Superhumps in the cataclysmic variable BG Triangulum

• Published in: Monthly notices of the Royal Astronomical Society Vol. 516; no. 2; pp. 2775 - 2781
• Main Authors: Stefanov, S Y, Latev, G, Boeva, S, Moyseev, M
• Format: Journal Article
• Language: English
• Published: Oxford University Press 13.09.2022
• Subjects: binaries: close; stars: individual: BG Triangulum; stars: activity; novae, cataclysmic variables
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stac2317

ABSTRACT We present a detailed photometric study of the bright cataclysmic variable, BG Triangulum (BG Tri), using ground-based observations mainly from the Rozhen Observatory, the All-Sky Automated Survey for Supernovae (ASAS-SN), the Transiting Exoplanet Survey Satellite (TESS) and the Wide Angle Search for Planets (WASP). We report on the discovery of a negative superhump with P−sh = 0.1515(2) d and a co-existing superorbital variation with P = 3.94(53) d in data from 2019 and 2020. A positive superhump with P+sh = 0.1727(14) d is also discovered in data from 2006. The obtained negative superhump deficit ε− = 0.044(1) and the positive superhump excess ε+ = 0.090(9) give us an independent photometric evaluation of the mass ratio (q) of the system, which we find to be q− = 0.37(2) and q+ = 0.40(5), respectively. We also present a study of the quasi-periodic oscillations and stochastic variability (flickering) in BG Tri. The light curves show a rich mixture of simultaneously overlapping quasi-periods ranging from 5 to 25 min. The multicolour (UBVRI) photometric observations from the Rozhen Observatory reveal the typical increase of the flickering amplitudes to the shorter wavelengths. The recently introduced A60 amplitude of the flickering light source in all studied photometric bands is systematically lower when the negative superhump is gone in season 2021.