On 2018 , April 29 , a bright classical nova ( CN ) Per 2018 was discovered .
Its progenitor is well-known dwarf nova V392 Per .
In this contribution we analyse UBVR _ { C } I _ { C } photometry and optical spectroscopy of the CN V392 Per .
From the V light curve ( LC ) we found the brightness decline times t _ { 2 ,V } = 3 d , t _ { 3 ,V } = 10 d and calculated absolute magnitude of the nova at maximum MV _ { max } = -9.30 { \pm } 0.57 using the new MV _ { max } - t _ { 3 } ” universal ” decline law and MV _ { 15 } relations , adopting the Gaia data for CNe .
We determined the colour excess E _ { B - V } = 0.90 \pm 0.09 and distance to the nova d = 3.55 \pm 0.6 kpc .
The optical spectrum obtained in brightness maximum resembles that of the F2 supergiant .
Its bolometric luminosity computed by fitting the continuum by atmospheric and black-body models is in agreement with the luminosity , that we have found from photometry .
We estimated the mass of the ONe white dwarf in V392 Per as M _ { wd } = 1.21 M _ { \odot } .
The CN Per 2018 can be classified as a fast super-Eddington nova with an outburst LC of plateau type .
Nova displayed He/N spectrum classification , large expansion velocities , and triple-peaked emission-line profiles during the decline , explained by equatorial ring seen nearly face on and a bipolar flow aligned almost with the line of sight .
The post maximum spectra of CN Per 2018 and available radio data were used to estimate the inclination angle of the system as i \sim 9 ^ { \circ } .
The difference in intensity of redward and blueward emission bumps is possible to explain by about 1.5 times higher density of the receding outtflow .
The rapid increase of the bipolar outflow radial velocities by \sim 300 km/s around day 5 after the maximum was caused by the fast bipolar winds from the burning white dwarf after shrinking of its pseudophotosphere .