Modelling of W UMa-type variable stars
| Autor: | P. L. Skelton, Derck P. Smits |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2009 |
| Předmět: |
stars
Science (General) K-type main-sequence star Science Social Sciences Contact binary Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics General Biochemistry Genetics and Molecular Biology Blue straggler lcsh:Social Sciences Q1-390 Astrophysics::Solar and Stellar Astrophysics lcsh:Social sciences (General) close individual lcsh:Science lcsh:Science (General) Astrophysics::Galaxy Astrophysics Visual binary Physics H1-99 Flare star ASAS120036-3915.6 eclipsing lcsh:H Social sciences (General) T Tauri star Stars Stellar mass loss General Earth and Planetary Sciences lcsh:Q lcsh:H1-99 Astrophysics::Earth and Planetary Astrophysics General Agricultural and Biological Sciences binaries lcsh:Q1-390 |
| Zdroj: | South African Journal of Science, Volume: 105, Issue: 3-4, Pages: 120-126, Published: APR 2009 South African Journal of Science, Vol 105, Iss 3/4 (2010) |
| Popis: | Most of the stars in the sky are binary or multiple star systems. In only a small percentage of binary systems are the two stars far enough apart to be able to resolve the individual stars. The binary nature of close systems can be inferred from the periodic Doppler shifts seen in the spectral lines of the stars as they orbit their common centre of mass, or, if the orbital plane is inclined at an angle to the observer so that one star passes in front of the other, by variations in the observed brightness of the stars. These stellar systems are referred to as eclipsing binaries. The vast majority of eclipsing binaries have been found by searching for stars whose brightness varies periodically. From Newton’s Law of Universal Gravitation it can be shown that the square of the period P of a binary system is proportional to the sum of the masses m1 and m2 of the stars, i.e. P 2 ∝ (m1 + m2). |
| Databáze: | OpenAIRE |
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