The stages of stellar evolution are the result of compositional changes over very long periods of time. The size of a star, on the other hand, is determined by a balance between the pressure exerted by the hot plasma and the gravitational force of the star’s masses.

The size of a star is a natural consequence of the balance between the inward pull of gravity and the outward pressure of radiation produces huge energy inside the star. When these two forces are balanced with each other, the outer layers of the star are stable and said to be in hydrostatic equilibrium. In general, both the gravitational force and the energy generation rate are determined by the mass of a star.

During most of their lives, stars burn hydrogen in their cores, and their structures are almost completely determined by their masses. Later in their lifetimes, energy is generated in a shell surrounding their cores, and the outer layers expand, such as in the red supergiant (for higher-mass stars) and red giant (for lower-mass stars) phases.

Although stars do not have surfaces, the most common definition for the outer boundary of a star is the photosphere or the location where light leaves the star. The biggest stars are red supergiants, and the biggest has a radius that is approximately 1,800 times the radius of the Sun (432,300 miles [695,700 km]). The reason for this maximum observed size is not well understood.

One might guess that a more massive star would grow to be bigger in its red supergiant phase, but more massive stars do not evolve through a red supergiant phase, and they consequently do not grow as large. Perhaps one could imagine a star with arbitrarily large mass and thus arbitrarily large size, but no stars have been found with masses beyond approximately 200 to 300 solar masses, even at that mass, they are smaller than the biggest red supergiants. One of the largest known stars is the red supergiant VY Canis Majoris, which would envelop Jupiter if it were placed at the Sun’s location.