52 research outputs found
SDSS J080434.20+510349.2: Eclipsing WZ Sge-Type Dwarf Nova with Multiple Rebrightenings
We observed the 2006 superoutburst of SDSS J080434.20+510349.2 during its
plateau phase, rebrightening phase, and post-superoutburst final decline. We
found that this object is a grazing eclipsing system with a period of
0.0590048(2) d. Well-defined eclipses were only observed during the late stage
of the superoutburst plateau and the depth decreased during the subsequent
stages. We determined the superhump period during the superoutburst plateau to
be 0.059539(11) d, giving a fractional superhump excess of 0.90(2)%. During the
rebrightening and post-superoutburst phases, persisting superhumps with periods
longer than those of superhumps during the plateau phase: 0.059632(6) during
the rebrightening phase and 0.05969(4) d during the final fading. This
phenomenon is very well in line with the previously known long-period "late
superhumps" in GW Lib, V455 And and WZ Sge. The amplitudes of orbital humps
between different states of rebrightenings suggest that these humps do not
arise from the classical hot spot, but are more likely a result of projection
effect in a high-inclination system. There was no clear evidence for the
enhanced hot spot during the rebrightening phase. We also studied previously
reported "mini-outbursts" in the quiescent state and found evidence that
superhumps were transiently excited during these mini-outbursts. The presence
of grazing eclipses and distinct multiple rebrightenings in SDSS
J080434.20+510349.2 would provide a unique opportunity to understanding the
mechanism of rebrightenings in WZ Sge-type dwarf novae.Comment: 14 pages, 12 figures, PASJ accepte
OT J002656.6+284933 (CSS101212:002657+284933): An SU UMa-Type Dwarf Nova with Longest Superhump Period
We observed the 2016 outburst of OT J002656.6+284933
(CSS101212:002657+284933) and found that it has the longest recorded
[0.13225(1) d in average] superhumps among SU UMa-type dwarf novae. The object
is the third known SU UMa-type dwarf nova above the period gap. The outburst,
however, was unlike ordinary long-period SU UMa-type dwarf novae in that it
showed two post-outburst rebrightenings. It showed superhump evolution similar
to short-period SU UMa-type dwarf novae. We could constrain the mass ratio to
less than 0.15 (most likely between 0.10 and 0.15) by using superhump periods
in the early and post-superoutburst stages. These results suggest the
possibility that OT J002656.6+284933 has an anomalously undermassive secondary
and it should have passed a different evolutionary track from the standard one.Comment: 6 pages, 3 figures, accepted for publication in PASJ (Letters), Note
added in proof has been added. Supplementary Information (si.pdf) is
available in the source fil
Discovery of Negative Superhumps during a Superoutburst of January 2011 in ER Ursae Majoris
We report on a discovery of "negative" superhumps during the 2011 January
superoutburst of ER UMa. During the superoutburst which started on 2011 January
16, we detected negative superhumps having a period of 0.062242(9) d, shorter
than the orbital period by 2.2%. No evidence of positive superhumps was
detected during this observation. This finding indicates that the disk
exhibited retrograde precession during this superoutburst, contrary to all
other known cases of superoutbursts. The duration of this superoutburst was
shorter than those of ordinary superoutbursts and the intervals of normal
outbursts were longer than ordinary ones. We suggest a possibility that such
unusual outburst properties are likely a result of the disk tilt, which is
supposed to be a cause of negative superhumps: the tilted disk could prevent
the disk from being filled with materials in the outmost region which is
supposed to be responsible for long-duration superoutbursts in ER UMa-type
dwarf novae. The discovery signifies the importance of the classical prograde
precession in sustaining long-duration superoutbursts. Furthermore, the
presence of pronounced negative superhumps in this system with a high
mass-transfer rate favors the hypothesis that hydrodynamical lift is the cause
of the disk tilt.Comment: 8 pages, 3 figures, Accepted for publication in PASJ Lette
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