We analysed photometric and spectroscopic optical observations of the eclip
sing symbiotic binary AX Persei. For the first time, we present and discuss
its historical, 1887-1999, photographic/B-band and visual light curve (LC)
. The red giant in AX Per losses mass via the wind at a rate of M(overdot)
= 7.4 +/- 1.7 10(-7) M.yr(-1) The terminal velocity of the wind is v(infini
ty) = 32 +/- 6 kms(-1). We estimated an effective radius of the H-II nebula
during the post-outburst stage (to JD 2450000) to foe of R-n = 192 +/- 25
R. and its average electron concentration (n) over tilde (e) = (2.9 - 3.6)
+/- 0.7 10(9) cm(-3) for the electron temperature T-e = 1-1.5 10(4) K. The
[O-III] nebula in AX Per is rather dense, having the electron concentration
n(e)([O-IIII]) approximate to 3 10(7) cm(-3) for T-e = 1-1.5 10(4) K. Spec
troscopic observations made in the middle of the 1992.8 and 1994.7 eclipses
showed that a significant part of flux emitted in the H-I, He-II and nebul
ar [O-III] lines originates in the vicinity of the hot component. Transitio
n of AX Per to its nebular phase occurred at/around JD 2450000. A small sim
ilar to0.6 mag brightening at that time and consequently very broad wave-li
ke variation in the LC developed. This event was caused by dilution of a sh
ell around the hot star, during which about of 1.5 10(50) particles (simila
r to1.3 10(-7) M.) were injected into the ionized region.