Modelling the rotational curves of spiral galaxies with a scalar field

Abstract

In a previous work (Mbelek 1998), we modelled the rotation curves (RC) of spiral galaxies by including in the equation of motion of the stars the dynamical terms from an external real self-interacting scalar field, ψ, minimally coupled to gravity and which respects the equivalence principle in the weak fields and low velocity approximation. This model appeared to have three free parameters: the turnover radius, r0. the maximum tangential velocity, vθmax = vθ(r 0), plus a strictly positive integer, n. Here, we propose a new improved version where the coupling of the ψ-field to dark matter is emphasized at the expense of its self-interaction. This reformulation presents the very advantageous possibility that the same potential is used for all galaxies. Using at the same time a quasi-isothermal dark matter density and the scalar field helps to better fit the RC of spiral galaxies. In addition, new correlations are established.