Author
• Hongsu Kim(Center for Theoretical Astronomy, Korea Astronomy and Space Science Institute)
• Uicheol Jang(Department of Astronomy, Space Science and Geology, Chungnam National University)