Abstract
We summarize the results of our study of the cataclysmic variable AE Aqr on the basis of simultaneous UBV RI observations. For the flares, we estimated the average risetime of about 300 sec, and colours (U−B)<sub>0</sub>~1.1 and (B−V )<sub>0</sub>~0.1. We also calculated temperatures, sizes, masses and expansion velocities of a few individual fireballs. In a single night (16.08.2012), we detected ~ 8 min quasi-periodic modulation.
Highlights
AE Aquarii is a fascinating magnetic cataclysmic variable (CV) with orbital period of 9.88 h
Like the typical CVs, it consists of a K4 IV/V star which transfers material toward a magnetic fast spinning white dwarf (WD)
AE Aqr has a relatively long orbital period and is one of the largest CVs having semimajor axis a = 2.33 ± 0.02 R, WD mass MW D = 0.63 ± 0.05 M, secondary mass M2 = 0.37 ± 0.04 M
Summary
AE Aquarii is a fascinating magnetic cataclysmic variable (CV) with orbital period of 9.88 h. Like the typical CVs, it consists of a K4 IV/V star which transfers material toward a magnetic fast spinning white dwarf (WD). AE Aqr has radio and millimeter synchrotron emission (Bastian, Dulk & Chanmugam 1988), and could be source of TeV γ-rays (Oruru & Meintjes 2012 and references therein). Our observations of AE Aqr were started in 1998 with an electophotometer in V-band and are extended to simultaneous multicolour (U BV RI) observations with the telescopes of the National Astronomical Observatory Rozhen (2.0m RCC, 50/70 cm Schmidt and 60 cm telescope) and the Belogradchick Astronomical Observatory (60 cm telescope). (ii) Aug 2010 - Aug 2011: simultaneous multicolor (U BV RI) CCD observations. (iii) Sep 2011 - Aug 2013: new simultaneous multicolor CCD observations. Observational methods and data reduction are described in Zamanov et al (2012)
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