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Spiral galaxies range from S0, the lenticular galaxies, to Sb, which have a bar across the nucleus, to Sc galaxies which have strong spiral arms. In total count, ellipticals amount to 13%, S0 to 22%, Sa, b, c galaxies to 61%, irregulars to 3.5%, and peculiars to 0.9%. At the center of most galaxies is a high concentration of older stars.
The rotation curve of a disc galaxy (also called a velocity curve) is a plot of the orbital speeds of visible stars or gas in that galaxy versus their radial distance from that galaxy's centre. It is typically rendered graphically as a plot , and the data observed from each side of a spiral galaxy are generally asymmetric, so that data from ...
The interfaces between regions with sharp differences in rotation are believed to be efficient sites for the dynamo processes that generate the stellar magnetic field. There is also a complex interaction between a star's rotation distribution and its magnetic field, with the conversion of magnetic energy into kinetic energy modifying the ...
Hence, when we observe a distant background galaxy (or some other celestial body), we may be lucky to see the same image of the galaxy multiple times, albeit more and more distorted. [11] A complete mathematical description for how light bends around the equatorial plane of a Kerr black hole was published in 2021. [12]
The interface between these two regions is where angular rotation gradients are strongest and thus where dynamo processes are expected to be most efficient. The inner differential rotation is one part of the mixing processes in stars, mixing the materials and the heat/energy of the stars.
The density wave theory also explains a number of other observations that have been made about spiral galaxies. For example, "the ordering of H I clouds and dust bands on the inner edges of spiral arms, the existence of young, massive stars and H II regions throughout the arms, and an abundance of old, red stars in the remainder of the disk".
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A video showing in 3D Laniakea and other nearby superclusters of galaxies. The Laniakea Supercluster encompasses approximately 100,000 galaxies stretched out over 160 Mpc (520 million ly). It has the approximate mass of 10 17 solar masses, or 100,000 times that of our galaxy, which is almost the same as that of the Horologium Supercluster. [3]