[vsnet-outburst 10875] SDSSp J230351.64+010651.0 bright outburst

[Taichi Kato]

SDSSp J230351.64+010651.0 bright outburst

  According to Jeremy Shears (baavss-alert message), this CV is undergoing
a bright outburst.  This outburst could be a superoutburst.
Time-resolved photometry is stronly encouraged.

  YYYYMMDD(UT)   mag  observer
  20091130.1070 <14.50:V (ASAS (Pojmanski, G. 2002, Acta Astron. 52,397))
  20100103.750  136C  (Jeremy Shears)

===
See also [vsnet-alert 9004] in 2006 (maximum 14.2v):
http://ooruri.kusastro.kyoto-u.ac.jp/pipermail/vsnet-alert/2006-September/000626.html
SDSSp J230351.64+010651.0 strong 0.07-d modulations on Sep. 1

   Kyoto observations have revealed that SDSSp J230351.64+010651.0 
showed strong 0.4-mag modulations on September 1, during the
decline stage of the recent outburst.  Although the coverage
is insufficient to determine the accurate periodicity, the recorded
period was close to 0.07 d (consistent with the claimed 100 min
periodicity).  The mean light curve had hump-like, rather than
sinusoidal, features.  The object had faded by 1.2 mag/d since
August 31, and further showed a much slower decline during the
subsequent nights.  The initial fading rate is consistent with
what could be expected for a normal outburst of a 100-min dwarf
nova.

   The presence of strong modulations following a short outburst
resembles that of BZ UMa, a short-period system without recorded
superoutbursts.

[vsnet-alert 8995] Re: SDSSp J230351.64+010651.0 outburst

   So, the amplitude of the current outburst is (at least)
4.9 mag.  Although this is not well above usual thresholds of
SU UMa-type superoutbursts, the literature description would
make it a suitable target for time-resolved photometry.
The reported "low mass-transfer" for such a period (100 min)
is relatively rare; from the lack of prominent emission from
the hot spot in quiescence, the object may resemble rather
unusual dwarf novae like HT Cas.

[vsnet-alert 8992] SDSSp J230351.64+010651.0 outburst

   According to Ian Miller, the SDSS dwarf nova SDSSp J230351.64+010651.0
is in outburst.  Szkody et al. describes (AJ 123, 430):

Using the best-fit period of 100 minutes, the phases for H were computed
with the time of the red-to-blue crossing of the emission lines for H
as phase zero. The absence of any eclipse during quiescence or outburst
suggests that SDSS 2303 is a system with a fairly low inclination.

The tomograms of SDSS 2303 are consistent with a low mass transfer rate
system with minimal disk emission and no evidence for a luminous
hot spot near the stream location. 

  The object is V=19.05 in quiescence.