Long-period SU UMa dwarf nova V1006 Cygni outburst activity and variability at different brightness states in 2015-2017

TL;DR

This study presents extensive photometric observations of the dwarf nova V1006 Cyg over three years, analyzing its outburst activity, superhumps, and brightness variability to understand its accretion processes and outburst mechanisms.

Contribution

It provides detailed timing and period analysis of superoutbursts, superhumps, and quiescent variability, revealing new insights into the behavior of V1006 Cyg during different brightness states.

Findings

Detected positive superhumps with specific periods during superoutburst.

Identified the orbital period during a wide outburst.

Observed quasi-periodic brightness variations during quiescence.

Abstract

CCD photometric observations of the dwarf nova V1006 Cyg were carried out in 2015-2017 with 11 telescopes located at 7 observatories. They covered the 2015 superoutburst with rebrightening, five normal outbursts of ~4-day duration and one wide outburst that lasted at least seven days. The interval between normal outbursts was 16 and 22 days, and between superoutbursts is expected to be longer than 124 days. The positive superhumps with the mean period of 0^d.10544(10) and 0^d.10406(17) were detected during the 2015 superoutburst and during the short-term quiescence between rebrightening and the start of the first normal outburst, respectively. During a wide 2015 outburst the orbital period 0^d.09832(15) was found. The amplitude of this signal was ~2.5 times larger at the outburst decline than at its end. During the quiescence stage between the first and the second normal outbursts in 2017 we possibly detected the negative superhumps with the period of 0^d.09714(7). In all other cases of quiescence we found only the quasi-periodic brightness variations on a time scale of 20-30 minutes with a different degree of coherence and a variable amplitude reaching 0.5 mag in extremal cases.