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For a star that has reached nuclear fusion, the collapse will continue, with the star's mass increasing at a rate that is proportional to the star's age. For an electron-degenerate star, the rate of increase in mass is much lower because of the rapid increase in pressure. The collapse may be halted after reaching the maximum mass where the force of gravity overcomes the gas pressure; this is known as the Chandrasekhar limit.[115] This limit is about 1.4 times the mass of the sun for a non-rotating star.[116]

The force that is responsible for the emission of energy of a star is called the force of gravity. The total pressure of the star is equal to the force per unit area of the surface. It is equal to the gravitational attraction of the sun (or another star or a planet) upon the star. This pressure can be balanced by the radiation pressure. For a star of a given mass, the force of gravity is the same as the radiation pressure. However, the radiation pressure is due to the absorption of the star's own energy. This energy itself is a product of the star's gravitational collapse, and is proportional to the star's energy density. This energy is the star's binding energy.

The gravity of a heavy object is responsible for a new type of oscillation in stars. A normal stellar oscillation is due to the periodic variation in pressure within the star, and is generally thought to be of acoustic nature. Such a wave pattern is then reflected back and forth between the star's surface and the interior, with most of the energy being transferred to the star's interior. This mode is known as radial or acoustic mode. The gravity of the object is responsible for a new type of oscillation that can occur in a star, which is of g-mode nature. This motion of the star is very similar to the motion of a rigid body that has a tri-axial ellipsoidal shape. If the gravity of the object is such that there is a region that is in pressure equilibrium with the surrounding mass, there will be a region which has a lower density in this region, and a higher density on either side. The oscillation of the star will be in this region, and the motion of the star is such that it is essentially rigid, with no energy loss or gain.

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