【摘 要】
：
UV Tri was observed photometrically from 1999 to 2000 at the Xinglong Station of the National Astronomical Observatories, Chinese Academy of Sciences,and was al
【机 构】
：
National Astronomical Observatories
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UV Tri was observed photometrically from 1999 to 2000 at the Xinglong Station of the National Astronomical Observatories, Chinese Academy of Sciences,and was also observed with StrSmgren uvbyHβ filter system at the Sierra Nevada Observatory (Spain) in 2000. From period analyses of the data, three pulsation frequencies, 9.3299 c d-1, 10.8483 c d-1 and 3.6035 c d-1 were obtained. We derived color indices: b - y = 0.215, m1 = 0.169, c1 = 0.783, andβ = 2.775. With these indices and some calibrations, we obtain: My = 2.44, Mbol = 2.27, log L/L⊙ =0.99, and log Teff= 3.875. Evolutionary sequences of stellar models with 1.00-2.00solar masses, at steps of 0.05 M⊙, are computed. Each sequence consists of 220evolutionary intervals. From a comparison between the observed and calculated physical parameters we conclude that UV Tri is in an early evolutionary phase before the turn-off point.
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