| Photometric Observations of the δ Scuti Star UV Trianguli and its Evolutionary Status |
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| 引用本文： | Zong－LiLiu,Ai－YingZhou,等.Photometric Observations of the δ Scuti Star UV Trianguli and its Evolutionary Status[J].中国天文和天体物理学报,2002,2(1):59-65. |
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| 作者姓名： | Zong－LiLiu Ai－YingZhou 等 |
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| 作者单位： | Zong~Li Liu1 *，Ai-Ying Zhou1 and E. Rodriguez2 1 National Astronomical Observatories，Chinese Academy of Sciences，Beijing 100012 2 Instituto de Astrofisica de Andalucia，CSIC，P. O. Box 3004，E-18080 Granada，Spain Formation，structure and evolution of |
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| 基金项目： | the National Natural
Science Foundation of China fOr the research grants. ElOy Rodrfguez acknowIedges partial
research suPport |
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| 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 Stroemgren uvby Hβ 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 0.05M⊙,are computed. Each sequence consists of 220 evolutionary 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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| 关 键 词： | 三角星座 UV型星 光度计 发展趋势 |
Photometric Observations of the δ Scuti Star UV Trianguli and its Evolutionary Status |
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| ZongLi Liu,AiYing Zhou,E.Rodrfguez.Photometric Observations of the δ Scuti Star UV Trianguli and its Evolutionary Status[J].Chinese Journal of Astronomy and Astrophysics,2002,2(1):59-65. |
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| Authors: | ZongLi Liu AiYing Zhou ERodrfguez |
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| Institution: | NationalAstronomicalObservatories,ChineseAcademyofSciences,Beijing100012 |
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| Abstract: | 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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