  Classical novae show a rapid rise in optical brightness over a few hours.
Until recently the rise phase, particularly the phenomenon of a pre-maximum
halt, was observed sporadically. Solar observation satellites observing Coronal
Mass Ejections enable us to observe the pre-maximum phase in unprecedented
temporal resolution. We present observations of V5589 Sgr with STEREO HI-1B at
a cadence of 40 min, the highest to date. We temporally resolve a pre-maximum
halt for the first time, with two examples each rising over 40 min then
declining within 80 min. Comparison with a grid of outburst models suggests
this double peak, and the overall rise timescale, are consistent with a white
dwarf mass, central temperature and accretion rate close to 1.0 solar mass,
5x10^7 K and 10^-10 solar masses per year respectively. The modelling formally
predicts mass loss onset at JD 2456038.2391+/-0.0139, 12 hrs before optical
maximum. The model assumes a main-sequence donor. Observational evidence is for
a subgiant companion; meaning the accretion rate is under-estimated.
Post-maximum we see erratic variations commonly associated with much slower
novae. Estimating the decline rate difficult, but we place the time to decline
two magnitudes as 2.1 < t_2(days) < 3.9 making V5589 Sgr a "very fast" nova.
The brightest point defines "day 0" as JD 2456038.8224+/-0.0139, although at
this high cadence the meaning of the observed maximum becomes difficult to
define. We suggest that such erratic variability normally goes undetected in
faster novae due to the low cadence of typical observations; implying erratic
behaviour is not necessarily related to the rate of decline.
