COMMISSION 27 OF THE I. A. U. INFORMATION BULLETIN ON VARIABLE STARS Number 921 Konkoly Observatory Budapest 1974 September 5 Veroffentlichungen der Remeis-Sternwarte Bamberg Astronomisches Institut der Universitat Erlangen-Nurnberg Band X, Nr. 111 Rosemary Hill Observatory, University of Florida Contribution No. 46 NEW SOUTHERN VARIABLE STARS On sky patrol plates taken at the Southern Station of the University of Florida, Gainesville and the Remeis-Sternwarte, Bamberg, located at the Mount John Observatory, New Zealand, the 13 stars of the following list were found to be variable (10 new stars and 3 confirmations of stars in the Catalogue of Suspected Variables). For the first time in 1973, simultaneous plates were taken in two colors on Kodak 103a-O (blue sensitive) and Kodak 103a-E (red sensitive). Thus estimates of color or spectral type can now be made, which aids in variable type identification. The brightnesses of these stars were estimated by comparison with standard stars in the Harvard-Groningen Atlas, Selected Areas (1965, A. Brun and H. Vehrenberg). Red photographic magnitudes are marked with an asterisk (*). Finding charts, 1deg in declination, with south up, are also given. Maximum Ampl. Remarks BV-Nr. RA Dec. Brightness pg 1900.0 BV 1609 Lep = 5h14m50s -13deg56'.7 12.0* 4m.0 x 1 = CSV 544 = Ross 351 BV 1610 Lep = 5h18m06s -13deg53'.6 12.2* 0.6 2 BV 1611 Lep = 5 19 40 -14 11.5 11.6* 0.5 3 BV 1612 Ori = 5 19 45 -10 44.8 11.7 0.5 4 BV 1613 Lep = 5 21 09 -14 28.4 11.6* 2.9 5 BV 1614 Ori = 5 22 04 -09 18.7 11.5* 2.1 6 BV 1615 Lep = 5 56 27 -12 12.1 13.4* 0.2 7 BV 1616 Lep = 6 05 10 -13 05.9 11.6* 4.5 x 8 = CSV 717 = Ross 354 BV 1617 Mon = 6h18m26s -10deg02'.3 12.4 1.2 9 BV 1618 Mon = 6 22 10 -10 11.7 13.6 1.1 10 BV 1619 CMa = 6 43 12 -13 33.0 12.1 1.3 11 = CSV 873 = S 3773 BV 1620 CMa = 6h44m18s -16deg28'.3 13.4 0.1 12 BV 1621 CMa = BD-16deg1860(8m.0) = HD 56429 (A0) 0.6 13 x Amplitude until plate limit (15m.5) Remarks: 1) BV 1609 is a long period variable with the following maxima: JD 243 9054.521 JD 243 9083.476 JD 244 0589.336 9059.510 9768.578 0590.336 9060.506 9769.588 0592.335 9082.466 244 0585.343 1980.134 1983.097 2) BV 1610 is an Algol-type eclipsing binary with a small color difference - probably an early F star. The following minima were found. JD 243 9054.521 JD 244 2035.969 9060.507 2038.960 3) Much structure is evident in the light curve of BV 1611, with many more minima than maxima. Although much past information exists for this star, efforts failed to yield a period. 4) BV 1612 had small amplitude variation in 1973 (0m.2-0m.5). It was at least 3m fainter in 1965 (below the plate limit). It reappeared faintly in October 1966 with more small amplitude variation. 5) BV 1613 is probably a Mira type variable, whose minima are below the plate limit on blue plates. Efforts failed to yield a period. 6) BV 1614 shows many more minima than maxima. 7) BV 1615 is a late type eclipsing binary which is below the plate limit in the blue at minimum. 8) BV 1616 is an eclipsing binary with a long period probable. 9) BV 1617 is prominent on the red plates, but just above the plate limit on the blue plates. 10) BV 1618 is a late type eclipsing binary. 11) BV 1619 is an RR-Lyrae type variable, whose preliminary ephemeris can be given by Max = JD 243 8739.506 + 0d.452239 +- 0.000007 The following maxima were found: Maximum E O-C Maximum E O-C JD 243 8739.506 0 0d.000 JD 243 9118.455 838 -0d.028 8759.432 44 0.027 9139.378 884 0.093 8768.403 64 -0.046 9167.324 546 -0.001 8797.329 128 -0.064 9181.285 977 -0.059 8798.322 130 0.026 9444.539 1559 -0.009 8812.271 161 -0.046 9450.515 1572 0.089 8813.271 163 0.050 244 0566.508 4040 -0.047 8817.269 172 -0.023 0685.015 4302 -0.027 8818.268 174 0.072 0709.951 4357 0.037 8822.266 183 0.000 2039.047 7256 0.000 No other periods between 0d.3 and 53d.6 were found. 12) BV 1620 is just east of a star of similar brightness which makes a good comparison star. The variable was much fainter in 1965 until regaining the 1973 level in November 1966. Small amplitude variations are superimposed on this long term variation. 13) BV 1621 is probably an eclipsing system with only two minima observed, JD 243 8814.270; JD 244 2038.045. Bamberg, August, 1974 N. L. MARKWORTH Remeis-Sternwarte Bamberg and University of Florida Gainesville [FIGURE 1] [FIGURE 2] [FIGURE 3] [FIGURE 4] [FIGURE 5] [FIGURE 6] [FIGURE 7] [FIGURE 8] [FIGURE 9] [FIGURE 10] [FIGURE 11] [FIGURE 12]