Outburst of S10932 on 1996 Mar. 26


(vsnet-alert 372)

Makoto Iida (VSOLJ) communicates that both GO Com and S10932 are detected in outburst on his CCD frames taken on Mar. 26. Follow-up observations are strongly encouraged.

Iida's observations

(vsnet-obs 2480)

S10932         960326.61128 147  Arm.VSOLJ  outburst & eclipse observation
S10932         960326.61356 148  Arm.VSOLJ
S10932         960326.61583 146  Arm.VSOLJ
S10932         960326.61825 151  Arm.VSOLJ
S10932         960326.62052 167  Arm.VSOLJ
S10932         960326.62278 154  Arm.VSOLJ
S10932         960326.62503 150  Arm.VSOLJ
S10932         960326.62728 145  Arm.VSOLJ

Outburst CCD images by Iida

Images taken outside eclipse (left) and in eclipse (right)

sequential CCD images of S10932 by Iida

Indiviual images were taken at:

      mid-exposure (in UT)
   1996 Mar. 26 14h 40m 15s
                14  43  32
                14  46  48
                14  50  17
                14  53  33
                14  56  48
                15  00  03
                15  03  17

Report by Peter Kroll

(vsnet-obs 2484)

Dear Colleagues,

Since the New Year outburst of S 10932 Com we were watching this star in almost every clear night, mainly to study its remarkably varying normal state light curve - apart from the eclipses. The normal brightness varies with an amplitude of up to one magnitude (R-band) within one orbital period. From night to night the variations are even larger - up to 1.5 mag.

Our last observations of S 10932 at 1996 March 14 show the star in its normal brightness region.

In an attempt to confirm the current outburst we found S 10932 NOT being brighter than usual (Mar 27.85). Since we know from the 96-Jan-1 outburst that the decline takes several days we should expect the star brighter than it is. On the other hand, Makoto Iida's images (ftp://ftp.kusastro.kyoto-u.ac.jp/pub/vsnet/DNe/S10932/s10932.gif) show the star really bright - no doubt that the star was in outburst.

Owing to the this rapid decline I would regard this outburst as only a small one or the maximum was earlier between 96-Mar-14 and 96-Mar-26. Perhaps there are more observers regularly watching this star in order to narrow the time of the maximum.

Best regards,

Peter Kroll

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