The rapidly oscillating Ap stars pulsate in high-overtone, low degree
p-modes with their pulsation axes aligned with their oblique magnetic
axes. They show non-linearity in their pulsation in three ways: 1) The
harmonics of the basic pulsation frequency are detectable. 2) The pul
sation phase seems to vary stochastically on a time scale of days to y
ears depending on the star. 3) The form of the nonradial surface disto
rtion is not constant with time. These three effects are illustrated w
ith HR 3831, the best studied of the roAp stars. HR 3831 pulsates in d
istorted dipole mode which can be modelled as a linear sum of axisymme
tric l = 0, 1, 2, and 3 spherical harmonics aligned with the magnetic
axis. This gives rise to a 7-frequency multiplet split by exactly the
rotation frequency. The form of the distortion shows small changes on
a time-scale of years. HR 3831 shows a 5-frequency rotationally split
first harmonic multiplet, a 3-frequency rotationally split second harm
onic multiplet, and a single third harmonic frequency has probably bee
n detected at an amplitude of 0.065 mmag. The first harmonic has chang
ed its form significantly over the last 10 years. A technique for deco
mposing the fundamental frequency septuplet into its component spheric
al harmonics is used to fit the pulsation phase as a function of rotat
ion phase. This allows a unique O-C to be defined for any length of li
ght curve. The long term behaviour of the O-C diagram cannot be modell
ed adequately with a combination of periodic (Doppler shift) and quadr
atic (evolution) terms; there seems to be a significant stochastic com
ponent. The direction of the pulsation phase reversal at rotational ph
ase 0.747 is indeterminate; sometimes it is a positive-going reversal,
sometimes negative-going. At present it is not known whether this is
a numerical artifact, or a physical effect in the star. If it is a phy
sical effect, it means that small non-periodic differences in pulsatio
n amplitude between the bipolar hemispheres have been detected.