Diskgalaxies

Diskgalaxies are a common type of galaxy characterized by a flattened, rotating disk shape. This disk typically contains a significant amount of gas and dust, which serve as the building blocks for new stars. The stars within a diskgalaxy orbit the galactic center in roughly circular paths within the disk.

A prominent feature of many diskgalaxies is a central bulge, a spherical or ellipsoidal concentration of stars at the galaxy's core. Spiral arms, often originating from the central region and extending outwards, are another common characteristic, particularly in spiral diskgalaxies. These arms are regions of higher density where star formation is actively occurring.

Diskgalaxies can be classified further based on their appearance, such as spiral galaxies (which possess prominent spiral arms) and lenticular galaxies (which have a disk and bulge but lack distinct spiral arms). Irregular diskgalaxies exist as well, lacking a clear, organized structure. The formation of diskgalaxies is thought to involve the gradual accretion of gas and smaller galaxies over cosmic time, leading to the settling of material into a rotating disk. Our own Milky Way galaxy is an example of a diskgalaxy, specifically a barred spiral.