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An eclipsing binary star is a binary star system in which the orbital plane of the two stars lies so nearly in the line of sight of the observer that the components undergo mutual eclipses. [20] In the case where the binary is also a spectroscopic binary and the parallax of the system is known, the binary is quite valuable for stellar analysis.
If the accretor in an X-ray binary has a minimum mass that significantly exceeds the Tolman–Oppenheimer–Volkoff limit (the maximum possible mass for a neutron star), it is expected to be a black hole. This is the case in Cygnus X-1, for example, where the radial velocity of the companion star has been measured. [13] [14]
Kepler-47 is a binary star system located about 1,055 parsecs (3,440 light-years) away from Earth. [14] The binary system is composed of a G-type main sequence star (Kepler-47A) and a red dwarf star (Kepler-47B). The stars orbit each other around their barycenter, or center of mass between them, completing one full orbit every 7.45 days. [4]
In astronomy, the Roche lobe is the region around a star in a binary system within which orbiting material is gravitationally bound to that star. It is an approximately teardrop-shaped region bounded by a critical gravitational equipotential , with the apex of the teardrop pointing towards the other star (the apex is at the L 1 Lagrangian point ...
An example of a visual binary: Theta1 Orionis C1 (lower) and C2 (upper), as imaged by VLT/GRAVITY. A visual binary is a gravitationally bound binary star system [1] that can be resolved into two stars. These stars are estimated, via Kepler's third law, to have periods ranging from a few years to thousands of years. A visual binary consists of ...
The most common kinds of binary system are binary stars and binary asteroids, but brown dwarfs, planets, neutron stars, black holes and galaxies can also form binaries. A multiple system is similar but consists of three or more objects, for example triple stars and triple asteroids (a more common term than 'trinary').
FU Orionis is a variable and binary star [9] system in the constellation of Orion, that in 1937 rose in apparent visual magnitude from 16.5 to 9.6, and has since been around magnitude 9. [ 10 ] [ 3 ] The name FU Orionis is a variable star designation in the Argelander system, which are assigned sequentially as new variables are discovered. [ 11 ]
Stages in the life of a binary system as a common envelope is formed. The system has mass ratio M1/M2=3. The black line is the Roche equipotential surface. The dashed line is the rotation axis. (a) Both stars lie within their Roche lobes, star 1 on the left (mass M1 in red) and star 2 on the right (mass M2 in orange).