Equilibrium structures of differentially rotating primary components of binary stars
We propose a method for computing the equilibrium structures and various other observable physical parameters of the primary components of stars in binary systems assuming that the primary is more massive than the secondary and is rotating differentially about its axis. An averaging approach is used to incorporate the rotational and tidal effects in the equations of stellar structure. Explicit expressions for the distortional terms appearing in the stellar structure equations have been obtained by assuming a general law of differential rotation.
scientific article; zbMATH DE number 1218381