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To: stefano@bicar.it
From: atel@astronomerstelegram.org
Subject: ATel  17725
Message-Id: <20260320070317.7A275288015E@server.astronomerstelegram.org>
Date: Fri, 20 Mar 2026 03:03:17 -0400 (EDT)

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Posted: Within the last 24 hours
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ATEL #17725							     ATEL #17725

Title:	AX Per returning to lower state after outburst
Author:	Marchev, D. ; Borisov, B. ; Atanasova-Sartliiska, T. ; Yordanova,
		G. ; Pavlova, N. (Konstantin Preslavsky University of Shumen); Marchev,
		V. (Institute of Astronomy and National Astronomical Observatory,
		Bulgaria)
Queries:	vlad.marchev@gmail.com
Posted:	19 Mar 2026; 14:01 UT
Subjects:Optical, Cataclysmic Variable, Star, Transient, Variables

In this telegram we are presenting multicolor photometric observations
of AX Per from AO Shumen. According to S. N. Shore et al. (ATel #17630)
there was an outburst in mid January increasing the star's brightness in
V band with half magnitude. Due to this interesting event, we did photometric
observations and followed the development of the brightness in these three
nights 9.03.2026, 13.03.2026 and 17.03.2026.  
The observations were done with 60cm telescope of the Astronomical Observatory
(AO) Shumen (Marchev, D. et al., Publ. Astron. Obs. Belgrade No. 107, 113
– 116, 2025) in Jonson photometrical system BVRI. The same standard stars
were used like in A. Henden and U. Munari A&A 458, 339-340 (2006). 
Our observations show steady decrease of brightness during the 9-day period
of observation. The average magnitude and their uncertainties are given
in Table 1 below. 
The outburst is mostly present in shorter wavelengths seen from the greater
brightness in B and V filters. This is also observed in spectral data (ATel
#17658) showing stronger emission for hydrogen and helium lines. The steady
decrease in brightness is indicating the star is returning to the original
state prior to the outburst. Magnitude of the star at 17.03 is very close
to the original state and following the trend that our observational data
shows, we can expect the star will be back to its brightness levels prior
to the outburst in 10 days. This shows that it takes twice as much time
for the star to return to its original state then it took for the outburst
to reach its maximum.  
The authors acknowledge the support of grant RD-08-105/2026 from the Science
Fund of Shumen University.

Table 1.: https://drive.google.com/file/d/1kGuFPfkvV0HjOpL1KzZM-iKPlW78z05b/view?usp=sharing
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