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한국우주과학회 편집위원회
Properties of the Variation of the Infrared Emission of OH/IR Stars
Mee-Ju Kim1, Yun-Deuk Jeong2, Pyung-Kil Min2†
1
Department of Astronomy and Space Science, Hankook University, Seoul 120-763, Korea
Department of Astronomy and Space Science, Seoul University, Seoul 170-293, Korea
2
†
Corresponding Author
E-mail: [email protected]
Tel: +82-2-2123-2300 Fax: +82-2-2123-2302
Received Nov 1, 2010 Revised Nov 21, 2010 Accepted Dec 3, 2010
Heading Title: Mee-Ju Kim et al. The M band Light Curves of OH/IR stars
article type: Research Paper
ABSTRACT
To study properties of the pulsation in the infrared emission for long period variables, we have collected and
analyzed the infrared observational data at M band for 12 OH/IR stars. We present the light curves using the
data that cover about 30 years including ……
Keywords: asymptotic giant branch and post-asymptotic giant branch, infrared: stars
1. INTRODUCTION
Stars with low and intermediate mass evolve into the asymptotic giant branch (AGB) before the
evolutionary stage of planetary nebulae. The OH/IR stars are generally believed to be the last evolutionary
phase of an ….
The Infrared Space Observatory (ISO, Kessler et al. 1996) with improved sensitivity and angular
resolution had performed ….
2. SAMPLE STARS
For this paper, we choose 12 OH/IR stars which have a wide range of pulsation periods (400 - 1,800
days). The sample stars are same as those used in paper II. We present the OH name of sample stars, the
general catalogue of variable stars (GCVS) name, …
3. RESULTS AND DISCUSSION
In Fig. 1, we plot the light curves for 12 OH/IR stars using the observation data (presented by symbols) at
M band with the best fitting sinusoidal curve (presented by a solid line). The sinusoidal curve, which is a
function of time (t), is in the form
y0 + Asin (2π t / P + q),
(1)
where y0 is the mean-brightness, A and P are …
We neglect the long-term trends caused by a secondary period within the time range of observation data.
The data points that do not follow the general trend are not used for determination of the pulsation
parameters. These unused data points are marked by parenthesis in Table 2 and the light curves (Fig. 1).
In Table 3, we list the new pulsation ….
…. OH maser observations by Herman & Habing (1985). The period of IK Tau from Hale et al. (1997) was
based on variations in 11 μm flux.
4. CONCLUSIONS
We have made the light curves at M band for 12 OH/IR stars. We have determined the pulsation
parameters of the sample stars and compared them with previous results of the infrared and radio …..
ACKNOWLEDGMENTS
This work was supported by the …..
REFERENCES
Clarkson WI, Charles PA, Coe MJ, Laycock S, Tout MD, et al., Long-term properties of accretion discs in
X-ray binaries - I. The variable third period in SMC X-1, MNRAS, 339, 447-454 (2003).
http://dx.doi.org/10.1046/j.1365-8711.2003.06176.x
Gruber DE, Rothschild RE, SMC X-1 variability observed from HEAO 1, ApJ, 283, 546-551 (1984).
http://dx.doi.org/10.1086/162338
Huang NE, Shen Z, Long SR, Wu MC, Shih HH, et al., The empirical mode decomposition and the Hilbert
spectrum for nonlinear and non-stationary time series analysis, Proc. R. Soc. Lond. A, 454, 903-995
(1998). http://dx.doi.org/10.1098/rspa.1998.0193
Moon DS, Eikenberry SS, Discovery of Coupling between Periodic and Aperiodic Variability and X-Ray
Quasi-periodic Oscillations from Hercules X-1, ApJ, 552, L135-L139 (2001).
http://dx.doi.org/10.1086/320330
Reynolds AP, Hilditch RW, Bell SA, Hill G, Optical spectroscopy of the massive X-ray binary SM X-1/Sk
160, MNRAS, 261, 337-345 (1993).
Still M, Boyd P, Fine-Turning the Accretion Disk Clock in Hercules X-1, ApJ, 606, L135-L138 (2004).
http://dx.doi.org/10.1086/421349
van der Meer A, Kaper L, van Kerkwijk MH, Heemskerk MHM, van den Heuvel EPJ, Determination of the
mass of the neutron star in SMC X-1, LMC X-4, and Cen X-3 with VLT/UVES, A&A, 473, 523-538
(2007). http://dx.doi.org/10.1051/0004-6361:20066025
Wijers RAMJ, Pringle JE, Warped accretion discs and the long periods in X-ray binaries, MNRAS, 308,
207-220 (1999). http://dx.doi.org/10.1046/j.1365-8711.1999.02720.x
Wojdowski P, Clark GW, Levine AM, Woo JW, Zhang SN, Quasi-periodic Occultation by a Precessing
Accretion Disk and Other Variabilities of SMC X-1, ApJ, 502, 253-264 (1998).
http://dx.doi.org/10.1086/305893
-10.4
(
)
Willems & de Jong 1982
Engels 1982
OH 26.4-1.9 (M Band)
Fix & Mutel 1984
Herman et al. 1984
Gehrz et al. 1985
Nyman et al. 1993
Period : 493 ± 4.78 (day)
Amplitude : 0.29 ± 0.035
-10.6
-2
Log [ F(Wm )]
(
)
-10.8
-11.0
-11.2
3000
4000
5000
6000
7000
8000
JD 2440000+
OH 26.5+0.6 (M Band)
-9.4
Evans & Beckwith 1977
Lebofsky et al. 1978
Period : 1564 ± 9.62 (day)
Amplitude : 0.45 ± 0.026
Ney & Merrill 1980
Werner et al. 1980
Engels 1982
Willems & de Jong 1982
Grasdalen et al. 1983
Le Bertre 1993
-2
Log [ F(Wm )]
-9.6
-9.8
-10.0
-10.2
(
-10.4
Jones et al. 1990
Nyman et al. 1993
)
(
2000
3000
4000
5000
6000
7000
8000
JD 2440000+
Fig. 1. M band light curves of OH/IR stars.
3.5
3.0
AmplitudeM [mag]
2.5
2.0
1.5
OH 42.3-0.1
1.0
1.0
1.5
2.0
2.5
AmplitudeL [mag]
Fig. 2. Amplitudes at L and M bands.
3.0
3.5
Lepine et al. 1995
ISO SWS01
)
4.0
9000
10000
11000
Table 1. Sample stars.
OH name
GCVS
26.2-0.6
26.4-1.9
26.5+0.6
28.7-0.6
30.1-0.2
30.7+0.4
32.8-0.3
39.9+0.0
42.3-0.1
45.5+0.1
127.8+0.0
178.0-31.4
V0438 Sct
V0440 Sct
V0437 Sct
V0439 Sct
V1361 Aql
V1360 Aql
V1365 Aql
V1367 Aql
V1368 Aql
V1369 Aql
V669 Cas
IK Tau
l.
(degree)
26.2092
26.4221
26.5434
28.7192
30.1369
30.7171
32.8271
39.9162
42.3081
45.4722
127.8147
177.9544
b.
Dist.
(degree) (kpc)
4.1
-00.5893
3.4
-01.9346
+00.6178 1.4
2.8
-00.5787
3.3
-00.2322
+00.4278 5.2
3.9
-00.3155
+00.0182 5.6
6.5
-00.1330
+00.0749 2.5
1.6
-00.0208
0.3
-31.4119
GCVS: general catalogue of variable stars.
Table 2. New pulsation parameters.
Period (day)
This work Previous
Radio
26.2-0.6
1,193±9.8 1330±50 1,181±13
26.4-1.9
493±4.8
540±20
652±26
26.5+0.6
1,564±9.6 1,630±100 1,566±16
28.7-0.6
641±6.3
640±10
627±17
30.1-0.2
923±8.5
970±40
853±21
30.7+0.4 1,158±54.2 1,140±30 1,039±27
32.8-0.3 1,729±15.5 1,750±130 1,536±10
39.9+0.0
771±7.1
770±20
823±45
42.3-0.1 1,723±24.9 1,650±150 1,945±83
45.5+0.1
721±5.8
720±20
760±31
127.8+0.0 1,506±13.8 1,537±18a) 1,994±130
IK Tau
466±0.8
470±72) 455.6±57
a)
Suh & Kim (2002), b) Hale et al. (1997).
Objects
Amplitude (mag) <m> (mag)
This work Previous
1.80±0.22 1.77
2.57±0.18
1.45±0.17 1.37
2.18±0.14
2.25±0.13 1.97
-0.36±0.09
2.00±0.23 1.30
1.67±0.18
1.55±0.14 1.52
2.10±0.10
2.55±0.27 1.61
2.80±0.20
2.90±0.20 2.68
2.70±0.15
2.00±0.27 1.49
3.02±0.19
1.05±0.17 0.72
4.44±0.13
1.50±0.19 1.45
3.12±0.13
2.00±0.18 2.00a)
0.74±0.30
1.15±0.08
-2.70±0.05