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[vsnet 1965] BZ Cam preprint (T. Watanabe)
- Date: Fri, 25 Feb 2000 21:38:12 +0900 (JST)
- To: vsnet
- From: Taichi Kato <tkato>
- Subject: [vsnet 1965] BZ Cam preprint (T. Watanabe)
- Cc: JCC00212@nifty.ne.jp
- Sender: owner-vsnet@kusastro.kyoto-u.ac.jp
BZ Cam preprint (T. Watanabe)
This paper will appear in VSOLJ Variable Star Bulletin.
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Detection of the second historical decline of BZ Cam
Tsutomu Watanabe
(117 Shirao dormitory , 1414 Oonakazato , Shizuoka , 418-0044 Japan)
E-mail : jcc00212@nifty.ne.jp
BZ Cam (= 0623+071) is a nova-like cataclysmic variable discovered in a
search for faint planetary nebulae on the Palomar Observatory sky survey
(Ellis et al. 1984) The first decline was discovered in 1928, then BZ Cam was
classified into a VY-Scl type Cataclysmic variable (Garnavich et al. 1988).
I detected the second historical decline of BZ Cam. The light curve is
shown in Figure 1 and the observation data are listed in Table 1. BZ Cam was
in the bright state on JD 2450850 - JD 2451300. Though, this star became
clearly fainter than 13 and half magnitude. This star is in the faint state
on and after JD 2451450. The magnitude has seemed to decrease gradually on
2451100 - 2451300. It is probable that this decrease was the first stage of
the following decline. Further observations are strongly encouraged to get
more detail and physical properties during the faint state.
12 +
| ' ''.
M | ': '. . .': .
a | ' '::::. .
g 13 + '
n | V
i | '
t | ''''. .
u 14 +
d |
e |
|
15 +
-+------+------+------+------+------+------+------+------+-
50800 50900 51000 51100 51200 51300 51400 51500 51600
Date ( JD -2400000 )
Figure 1: Light curve of BZ Cam
Table 1: Observation data of BZ Cam
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JD-2400000 Mag. JD-2400000 Mag. JD-2400000 Mag. JD-2400000 Mag.
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50874.192 12.5 51141.188 12.5 51197.094 12.8 51460.192 13.7
50880.099 12.5 51159.203 12.6 51199.187 12.7 51461.199 13.7
50888.051 12.6 51165.160 12.6 51201.094 12.8 51462.280 13.7
50889.099 12.6 51166.213 12.6 51207.051 12.9 51472.228 13.8
50907.121 12.5 51167.176 12.6 51213.994 12.9 51487.206 13.7
50930.056 12.6 51169.203 12.7 51216.069 12.9 51488.224 13.5
50933.012 12.6 51173.140 12.9 51218.065 12.9 51491.132 13.7
50938.071 12.7 51176.280 12.7 51219.180 12.8 51501.214 13.7
50956.994 12.6 51177.099 12.7 51222.128 12.9 51502.278 13.8
51061.269 12.3 51186.144 12.8 51222.997 12.8 51512.125 13.8
51090.260 12.3 51187.158 12.8 51224.097 12.8 51520.107 13.9
51109.188 12.6 51188.098 12.8 51225.108 12.9 51528.122 13.9
51111.299 12.3 51189.076 12.8 51227.096 12.9 51547.153 13.9
51125.256 12.4 51190.039 12.7 51230.132 12.9 51547.928 13.9
51128.133 12.5 51191.076 12.8 51232.067 12.9 51551.125 13.9
51135.194 12.6 51192.217 12.9 51276.131 13.0
51136.169 12.5 51194.101 12.8 51304.994 12.9
51137.144 12.5 51195.208 12.8 51453.322 <13.3
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The magnitude was estimated against neighboring GSC stars.
The prefix '<' indicates the upper limit ( the variable was not seen )
Instrument: 32cm reflector + visual
Remarks
This detection of the decline was announced in vsnet-alart 3544 (Kato 1999)
and confirmed in vsnet-alart 2551 (Uemura 1999).
References
Ellis, G.L., Grayson, E.T., Bond, H.E., 1984, PASP, 96, 283
Garnavich,P., Szkody, P., 1988, PASP, 100, 1522
Kato, T., vsnet-alart 3544:
http://www.kusastro.kyoto-u.ac.jp/vsnet/Mail/alert3000/msg00544.html
Uemura, M., vsnet-alart 3551:
http://www.kusastro.kyoto-u.ac.jp/vsnet/Mail/alert3000/msg00551.html
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