V974 Cyg - A Triple System with Apsidal Motion

摘要: = 0.47. We observed the star during 9 nights in 2007-10 at Russian Academy ofSciences observatory near Moscow (Zvenigorod, UBV photometer, EMI 9789 photomulti-plier), Crimean of University, Ukraine (Nauchny, CCD Ap-47p),the Astrophysical Observatory, (Simeiz, VersArray 512UV) and atStar´a Lesn´a Observatory Astronomical Institute Slovak Sciences(UBVR R 2949S photomultiplier). Everywhere we used same type tele-scopes - 60cm reflectors “Zeiss-600” standard Johnson filters. The nearbystar GSC2660.3950 on frame as variable served a comparison both forCCD photoelectric observations. GSC2660.3723 (V 10.m 6) HD187072 servedas check stars for observations respectively. Using UBVmagnitudes HD186377 from SIMBAD data base, derived absolute magnitudesof under investigation Star´a observatory, see Table 1. All observationswere corrected atmospheric extinction transformed to UBVsystem.Table magnitudes starsStar V U − B remarksHD186377 5.936(2) 0.191(8) 0.123(7) HR 7502HD187072 8.790(5) 0.109(22) 0.113(16) checkGSC2660.3950 10.249(7) 0.047(15) 0.384(8) comparisonV974 Cyg 12.117(7) 0.194(11) 0.227(5) variable, platoThe CCD-observations filter were most suitable analysis lightcurve because their largest number highest precision. So them derive thegeometrical parameters system. As there are no effects proximity light ofthe system between minima, simple model two spherical revolving theelliptic orbit. results presented 2 Fig. determine colours components only. have found that thesecondary component is little bit bluer than primary, ∆(B −V) 0