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[vsnet 1903] FY Per paper by Watanabe et al.
- Date: Sat, 23 Oct 1999 20:44:16 +0900 (JST)
- To: vsnet
- From: Taichi Kato <tkato>
- Subject: [vsnet 1903] FY Per paper by Watanabe et al.
- Sender: owner-vsnet@kusastro.kyoto-u.ac.jp
FY Per paper by Watanabe et al.
The following article is to be published in VSOLJ Variable Star Bulletin.
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Medium-term variability of FY Per
Tsutomu Watanabe
117 Shirao dormitory , 1414 Oonakazato , Shizuoka , 418-0044 Japan
E-mail : jcc00212@nifty.ne.jp
Hiroyuki Maehara
1-13-4 Namiki , Kawaguchi , Saitama , 332-0034 Japan
E-Mail : mira@cablenet.ne.jp
The light variability of FY Per was discovered by Morgenroth (1936).
This star has been classified as a cataclysmic variable (Ritter 1990;
Zwitter & Munari 1994) or a Herbig Ae/Be star (Okazaki 1993). Richter
(1964) suggested that this star varies irregularly. Short-term variability
was discussed by Sazonov & Shugarov (1992), who claimed the detection of
the 0.064848 d period, however a more extensive study by Okazaki (1993)
could not confirm the evidence of short period variation. Sazonov &
Shugarov (1992) reported that the duration of small outbursts is about 20 d,
though more details were obscure.
The authors started intensive monitoring and obtained 140 data from 1996
July (JD 2450290) through 1999 August (JD 2451422). The original data are
listed in Table 1 and the light curve is shown in Figure 1. The smoothed
light curve between JD 2451000 and JD 2451300 which used 2-day means is shown
in Figure 2. This light curve demonstrates following characteristics ;
(1) The observed magnitude range is 11.0-12.2v.
(2) Two distinct patterns of variability exist:
(a) The star is mainly in the bright state, and short declines with
6-8 d duration are shown; for example JD 2451170 - JD 2451250.
(b) The star is mainly in the faint state, and short outbursts are
shown (faint state duration is equal to or more than bright state
duration); for example JD 2451050 - JD 2451150.
(3) Short declines and short outbursts mentioned above occurred
quasiperiodically with 20-30 d.
These characteristics seem different from the previously known characteristics
of cataclysmic variables. Further observations are strongly encouraged to get
more detail during the bright state and the faint state.
Table 1 : Observation data of FY Per
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JD-2400000 Mag. Observer JD-2400000 Mag. Observer JD-2400000 Mag.
Observer
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50290.185 12.1 Wnt 51109.205 12.5 Wnt 51196.101 11.1 Wnt
50339.210 12.0 Wnt 51111.194 11.2 Wnt 51197.069 11.2 Wnt
50383.277 11.6 Mhh 51111.236 12.0 Mhh 51199.089 11.1 Wnt
50413.082 11.4 Mhh 51119.127 11.3 Wnt 51201.064 11.1 Wnt
50418.150 11.4 Mhh 51120.994 11.5 Wnt 51205.040 11.7 Mhh
50425.212 12.0 Wnt 51125.096 11.8 Wnt 51206.956 11.2 Wnt
50450.991 11.6 Mhh 51125.240 11.9 Mhh 51208.113 11.1 Wnt
50455.927 11.7 Mhh 51125.969 11.9 Wnt 51208.960 11.0 Wnt
50467.003 11.3 Mhh 51127.131 11.9 Wnt 51209.912 11.1 Wnt
50467.050 11.2 Wnt 51128.131 11.9 Wnt 51213.965 11.1 Wnt
50483.997 11.3 Wnt 51129.124 12.0 Mhh 51216.041 11.1 Wnt
50492.045 11.5 Mhh 51129.216 11.9 Wnt 51216.963 11.3 Wnt
50499.085 11.3 Wnt 51130.078 12.1 Mhh 51218.041 11.2 Wnt
50721.202 11.2 Wnt 51131.220 11.8 Wnt 51219.165 11.3 Wnt
50730.142 12.0 Wnt 51132.994 11.9 Wnt 51220.097 11.1 Wnt
50760.973 11.2 Wnt 51135.178 11.3 Wnt 51222.058 11.3 Wnt
50761.194 11.0 Mhh 51136.162 11.1 Wnt 51222.901 11.3 Wnt
50771.199 11.5 Mhh 51137.106 11.2 Wnt 51223.997 11.5 Mhh
50771.217 11.3 Wnt 51137.169 11.5 Mhh 51224.074 11.4 Wnt
50785.103 11.3 Wnt 51141.015 11.3 Wnt 51225.085 11.4 Wnt
50810.093 11.2 Wnt 51159.165 11.8 Wnt 51227.024 11.3 Wnt
50819.218 11.1 Wnt 51165.103 12.0 Mhh 51230.023 12.0 Mhh
50832.065 11.2 Wnt 51165.135 11.7 Wnt 51230.125 11.4 Wnt
50838.023 11.2 Wnt 51166.162 11.6 Wnt 51230.991 12.2 Mhh
50838.968 11.2 Wnt 51168.078 11.9 Mhh 51232.024 12.0 Wnt
50848.136 11.1 Wnt 51169.153 11.3 Wnt 51233.017 12.2 Mhh
50855.090 11.2 Wnt 51172.167 11.5 Mhh 51233.057 11.8 Wnt
50855.938 11.1 Wnt 51173.117 11.1 Wnt 51238.044 11.2 Wnt
50879.945 11.1 Wnt 51174.007 11.2 Wnt 51241.010 11.3 Wnt
50887.949 11.2 Wnt 51176.269 11.1 Wnt 51253.910 11.4 Mhh
51017.247 11.4 Wnt 51177.053 11.2 Wnt 51265.976 11.5 Wnt
51048.256 11.9 Wnt 51179.094 12.1 Mhh 51298.974 11.3 Wnt
51050.281 12.1 Mhh 51181.112 12.2 Mhh 51369.228 11.4 Wnt
51060.156 11.4 Wnt 51184.094 11.7 Mhh 51384.267 11.7 Wnt
51061.139 11.5 Wnt 51184.176 11.1 Wnt 51390.242 11.8 Wnt
51065.294 12.1 Mhh 51186.141 11.2 Wnt 51393.198 12.0 Wnt
51073.132 12.0 Wnt 51187.028 11.2 Wnt 51398.290 12.1 Wnt
51073.255 11.7 Mhh 51188.008 11.1 Wnt 51399.251 12.3 Wnt
51075.158 12.1 Wnt 51188.099 11.3 Mhh 51400.235 12.3 Wnt
51076.165 12.2 Mhh 51189.073 11.0 Wnt 51401.281 12.1 Mhh
51082.226 11.6 Mhh 51190.017 11.0 Wnt 51402.226 12.3 Wnt
51089.186 11.6 Mhh 51190.158 11.4 Mhh 51405.194 12.3 Wnt
51089.208 11.3 Wnt 51191.042 11.0 Wnt 51408.158 12.2 Wnt
51090.215 11.3 Wnt 51192.192 11.1 Wnt 51411.283 12.1 Wnt
51096.189 12.3 Mhh 51192.990 11.4 Mhh 51412.274 12.1 Wnt
51105.115 12.3 Mhh 51194.065 11.1 Wnt 51422.271 12.2 Wnt
51109.169 11.8 Wnt 51195.156 11.1 Wnt
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The magnitudes were estimated against these GSC stars: GSC3355.646 (V=11.0),
GSC3355.883 (V=11.1), GSC3355.741 (V=11.5), GSC3355.699 (V=12.2).
Observer code : Mhh (H. Maehara) , Wnt (T. Watanabe)
Instrument: 20cm reflector + visual (H. Maehara)
32cm reflector + visual (T. Watanabe)
|
|
11 + ' .... . .::.
| :.. ' :.''''' .':.:::.: .
| ' . . ' : . .' :'. '
| ' : .' :.. .
| . ': : ' '
12 + . ' ' ' .: ': '. ' :.
| '.. ' ' .:'
| .
|
|
13 +
+---------+---------+---------+---------+---------+---------+----
50200 50400 50600 50800 51000 51200 51400
Date ( JD - 2400000 )
Figure 1: Light curve of FY Per
|
|
11 + .... ...
| . . .. :' ' .' ' .:.. :
| ' .. . . ' ' ' . '
| ' ' ' .
| . . ... '. .
12 + . . . ' . '
| ' . .' '
|
|
|
13 +
-+----------+----------+----------+----------+----------+----------+
51000 51050 51100 51150 51200 51250 51300
Date ( JD - 2400000 )
Figure 2: Smoothed light curve which used 2-day means
Acknowledgments
I would like to thank Dr.Taichi Kato (Kyoto University) for helpful
suggestions and reading the manuscript..
References
Morgenroth,O., 1936, Astron. Nachr., 261, 261
Okazaki,A., 1993, Ap&SS, 210, 227
Ritter,H., 1990, A&AS, 85, 1179
Sazonov,A.V. & Shugarov,S.YU., 1992, IBVS, 3744 ,1
Zwitter,T. & Munari,U., 1994, A&AS, 107, 503
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