SUMMARY
Every galaxy with a central bulge is likely to harbor a supermassive black hole, as evidenced by the rotation curves of stars near the centers of galaxies like the Milky Way and M31. However, bulgeless galaxies, such as M33, do not exhibit the necessary stellar velocity dispersions to support a central black hole. Current research indicates that while large galaxies typically contain supermassive black holes, smaller elliptical or irregular galaxies may not. Direct evidence for black holes includes rotation rates and X-ray emissions from accretion disks, while indirect evidence is supported by mathematical predictions and observed phenomena.
PREREQUISITES
- Understanding of galactic structures and evolutions
- Familiarity with rotation curves and stellar velocity dispersions
- Knowledge of X-ray emissions and accretion disks
- Basic grasp of astrophysical mathematics and physics laws
NEXT STEPS
- Research the role of supermassive black holes in galaxy formation
- Learn about the methods used to measure stellar velocity dispersions
- Explore the significance of X-ray emissions in black hole detection
- Investigate the characteristics of bulgeless and irregular galaxies
USEFUL FOR
Astronomers, astrophysicists, and students of galactic dynamics seeking to understand the relationship between galaxy structure and the presence of black holes.