COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS Number 3791 Konkoly Observatory Budapest 19 October 1992 HU ISSN 0374 - 0676 NEW RESULTS ON THE HIGH AMPLITUDE DELTA SCUTI STAR BE Lyn The variability of BE Lyn was discovered in April 1985 by Oja (1986) during routine UBV observations of astrometric standard stars. Oja (1987) and Rodriguez et al. (1990a) carried out two extensive sets of photometric observations, found the object to be a high amplitude Delta Scuti star, and published the following elements, respectively: JD hel. max.= 2446506.0074 + 0.0958697 x E (I) JD hel. max.= 2446951.41733 + 0.095869448 x E (II) The monoperiodicity of BE Lyn is also confirmed by Poretti et al. (1990). Physical parameters of the pulsating variable are published by Rodriguez et al. (1990a), Rodriguez et al. (1990b) and Garrido et al. (1990). As a result of a new set of photoelectric observations, obtained in 1991 at the 0.34m Cassegrain telescope of the Nurnberg Observatory, we present seven new times of maxima. Using a 1P21 phototube, all observations were made in V colour. The light curve of BE Lyn (April 1991) is shown in Figure 1. There seems to be an increased scatter at phase 0.1-0.3, which may be due to some bumps. The observational data is accessible on request. [FIGURE 1] Fig.1. Light curve of BE Lyn (P=0.095869483) Table 1 Photoelectric maxima of BE Lyn JD hel. max. Epoch O-C(I) O-C(II) Obs. Reference 2446498.3379 -19287 +.0001 -.0003 Oja (1987) 6507.3501 -19193 +.0005 +.0001 Oja (1987) 6507.4459 -19192 +.0005 +.0001 Oja (1987) 6508.4049 -19182 +.0008 +.0004 Oja (1987) 6509.4587 -19171 +/-.0000 -.0004 Oja (1987) 6510.4175 -19161 +.0001 -.0003 Oja (1987) 6524.4152 -19015 +.0008 +.0005 Oja (1987) 6950.4595 -14571 +.0002 +.0008 Rodriguez et al. (1990a) 6951.4174 -14561 -.0006 +/-.0000 Rodriguez et al. (1990a) 7115.6420 -12848 -.0008 +.0002 Rodriguez et al. (1990a) 7118.6131 -12817 -.0017 -.0006 Rodriguez et al. (1990a) 7118.7102 -12816 -.0005 +,0006 Rodriguez et al. (1990a) 7121.6813 -12785 -.0013 -.0003 Rodriguez et al. (1990a) 7219.5637 -11769 -.0019 -.0006 Rodriguez et al. (1990a) 7551.4645 -8302 -.0020 +/-.0000 Rodriguez et al. (1990a) 7551.5599 -8301 -.0024 -.0004 Rodriguez et al. (1990a) 7551.6560 -8300 -.0022 -.0002 Rodriguez et al. (1990a) 7553.5729 -8280 -.0027 -.0007 Rodriguez et al. (1990a) 7553.6692 -8279 -.0023 -.0003 Rodriguez et al. (1990a) 8347.3728 0 -.0039 -.0001 Wu this paper 8347.4679 1 -.0047 -.0009 Wu this paper 8357.3444 104 -.0028 +.0011 Wk/Wu this paper 8358.3988 115 -.0029 +.0009 Wk/Wu this paper 8359.3557 125 -.0047 -.0009 Gz/Wu this paper 8367.5060 210 -.0034 +.0005 Wk this paper 8624.3400 2889 -.0043 +.0002 Wk/Wu this paper Abbreviations of the observers' names: Gz = H. Garzarolli Wk = M. Wieck Wu = E. Wunder On the base of all known times of maxima, listed in Table 1, we calculated the improved elements of BE Lyn by the method of least squares: JD hel. max.=2448347.37290 + 0.095869483 x E (III) +/-18 +/-14 The difference to the elements of Oja (1987) and Rodriguez et al. (1990a) exceeds significantly the error of the new elements. We therefore propose to use the improved formula for ephemeris. E. WUNDER M. WIECK M. GARZAROLLI Nurnberg Observatory Regiomontanusweg 1 8500 Nurnberg 20, F. R. G. References: Garrido, R., Garcia-Lobo, E., Rodriguez, E., 1990, Astron. Astrophys., 234, 262 [BIBCODE 1990A&A...234..262G ] Oja, T., 1986, Astron. Astrophys. Suppl. Ser., 65, 405 [BIBCODE 1986A&AS...65..405O ] Oja, T., 1987, Astron.Astrophys., 184, 215 [BIBCODE 1987A&A...184..215O ] Poretti, E., Antonello, E., Le Borgne, J. F., 1990, Astron. Astrophys., 228, 350 [BIBCODE 1990A&A...228..350P ] Rodriguez, E., Lopez de Coca, P., Rolland, A., Garrido, R., 1990a, Rev. Mexicana Astron. Astrof., 20, 37 [BIBCODE 1990RMxAA..20...37R ] Rodriguez, E., Rolland, A., Lopez de Coca, P., 1990b, Astrophys. Space Sci., 169, 113 [BIBCODE 1990Ap&SS.169..113R ]