Radial-velocity planets are those detected indirectly by observing the orbital motion of their host stars in response to the gravitational pull of the planets. The stellar motion is measured from the Doppler effect on the stellar spectral lines.
In a system consisting of a star and a planet, because of the gravitational force of the planet on the star, the planet and its host star orbit their common center of mass. This causes variations in the distance of the star to the observer creating what is known as radial velocity. Measuring the velocities of stars along the line of sight dates back to more than a century ago. However, it has been only in the past couple of decades that technological advancements reached to the point where the precision was good enough to detect the very small accelerations of a host star induced by orbiting planets. The first serious survey using radial velocity to search for planets around other stars was pursued by a team of Canadian...
KeywordsDoppler shift Radial velocity Spectroscopic orbit
References and Further Reading
- Campbell B, Walker GAH, Yang S (1988a) A search for planetary mass companions to nearby stars. In: Bioastronomy – the next steps; Proceedings of the ninety-ninth IAU Colloquium, Balaton, Hungary, 22–27 June 1987 (A88-55201 24-88). Kluwer, Dordrecht, pp 83–90Google Scholar
- Haghighipour N (2010) Planets in binary star systems. Astrophysics and Space Science Library, vol 366. Springer. ISBN 978-90-481-8686-0Google Scholar