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Sirius is a binary star system consisting of two white stars orbiting each other with a separation of about 20 AU (roughly the distance between the Sun and Uranus) and a period of 50.1 years.
It is a binary star system, consisting of a yellow-white main sequence star of spectral type F5 IV-V, named Procyon A, and a faint white dwarf companion of spectral type DA, named Procyon B.
What the naked eye perceives as a single star is actually a binary star system, consisting of a white main-sequence star of spectral type A1V, termed Sirius A, and a faint white dwarf companion of spectral type DA2, called Sirius B. The distance separating Sirius A from its companion varies between 8.2 and 31.5 AU.
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This closely orbiting binary star system consists of a main sequence star and a white dwarf 31 million kilometres apart.
The star system 59 Serpentis, also known as d Serpentis, is a triple star system consisting of a spectroscopic binary containing an A-type star and an orange giant and an orange giant secondary.
It is a multiple star system consisting of three B-type stars, the spectroscopic binary α1 and α2, that are of roughly the same brightness and are close enough together to appear as one star to the naked eye.
In all likelihood this is a binary star system containing a low-mass normal star and a nonluminous companion.
If the images of the two components of a binary star system can be separated by telescope, it is called a visual binary.
In the case of a binary star system where one of the stars (star 1) increases its size, star 1 will reach a limiting surface.
Now two astronomers have found a second dusty ring, this one around a binary star system.
The radial velocity measurements confirmed that the binary star system was actually speeding away from us.
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