COMMISSION 27 OF THE I.A.U. INFORMATION BULLETIN ON VARIABLE STARS Number 3000 Konkoly Observatory Budapest 16 March 1987 HU ISSN 0374 - 0676 VARIABLE NATURE OF Be STARS In an earlier communication, we (Kilambi et al., 1986) had reported the photoelectric variable nature of six B-emission line stars, HR 1508, HR 1789, HR 2538, HR 2996, HR 5193 and HD 45677 observed through Red and near Infrared passbands of the Johnson's system. In continuation of it, we are reporting the variable/non-variable nature of the remaining B-emission line objects observed during 1982-83 observing season. The observational procedure, the extinction correction and the standardization procedure followed are already published in the previous communication by Kilambi et al.(1986). Table I gives the observations of these stars and the columns are self explanatory. The mean internal probable error of a single measurement in 'R' and (R-I) is +-0.02m and +-0.03m, respectively. A few of the programme stars were observed earlier by Johnson (1965, 1966), Mendoza (1958) and Feinstein and Marraco (1979) on the standard RI system. These observations are also incorporated in the determination of variable/non-variable nature of the stars. TABLE I Star Spectral Heliocentric R (R-I) type Date of observation (J.D.2440000+ ) Phi And B7 Ve 5315.1150 + 4.26 -0.00 HR 335 5315.1160 4.25 0.00 HD 6811 gamma Cas B0 1Ve 5315.1027 2.30 -0.11 HR 264 5315.1036 2.30 -0.08 HD 5394 Phi Per B2 Ve 5315.1232 3.92 0.01 HR 496 5315.1238 3.91 0.03 HD 10516 HR 985 B2.5 Ven 5315.1684 5.11 -0.05 HD 20336 5315.1689 5.10 -0.03 Psi Per B5 Ve 5315.1756 4.18 -0.01 HR 1087 5315.1764 4.18 -0.01 HD 22192 AB Aur B9q 5356.2660 6.95 +0.03 HD 31293 5356.2667 6.95 +0.03 HD 31648 A2q 5356.2778 7.56 +0.06 5356.2789 7.55 +0.07 Zeta Tau B2IIIe 5315.3055 2.94 -0.11 HR 1910 5315.3062 2.94 -0.11 HD 37202 HD 37806 A0e 5356.3151 7.82 -0.01 5356.3158 7.84 -0.04 HR 2142 B2Ve 5315.3359 5.06 +0.0S 5315.3366 5.05 +0.06 5324.3636 5.08 +0.04 5324.3643 5.08 +0.04 17 Lep A0 + M1 5315.3422 4.34 +0.54 5315.3428 4.34 +0.54 5324.3925 4.36 +0.50 5324.3931 4.35 +0.50 13 Mon A0 5324.4027 4.50 -0.02 HR 2385 5324.4033 4.50 -0.02 HD 46300 S Mon 07f 5324.4104 4.78 -0.11 HR 2456 5324.4114 4.78 -0.11 HD 47839 HD 50138 B6 IIIe 5356.3702 6.72 +0.06 5356.3707 6.72 +0.0S Omicron Pup B0V pe: 5356.3882 4.37 +0.06 HR 3034 5356.3887 4.37 +0.07 HD 63462 HR 3858 B5e 5356.3980 4.78 -0.09 HD 83953 5356.3986 4.74 -0.04 HR 3946 B5e 5356.4048 6.30 -0.07 HD 86612 5356.4053 6.29 -0.08 HR 4123 B9Ven: 5356.4111 5.62 -0.06 HD 91120 5356.4124 5.63 -0.02 Zeta Crv B8e 5437.3371 5.26 -0.14 HR 4696 5437.3378 5.25 -0.12 HD 107348 Theta CrB B6Vnne 5437.3543 4.12 -0.16 HR 5778 5437.3549 4.12 -0.16 HD 138749 4 Her B7e 5437.3959 5.77 -0.17 HR 5938 5437.3970 5.78 -0.18 HD 142926 48 Lib B5 IIIpe 5437.4063 4.93 -0.13 HR 5941 5437.4068 4.93 -0.13 HD 142983 Chi Oph B2 IVpe 5437.4135 4.00 +0.11 HR 6118 5437.4142 4.00 +0.09 HD 148184 HD 259431 B5e 5356.3363 8.22 +0.21 5356.3370 8.22 +0.21 Figure 1-16: Variable/non-variable nature of Be stars. Red magnitudes (filled circles), infrared magnitudes (filled triangles). [FIGURE 1] [FIGURE 2] [FIGURE 3] [FIGURE 4] REMARKS : HR 335: Slightly brighter than 1963 observations. HR 264: No change in brightness, but yet reported as a variable with V = 1.6-3.0 in the literature. HR 496: No change in brightness since early 1962. Double-lined spectroscopic binary with P=126.7 days. HR 985: More or less constant in brightness. HR 1087: No change in brightness in both R, I passbands. HR 1910: The present observations are comparable with that of late 1963 measurements, eventhough, some fainter values were recorded in the early part of 1964. Single-lined spectroscopic binary with P= 132.91 days and reported as variable with V= 2.9-3.0. HR 2142: No change in brightness. HR 2358: No change in brightness. HR 2456: No change in brightness. HR 3034: Eventhough, it was fainter in the early part of 1964, but brightened in late 1966 and since then, maintained more or less constant brightness. HR 3858: No change in brightness except for minor fluctuations. HR 3946: The present R, I magnitudes agree with that of early 1970 observations, eventhough, it was brighter by almost 0m.2 in 1975. HR 5778: No change in brightness. HR 5941: No change in brightness, but reported as variable with V=4.8- 5.0 in the literature. HR 6118: No change in brightness in R passband but, slightly fainter in I passband. G.C. KILAMBI, P. VIVEKANANDA RAO, M.B.K. SARMA Centre of Advanced Study in Astronomy, Osmania University, HYDERABAD (India) References : Feinstein, A and Marraco, R.G., 1979, Astron. J. 84, 1713. [BIBCODE 1979AJ.....84.1713F ] Johnson, H.L., 1965, Astrophys. J. 141. 923. [BIBCODE 1965ApJ...141..923J ] Johnson, H.L., 1966, Comm. Lunar and Planetary-Labs., 4, 99, [BIBCODE 1966CoLPL...4...99J ] Kilambi, G.C., Vivekananda Rao, P. and Sarma, M.B.K., 1986, I.B.V.S. No. 2950. Mendoza, V.E.E., 1958, Astrophys. J. 128, 207. [BIBCODE 1958ApJ...128..207M ]