ROP Changes 1998

from VSSC97

Recurrent Objects Programme: Changes

Gary Poyner

A recent review of the Recurrent Objects Programme has resulted in a series of changes to the objects which are currently being monitored. The following notes give details of stars which have now been dropped from the programme, and lists those which are to be added. The stars which have been dropped will still be included in the telescopic programme, and should continue to be observed. They will, however, no longer be regarded as alert stars. These changes take effect immediately. It should be remembered that the Recurrent Objects Programme was set up to monitor poorly studied CVs, whose period of outburst (if known at all) is greater than one year, and whose details of amplitude are very limited or completely unknown.

Stars dropped from the programme:

AK Cnc
12 confirmed outbursts have been detected by ROP observers since 1992 (Dec 92, Nov 93, Feb 94, Apr 94, Mar 95, May 95, Oct 95, Jan 96, May 96, Nov 96, Apr 97, Feb 98). Superhumps of an amplitude of 0.18 magnitude were detected for the first time by observers at Ouda Station, Kyoto University on January 13, 1992, thus identifying AK Cnc as a UGSU type star.
TV CrV
3 outbursts have been observed (Jun 94, Apr 95, Apr 97) none of which were observed from the UK. Superhumps were detected during the 1994 outburst (Kyoto University) which led to the UGSU classification.
W Com
2 major outbursts were detected in 1995 and 1998, but it has remained in a high state (above magnitude 15) since 1995. It is difficult to continue to classify this star as a recurrent object.
CI Aql
IBVS 4232 shows that CI Aql is in fact an Eclipsing Binary with a small amplitude. The 1917 outburst remains a mystery.
DM Lyr
14 confirmed outbursts have been observed since 1992. Both normal and superoutbursts have now been observed (Jly 92, Sep 92, May 94, Jly 94, Sep 94, Feb 95, Nov 95, Jly 96, Feb 97,May 97, Aug 97, Nov 97, Mar 98, Jly 98).
V795 Cyg
6 outbursts have been observed since 1992. No superhumps have been detected during any outburst. UGSS classification remains. Several outbursts have probably been missed during late winter periods (Nov 92, Nov 93, Aug 94, May 95, Apr 97, Mar 98).
V1028 Cyg
6 outbursts have been detected since 1992. UGSU type was confirmed during the July 1995 outburst (Sep 92, Nov 92, Jly 95, Aug 96, May 97, Nov 97).
V632 Cyg
10 outbursts have been observed since 1993. No superhumps were detected (Nov 93, Jly 94, Oct 94, Mar 95, Oct 95, May 96, Oct 96, Nov 96, Jly 97, Dec 97).
DX And
6 outbursts have been observed since 1992. UGSS classification remains. Probably at least two outbursts have been missed during this period when the field lies low in the north during early Spring (Feb 92, Aug 93, Sep 94, Jun 95, Feb 96, Dec 96).

Stars to be added:

Var 61 Her
Discovered by Antipin. (See IBVS 4578) 18h 05m 46.4 +31 40'18" (2000.0) Type UG? Range 13.5B - <18.0
V660 Her
This was seen to undergo an outburst on July 6 1995, resembling a superoutburst (As. Ap. Sup. 130, 485). 17h 42m 09.19 +23 48'30" (2000.0) Type UGSU? Range 14.2V - 19.0p
V358 Lyr
On Steve Howell’s suspected TOAD list. No previous known visual outbursts. 18h 59m 34s +42 24'14" (2000.0) Type UGWZ? Range 16p - <20.0p
USNO 1425.09823278
Just the one outburst in 1997, which turned out to be a superoutburst. 19h 27.2m +54 18' (2000.0) Type UGSU, Range 13.3 - 19.9R
Var 62 And
Discovered by Antipin (see IBVS 4578) 00h 11m 07.3 +30 32'36" (2000.0) Type UG, Range 15.5B - <17.8

The Recurrent Objects Programme list