Accretion disks are rotating disks of gas and dust that surround certain astronomical objects, such as black holes, white dwarfs, and young stars. These disks are formed when material from a nearby source, such as a companion star, is pulled in by the gravitational force of the central object. As the material spirals inward, it heats up and emits radiation across the electromagnetic spectrum, including visible light, infrared, X-rays, and gamma rays. Accretion disks play a crucial role in the formation and evolution of various astronomical objects. They are able to efficiently transfer angular momentum and energy to the central object, allowing it to grow in size and mass over time. Accretion disks also provide a powerful source of energy, making them visible across vast distances in the Universe. Researchers study accretion disks to better understand the physical processes at work in these systems, such as the mechanisms of gas accretion, disk stability, and the generation of magnetic fields. By studying accretion disks, scientists can gain insight into the evolution of galaxies, the formation of planetary systems, and the physics of extreme environments such as black holes.