Evolution of pre-main-sequence binary star systems

Astronomy and Astrophysics – Astronomy

Scientific paper

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Binary Stars, Stellar Evolution, Astronomical Models, Stellar Mass

Scientific paper

A quasistatic polytropic model representing the pre-main-sequence contraction phase was applied to both components of close binary star systems. Models were calculated for eleven observed semi-detached close binaries published in the literature and the results were compared with the observed systems. The names and ages of the three that are likely to be pre-main-sequence are: U Caphei (610,000 years), X Trianguli (4.6 million years), and W Ursae Minoris (1.87 million years). The following four systems were found not to fit the pre-main-sequence model in this investigation: TV Cassiopeia, AI Draconis, Beta Persei, and TX Ursae Majoris. The following four systems could be pre-main-sequence with modifications to the model: Im Aurigae (350,000 years), delta Librae (820,000 years), U Sagittae (378,000 years), and V505 Sagittarii (1.89 million years).

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