[vsnet-obs 1338] CCD observation of PU Per

[tkato@kusastro.kyoto-u.ac.jp]

  PU Per has faded quite rapidly as the following observations indicates.

  mid-UT     V-C   S.D.   N band    V-mag
---------------------------------   -----
951013.714  3.110 0.099  67 V        16.5
951014.624  4.966 0.283   4 V        18.4

  comparison star: 02h41m58s.80 +35o44'13".4 (J2000.0)
                   GSC V=13.5 (13.42 in revised VSNET chart)

  From low-amplitude hump-like features (likely orbital humps during
decline) in Oct. 13 observations, we have estimated a rough period of
0.058 +/- 0.002 day.  If this modulation actually reflects the orbital
motion, this dwarf nova is suspected to be a ultrashort orbital period
SU UMa-type dwarf nova (WZ Sge-like object or extreme TOAD).  The rate
of decline supports this idea.  The second outburst observed in Romano,
Minello (1976, IBVS 1140) can be identified as a superoutburst.

  Historical outbursts by Romano, Minello (1976):

    I max            II max
2440641  [19.1   2441280  [19.0
    644   17.4       295   15.2
    645  [19.0       298   15.2
                     301   16.6
                     303   19.0
                     308  [19.0

  Further close monitoring would be recommended.  One should remember
the present short outburst may trigger a superoutburst as recently
observed in GO Com.  Please continue a close watch.

Regards,
Taichi Kato, Daisaku Nogami & Ouda team

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