This is a spectroscopic binary star system with an estimated period of 2,500 days.

Despite this, it is suspected of being a spectroscopic binary star.

The second component is a spectroscopic binary star system.

He concluded that it was in orbit in a spectroscopic binary star system with a period of about 100 days.

Alpha Equulei is a unique spectroscopic binary star consisting of two components.

Astronomy: a kind of spectroscopic binary star.

This is a single-lined spectroscopic binary star system that belongs to the Pleiades group.

It is a spectroscopic binary star, located about 3 north of Mu Geminorum.

Omega-2 Tauri is a white A-type spectroscopic binary star with an apparent magnitude of +4.93.

Epsilon Ceti is a spectroscopic binary star.

It is a spectroscopic binary star, one in which the companion star is only known through analysis of the spectra.

Gliese 678 is a spectroscopic binary star system approximately 60 light-years away in the constellation of Ophiuchus.

Theta Cephei is a white spectroscopic binary star, located about 135 light-years from Earth.

Along with Carl Vogel, Pickering discovered the first spectroscopic binary stars.

Conversely, spectroscopic binary stars move fast in their orbits because they are close together, usually too close to be detected as visual binaries.

Capella was discovered, in 1899, to be a spectroscopic binary star, period 104 days, the two nearly equal components being inseparable in our largest telescopes.

HD 176051 is a spectroscopic binary star system located approximately 49 light years away from Earth, in the constellation Lyra.

In 1958, American astronomer Horace W. Babcock discovered that this is a spectroscopic binary star.

Atik is a spectroscopic binary star consisting of a spectral type B1 giant and a type B3 dwarf orbiting each other every 4.5 days.

It consists of what appears to be a visual binary star which, upon closer inspection, can be seen to consist of two spectroscopic binary stars.

The Struve-Sahade effect (S-S effect) occurs with a double-lined spectroscopic binary star system.

Pi Orionis (π Ori, π Orionis) is a spectroscopic binary star in the constellation Orion.

This is a spectroscopic binary star system, with the presence of the secondary component being revealed by the shifts of absorption lines in the spectrum resulting from the Doppler effect.

This is a spectroscopic binary star system consisting of a pair of stars orbiting around each other with a separation that can not currently be resolved with a conventional telescope.

Epsilon Herculis (ε Her, ε Herculis) is a fourth-magnitude spectroscopic binary star in the constellation Hercules.