2011/09/20 by Jeremy Shears, Tom Krajci, Shears, Jeremy +17
Engineering · Physics and Astronomy · #Astronomical Observations and Instrumentation #Astrophysical Phenomena and Observations #FOS: Physical sciences #Laser-Plasma Interactions and Diagnostics #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1109.4237
Accepted for publication in the Journal of the British Astronomical Association. 15 pages, 4 figures
arxiv created 2011/09/20 · openalex publication_date 2011/09/20 · arxiv updated 2011/09/21 · openalex created_date 2022/09/14 · openalex updated_date 2026/07/28
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)