Accretion of a Satellite onto a Spherical Galaxy Ii. Binary Evolution and Orbital Decay

We study the dynamical evolution of a satellite (of mass M) orbiting around a companion spherical galaxy. The satellite is subject to a back-reaction force F∆ resulting from the density fluctuations excited in the primary stellar system. We evaluate this force using the linear response theory developed in Colpi and Pallavicini (1997). F∆ is computed in the reference frame comoving with the primary galaxy and is expanded in multipoles. To lowest order, the force depends on a time integral involving a dynamical 4-point correlation function of the unperturbed background. The equilibrium stellar system (of mass Nm) is described in terms of a Gaussian one-particle distribution function. To capture the relevant features of the physical process determining the evolution of the detached binary, we introduce in the Hamiltonian the harmonic potential as interaction potential among stars. The evolution of the composite system is derived solving for a set of ordinary differential equations; the dynamics of the satellite and of the stars is computed self-consistently. We determine the conditions for tidal capture of a satellite from an asymptotic free state and give an estimate of the maximum kinetic energy above which encounters do not end in a merger, as a function of the mass ratio M/Nm. We find that capture always leads to final coalescence. If the binary forms as a bound pair, stability against orbital decay is lost if the pericentric distance is smaller than a critical value. This instability is interpreted in terms of a near resonance condition and establishes when the orbital Keplerian frequency becomes comparable to the internal frequency ω of the stellar system. We show that before coalescence eccentric orbits become progressively less eccentric: The circularization is explored as a function of mass ratio. The time scale of binary coalescence τb is a sensitive function of the eccentricity e, for a fixed semimajor axis a and M/Nm ratio: the mismatch between τb at e ∼ 0 and τb at e ∼ 1 can be very large; typically τb(e <∼ 1) ∼ 6ω −1, and the time ratio τb(0)/τb(1) >∼ 5 (for M/Nm = 0.05). In addition we find that τb obeys a scaling relation with M/Nm, for circular orbits: τb ∝ (M/Nm)−α with α ∼ 0.4. In grazing encounters τb is nearly independent of mass. In a comparison with Weinberg’s perturbative technique we demonstrate quantitatively that pinning the center of mass of the galaxy would induce a much larger torque on the satellite. Subject headings: galaxies: clustering – stars: stellar dynamics