Stellar Dynamics around a Massive Black Hole I: Secular Collisionless
  Theory
  We present a theory in three parts, of the secular dynamics of a (Keplerian)
stellar system of mass $M$ orbiting a black hole of mass $M_\bullet \gg M$.
Here we describe the collisionless dynamics; Papers II and III are on the
(collisional) theory of Resonant Relaxation. The mass ratio, $\varepsilon =
M/M_\bullet \ll 1$, is a natural small parameter implying a separation of time
scales between the short Kepler orbital periods and the longer orbital
precessional periods. The collisionless Boltzmann equation (CBE) for the
stellar distribution function (DF) is averaged over the fast Kepler orbital
phase using the method of multiple scales. The orbit-averaged system is
described by a secular DF, $F$, in a reduced phase space. $F$ obeys a secular
CBE that includes stellar self-gravity, general relativistic corrections up to
1.5 post-Newtonian order, and external sources varying over secular times.
Secular dynamics, even with general time dependence, conserves the semi-major
axis of every star. This additional integral of motion promotes extra
regularity of the stellar orbits, and enables the construction of equilibria,
$F_0$, through a secular Jeans theorem. A linearized secular CBE determines the
response and stability of $F_0$. Spherical, non-rotating equilibria may support
long-lived, warp-like distortions. We also prove that an axisymmetric,
zero-thickness, flat disc is secularly stable to all in-plane perturbations,
when its DF, $F_0$, is a monotonic function of the angular momentum at fixed
energy.
