Astronomy and Astrophysics – Astronomy
Scientific paper
May 1979
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979phdt.........4w&link_type=abstract
Ph.D. Thesis Florida Univ., Gainesville.
Astronomy and Astrophysics
Astronomy
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).
No associations
LandOfFree
Evolution of pre-main-sequence binary star systems does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Evolution of pre-main-sequence binary star systems, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Evolution of pre-main-sequence binary star systems will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1702841