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Equilibrium Structures of Differentially Rotating and Tidally Distorted White Dwarf Models of Stars

“…Unstable Springer tidally distorted white dwarf models. The equilibrium structures of such white dwarf models can be computed using the technique earlier used by Mohan et al (1997) for obtaining the equilibrium structures of differentially rotating primary components of binary stars, assuming that the primary components have a polytropic structure. This approach uses the averaging technique of Kippenhahn and Thomas (1970) to account for the distortional effects caused by rotational and tidal forces.…”

“…In one such approximation Mohan et al (1990) used averaging techniques of Kippenhahn and Thomas (1970) in conjunction with certain results of Roche equipotentials earlier obtained by Kopal (1972) to determine the equilibrium structure of rotationally and tidally distorted stellar models. Later, Mohan et al (1997) adopted this methodology to compute the inner structures and various observable parameters of differentially rotating and tidally distorted polytropic models of stars. The approximation of exact equipotential surfaces of rotationally and tidally distorted stars by corresponding Roche equipotentials used in this method may not be very much justified for the white dwarf stars.…”

“…Mohan et al, 1997) to determine the effects of differential rotation and tidal distortions on the equilibrium structures of white dwarf stars.…”

“…This method utilizes the averaging approach of Kippenhahn and Thomas (1997) and the concept of Roche equipotentials in a manner earlier used by Mohan et al (1997) to incorporate the effects of rotation and tidal distortions on the equilibrium structures of certain rotationally and tidally distorted stellar models. The use of the method has been illustrated by applying it to obtain the structures and some observable parameters of certain differentially rotating and tidally distorted binary systems whose primary component is assumed to be a white dwarf star.…”

Equilibrium Structures of Rotationally and Tidally Distorted Polytropic Models of Stars

“…Approximate methods have therefore often been used in literature to study such problems. In one such approximation (Kopal, 1972(Kopal, , 1978Mohan and Singh, 1978;Mohan and Saxena, 1983;Mohan et al, 1990Mohan et al, , 1992Mohan et al, , 1997) the actual equipotential surfaces of a rotationally and tidally distorted star are approximated by equivalent Roche equipotentials, assuming both stars in the binary system to be point masses. This approximation is valid for highly centrally condensed types of stars.…”