The orbital and superhump periods of the SU UMa-type dwarf nova V1212 Tauri

TL;DR

This study presents detailed photometric observations of the 2011 superoutburst of the dwarf nova V1212 Tauri, revealing three superhump regimes, period changes, and an orbital period estimate, enhancing understanding of SU UMa-type dwarf novae.

Contribution

First detailed multi-regime superhump period analysis of V1212 Tauri during a superoutburst, including orbital period determination.

Findings

Identified three distinct superhump regimes with varying periods.

Measured orbital period as 0.06818 days.

Observed period increase and decrease during different phases.

Abstract

We report CCD photometry of the superoutburst of the dwarf nova V1212 Tau obtained during 2011 January and February. The outburst amplitude was at least 6 magnitudes and it lasted at least 12 days. Three distinct superhump regimes were observed. Initially low amplitude superhumps (0.03 to 0.05 magnitude peak-to-peak) with Psh = 0.0782(52) d were present. The superhumps reached a maximum amplitude of 0.31 magnitudes at the beginning of the plateau phase, with Psh = 0.07031(96) d. Subsequently the star began to fade slowly. During the first part of the decline, the period increased with dPsh/dt = +1.62(9) x 10-3 and the amplitude of the superhumps also declined. Mid way through the slow decline, the superhumps partially regrew and this point coincided with a change to a new superhump regime during which the period decreased with dPsh/dt = -1.50(39) x 10-3. We determined the orbital period as Porb = 0.06818(64) d and the superhump period excess as epsilon = 0.034(15)