Mass-Defect Effect In The Gravitational Field

Gravitational effect is an important content in astrophysics and astron-omy. Researches on these gravitational effects have important practical signif-icance and theoretically guiding significance. Among them, mass-defect effect ?when particle moves to the gravitational area from the infinity and com-bines into gravitational mass, part of its mass will be radiated out in the form of heat energy or other forms of energy - is an important gravitational effect. Specifically, to a test particle, its mass defect is Am = m₀- m , where mo and m are the mass of the particle when it is in the infinity and in the grav-itational field, respectively. To a spherical shell (or a solid sphere), its mass defect is AM = M₀ - M, where MO is the total mass of the matter scattering in the infinity and M is the mass of the gravitational spherical shell (or the gravitational sphere) combined by the matter scattering in the infinity. The lost mass is radiated out in the form of heat energy or other forms of energy. Calculating the mass-defect in the different gravitational field helps us study the formation and evolution of different kind of celestial body.In the first chapter of this paper we introduce the concept and the category of the gravitational effect before presentation of the mass-defect effect. Then we simply introduce the basic knowledge in stellar and accreting theory relating to the mass-defect effect. In the second chapter we discuss the mass-defect in the Schwarzshild field and R-N field, and if a = 0 the latter will reduce to the case in the former. In the third chapter, we obtain theNull Hellings-Nordtvedt metric (NHN metric) from the Hellings-Nordtvedt theory before we calculate the mass-defect by this metric. In the last chapter, we simply introduce' the process of the formation arid evolution of the star, the accreting phenomenon, etc, from which we know that these processes or phenomenonare accompanied with the loss of mass. Therefore, discusting the mass-defect effect have important significance in astrophysics and astronomy.