ISSN 0917-2211

Variable Star Bulletin
No.34

Sep. 1999

Outburst of BF Eri
Tsutomu Watanabe(117 Shirao dormitory , 1414 Oonakazato , Shizuoka , 418-0044 Japan)
E-mail : jcc00212@nifty.ne.jp Received 1999 May. 30
BF Eri is listed as a semiregular-type pulsating star (196 days period, 13.5-15.5p magnituderange) in GCVS (Kholopov86). However, this star is identi¯ed with the X-ray source 1ES0437-046 (Elvis et al.92) and pointed out to be a cataclysmic variable by spectroscopy (Schachteret al. 1996). Two outbursts were detected by VSOLJ member's monitoring. The light curve isshown in Figure 1. The observation data are listed in Table 1. The light curve demonstrates that
BF Eri is a dwarf nova with a period of 40-50 days. The observed magnitude range is13.2-<14.7v, which is consistent with the GCVS value. Further obsevations are strongly
encouraged to get more detail of outburst characteristic and physical parameters.

Table 1: Magnitude estimates of BF EriDate(UT)981024.720
981107.624
981117.703
981219.647
990108.546
990109.576
990110.572
990111.520
990112.551
990115.570
990116.443
990118.565

Mag.
<14.7
<13.6
14.7
<13.8
13.3
13.2
13.3
13.4
13.5
13.9
14.6
14.7

Obs.
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt

Date(UT)
990120.604
990122.555
990128.474
990128.560
990129.620
990130.474
990131.426
990204.469
990206.549
990207.481
990208.547
990212.565

Mag.
<13.8
<14.6
<13.6
<14.0
<12.4
<13.6
<13.4
<14.6
<14.6
<14.6<14.1
<14.6

Obs.
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt

Date(UT)
990213.432
990214.578
990215.585
990217.529
990220.605
990221.419
990222.431
990222.441
990222.523
990228.389
990228.535

Mag.
<14.1
<14.1
<13.6
<13.9
<13.2
13.6
13.92V
14.02V<13.6
14.40V
<12.7

Obs.
Wnt
Wnt
Wnt
Wnt
Wnt
Wnt
Kis
Kis
Wnt
Kis
Wnt

Mag. (Magnitude)
The pre¯x < indicates the upper limit (the variable was not seen)
V : Johnson V other : visual
Magnitude was estimated by GSC magnitude.
Obs. (Observer)
Kis: Seiichiro Kiyota (25cm Schmidt Cassegrain + Apogee AP-7 + Optec Max¯lter 2)
Wnt: Tsutomu Watanabe (32cm re°ector + visual)Acknowledgments
This work is based on the VSOLJ database. I wish to thank Seiichiro Kiyota for his valuable
observation and Dr.Taichi Kato (Kyoto University) for his helpful suggestions and reading themanuscript.
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Figure 1.

Light curve of BF Eri

References
Elvis M., Plummer D., Schachter J., Fabbiano G., ApJS 80, 257 (1992)
Kholopov, et al, General Catalogue of Variable Stars (1986)
Schachter J., Remillard R., Saar S., Favata F., Sciortino S., Barbera M., ApJ 46, 747 (1996)

Outburst of TmzV34 (= RXJ0915.8+0900)
Tsutomu Watanabe(117 Shirao dormitory , 1414 Oonakazato , Shizuoka , 418-0044 Japan)
E-mail : jcc00212@nifty.ne.jp Received 1999 May. 31
This object was ¯rst discovered by ROSAT(= RX J0915.8+0900). Bade et al.(1998) identi¯ed it
as a cataclysmic variable. Takamizawa (1998) independently discovered this star as a new variablestar, TmzV34 (initially reported as an irregular variable with a range of 13.1-15.0p), and detected
one outburst at 13.1 mag. on 1994 Nov. 30.715 from his patrol ¯lms. On 1999 Apr. 8.596 UT, I
detected a further outburst at 13.6 mag. visualy. On 1999 Apr. 7.616 UT, the object seemedslightly fainter than 13.7 mag. On 1999 Apr. 13.564 UT , it was not seen. (upper limit 13.1 mag.)
Further obsevations are strongly encouraged.
Acknowledgments
I wish to thank Dr.Taichi Kato (Kyoto University) for his helpful suggestions and reading themanuscript.
Remarks
This outburst detection was announced in vsnet-alart (Kato 1999)
References
References
Bade N., Engels D., Voges W., Beckmann V., Boller TH., Cordis L., Dahlem M.,Englhauser J.,
Molthagen K., Nass P., Studt J., Reimers D., A & AS 127, 145B (1998)
Kato T., "Outburst of TmzV34 = RXJ0915.8+0900", vsnet-alart 2854 (1999)
Takamizawa K., VSOLJ Variable Star Bulletin 30-31, 3 (1998)
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Outburst of Goranskij's variable near GM SgrTsutomu Watanabe(117 Shirao dormitory , 1414 Oonakazato , Shizuoka , 418-0044 Japan)
E-mail : jcc00212@nifty.ne.jp Received 1999 Aug. 23
Goranskij's variable (= GSC 6848.03786 = USNO0600.16547317, R.A.18h 19m 21s.64
DEC.-25± 24' 25".7 (J2000) ) was discovered as a candidate of GM Sgr(Luyten's variable)(Granskij 1990). Original GM Sgr (Luyten's variable) was classi¯ed as a long period variable(Lutyen 1927) and observed late-type spectrum (Hoard 1995). Goranskij's variable was classi¯ed
as a possible novalike variable (Granskij 1990). On 1999 Aug. 8.610 UT, I detected a furtherobvious outburst of this object at 12.9 Mag. visualy. This outburst was con¯rmed by otherobserver (Stubbings 1999a,b). The chart which I was used is stored at the publicly available
ftp-site, f tp : ==f tp:kusastro:kyoto ¡ u:ac:jp=pub=vsnet=charts=GMS gr:ps;and this object is marked " = GM Sgr?". Further obsevations are strongly encouraged.
Remarks This outburst detection was announced in vsnet-alart (Kato 1999).
Acknowledgments I wish to thank Dr.Taichi Kato (Kyoto University) for his helpful advice.
References
Granskij, V. P. 1978, Astr.Tsirk., 1024, 3
Hoard, D. W., Szkody, P., Wachter, S. 1995, AJ 110, 1824
Kato, T. 1999, vsnet-alart3345(http://www.kusastro.kyoto-u.ac.jp/vsnet/Mail/vsnet-alert/msg03345.html)
Luyten, W. J. 1927, Harvard Bull., No.852, 1
Stubbings, R. 1999a, vsnet-obs 22248(http://www.kusastro.kyoto-u.ac.jp/vsnet/Mail/obs22000/msg00248.html)
Stubbings, R. 1999b, vsnet-obs 22282(http://www.kusastro.kyoto-u.ac.jp/vsnet/Mail/obs22000/msg00282.html)

Detection of the second historical decline of VY-Scl type variable LQ Peg
Tsutomu Watanabe(117 Shirao dormitory , 1414 Oonakazato , Shizuoka , 418-0044 Japan)
E-mail : jcc00212@nifty.ne.jp Received 1999 Sep. 07
LQ Peg (= PG 2133+115, R.A.21h 36m 19s.13, DEC.+11 ゜ 40' 54".68 (J2000)) was discovered
as an ultraviolet-excess object and spectroscopically con¯rmed to be a cataclysmic variable(Green et al. 1982, 1986; Ferguson et al. 1984). A decline was found between 1969 and 1970 byphotographic observation in 1960-1995 (Sokolov et al. 1996), then this star was listed in 73th
Name list (Kazarovets & Sumus 1997). The star has been considered as a likely VY Scl-typevariable.
I detected the ¯rst-ever decline since the discovery of the VY Scl-type nature. LQ Peg had been
seen at 14 and a half Mag., though on 1999 Jul. 9.716 UT, this star could not been seen at alimiting magnitude of 14.6, moreover on 1999 Aug. 17.717 UT, this star was fainter than 15.3
Mag.(see Table 1). This decline was con¯rmed by CCD observation (Kato 1999a). Furtherobservation is encouraged to get a more detailed characteristics and physical parameters.
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Table 1:Recent observation of LQ Peg
Date (UT)1998 September 16.642
1998 November 7.558
1998 November 15.474
1999 July 9.716
1999 August 11.701
1999 August 14.726
1999 August 17.613
1999 August 17.717

Date (JD)
2451073.142
2451125.058
2451132.974
2451369.216
2451402.201
2451405.226
2451408.113
2451408.217

Magnitude
14.6
fainter than 13.7
14.6
fainter than 14.6
fainter than 14.9
fainter than 15.2
fainter than 15.2
fainter than 15.3

Instrument: 32cm re°ector + visual
Magnitude was estimated against neighboring GSC stars
Acknowledgments This decline detection was announced in vsnet-alart (Kato 1999b).
Remarks I wish to thank Dr.Taichi Kato ( Kyoto University ) for his helpful suggestions andreading the manuscript.
References
Ferguson,D.H., Green,R.F., Liebert,J., 1984, ApJ, 287, 320
Green,R.F., Ferguson,D.H., Liebert,J., Schmidt,M. 1982, PASP, 560, 94
Green,R.F., Schmidt,M., Liebert,J. 1986, ApJ Suppl., 61, 305
Kato, T. 1999a, vsnet-obs 22278
http://www.kusastro.kyoto-u.ac.jp/vsnet/Mail/obs22000/msg00278.html
Kato, T. 1999b, vsnet-alart 3350
http://www.kusastro.kyoto-u.ac.jp/vsnet/Mail/vsnet-alert/msg03350.html
Kazarovets,E.V., Samus,N.,N. 1997, IBVS, 4771, 1
Sokolov,D.A., Shugarov,S.YU., Pavlenko,E.P., 1996, in LONG-TERM BRIGHTNESS OF TWO
CVS, Cataclysmic Variables and Related Objects, edited by A.Evans and J. H. Wood
(Kluwer Academic Publishers), p219

EditorSta®

Keiichi
MakotoMasahiko
Seiichiro

Saijo
Watanabe
MomoseKiyota

VSOLJc/o Keiichi Saijo National Science Museum, Ueno-Park, Tokyo Japane-mail:skiyota@abr.a®rc.go.jp (Seiichiro Kiyota)

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