  Here we analyze high-resolution spectra of the Nova V392 Per obtained during
the 2018 outburst. The H$\alpha$ and H$\beta$ emission lines show a triple-peak
structure with radial velocities of about -2000 km/s, -250 km/s and 1900 km/s
respectively. The near infrared spectrum is dominated by the narrow and
single-peaked Paschen lines of hydrogen and the OI $\lambda$8446 and OI
$\lambda$7773 emission lines. Using DIBs and the KI line, we estimate the
interstellar excess towards V392 Per. Based on AAVSO and ASAS-SN photometry
data, we calculate that the t$_2$ and t$_3$ decline times are $\sim$ 3 d and
$\sim$ 11 d respectively, which classifies V392 Per as a very fast nova. We
also briefly discuss the similarity between V392 Per and other very fast novae
and the possible future evolution of the system in terms of the hibernation
model.
