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 also observed with Stromgren 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 cd-1 and 3.6035 cd-1 were obtained. We derived color indices: b - y = 0.215, m1 = 0.169, c1 = 0.783, and β = 2.775. With these indices and some calibrations, we obtain: Mv = 2.44, Mbol = 2.27, logL/L = 0.99, and log Teff = 3.875. Evolutionary sequences of stellar models with 1.00-2.00 solar masses, at steps of 0.05 M, are computed. Each sequence consists of 220 evolutionary intervals. From a comparison between the observed and calculated physical parameters we conclude that UV Thi is in an early evolutionary phase before the turn-off point.
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 Stromgren 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 cd-1 and 3.6035 cd-1 were obtained. We derived color indices: b - y = 0.215, m1 = 0.169, c1 = 0.783, and β = 2.775. With these indices and some calibrations, we obtain: Mv = 2.44, Mbol = 2.27, logL/L = 0.99, and log Teff = 3.875. Evolutionary sequences of stellar models with 1.00-2.00 solar masses, at steps of 0.05 M, are computed. Each sequence consists of 220 evolutionary intervals. From a comparison between the observed and calculated physical parameters we conclude that UV Thi is in an early evolutionary phase before the turn-off point.
基金
the National NaturalScience Foundation of China fOr the research grants. ElOy Rodrfguez acknowIedges partialresearch suPport
