Translated this means that c is a large number that can produce allot of energy from a small amount of mass. For example 1000kg of matter can release enough energy to supply the needs of the entire country of the United States for one year. This process is like a slowly exploding hydrogen bomb with gravitational forces keeping the star from flying apart. Where the star ends up on the main sequence depends on its mass. The more mass a star has the hotter it burns and the more luminous it becomes and vice versa.
Massive stars have higher core temperatures that burn faster than low mass stars that burn slower.
Thus massive stars spend less time on the main sequence even though they have more fuel to burn to begin with. Meanwhile the core continues to contract and get even hotter. The star pulsates rapidly with growing vigor until a final violent pulsation rips off the cool outer layers and a hot core is left behind. Without energy to burn the star cools to become an invisible black dwarf. M57 Attributes of a star that amateur astronomers need to be aware of can be divided into magnitude, and color spectra.