Main Image
Volume 315 - The Golden Age of Cataclysmic Variables and Related Objects IV (GOLDEN 2017) - Cataclysmic Variables
Transient emission of selected CRTS Cataclysmic Variables
H. Szegedi,* A. Odendaal, P. Meintjes, B. van Soelen, J.P. Marais, A. Rajoelimanana, M.M. Nyamai, R. Britto, L. Hanlon, D. Murphy, A. Martin-Carrillo, M. Motsoaledi, J.R. Thorstensen
*corresponding author
Full text: pdf
Pre-published on: 2018 July 06
Published on: 2018 September 13
We present optical photometric and spectroscopic observations of three SU UMa-type dwarf novae, i.e. AR Pic, QW Ser and V521 Peg, conducted in 2016 and 2017. These sources were selected from the Catalina Real-Time Transient Survey and observed during quiescence, outburst (AR Pic and QW Ser) and superoutburst (V521 Peg). For AR Pic, strong flickering in the light curves and an asymmetric double-peaked H$\beta$ emission line in the spectra, confirmed the presence of a very active hot spot. During outburst, detected on 18 February 2017, it exhibited a $\sim 3.3$ magnitude brightening. The projected velocity of the inner edge of the accretion disc is $\sim 2000 \rm~km~s^{-1}$. An outburst of QW Ser was detected on 8 August 2016. Absorption lines, characteristic of an optically thick disc during outburst, were detected and an outflow velocity of $\sim 1000 \rm ~km~s^{-1}$ was determined. Optical spectra during the superoutburst of V521 Peg were obtained for the first time, confirming the superoutburst nature of the outburst, as also observed in other SU UMa-type dwarf novae. The superoutburst was detected on 1 September 2017. Well-defined superhumps were observed, with an average superhump period of $P_{\rm sh} \sim 1.48$ hr. A mass ratio of $q \sim 0.14$ was determined from the period excess of $\varepsilon \sim 3 \%$.
Open Access
Creative Commons LicenseCopyright owned by the author(s) under the term of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.