2011/11/09 by Е. П. Павленко, Pavlenko, E., Viktor Malanushenko +21
Engineering · Physics and Astronomy · #Astronomical Observations and Instrumentation #Astrophysical Phenomena and Observations #FOS: Physical sciences #Gamma-ray bursts and supernovae #Solar and Stellar Astrophysics (astro-ph.SR)
paper · pdf · doi:10.48550/arxiv.1111.2339
openalex publication_date 2011/11/09 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
SDSS J080434.20+510349.2 is the 13th dwarf nova containing a pulsating white\ndwarf. Among the accreting pulsators that have experienced a dwarf novae\noutburst, SDSS J0804 has the most dramatic history of events within a short\ntime scale: the 2006 outburst with 11 rebrightenings, series of December 2006 -\nJanuary 2007 mini-outbursts, the 2010 outburst with 6 rebrightenings. Over\n2006-2011, SDSS J080434.20+510349.2 in addition to positive 0.060d superhumps\nduring the outburst and 1-month post-outburst stage, 0.059005d orbital humps\nin quiescence, displayed a significant short-term variations with periods P1 =\n12.6 min, P2 = 21.7 min, P3 = 14.1 min and P4 = 4.28 min. The 12.6-min\nperiodicity first appeared 7 months after the 2006 outburst and was the most\nprominent one during the following \∼ 900 days. It was identified as\nnon-radial pulsations of the white dwarf. The period of this pulsations varied\nwithin a range of 36 s, and amplitude changed from 0.013m to 0.03m.\nSimultaneously one could observe the 21.7-min and 14.3-min periodicities with a\nmuch lower significance level. During the minioutbursts the 21.7-min\nperiodicity became the most powerful, the 12.6-min periodicity was less\npowerful, and the 12.6-min periodicity had the lowest significance. After the\n2011 outburst the most prominent short-term periodicity appeared \∼ 7 months\nafter the outburst, but at 4.28 min. We identified that variability with\nperiods P2, P3 and P4 could be additional pulsation modes, however the relation\nof P4 to white dwarf pulsation also can't be excluded.\n