The radial velocity of an object with respect to a given point is the rate of change of the distance between the object and the point. That is, the radial velocity is the component of the object's velocity that points in the direction of the radius connecting the object and the point. In astronomy, the point is usually taken to be the observer on Earth, so the radial velocity then denotes the speed with which the object moves away from or approaches the Earth.
In astronomy, radial velocity most commonly refers to the spectroscopic radial velocity, which is determined by spectroscopy. i.e. by measuring the frequencies of light received from the object. By contrast, astrometric radial velocity is determined by astrometric observations (for example, a secular change in the annual parallax).
Spectroscopic radial velocity
Light from an object with a substantial relative radial velocity at emission will be subject to the Doppler effect, so the frequency of the light decreases for objects that were receding (redshift) and increases for objects that were approaching (blueshift).
The radial velocity of a star or other luminous distant objects can be measured accurately by taking a high-resolution spectrum and comparing the measured wavelengths of known spectral lines to wavelengths from laboratory measurements. A positive radial velocity indicates the distance between the objects is or was increasing; a negative radial velocity indicates the distance between the source and observer is or was decreasing.
In many binary stars, the orbital motion usually causes radial velocity variations of several kilometers per second (km/s). As the spectra of these stars vary due to the Doppler effect, they are called spectroscopic binaries. Radial velocity can be used to estimate the ratio of the masses of the stars, and some orbital elements, such as eccentricity and semimajor axis. The same method has also been used to detect planets around stars, in the way that the movement's measurement determines the planet's orbital period, while the resulting radial-velocity amplitude allows the calculation of the lower bound on a planet's mass using the binary mass function. Radial velocity methods alone may only reveal a lower bound, since a large planet orbiting at a very high angle to the line of sight will perturb its star radially as much as a much smaller planet with an orbital plane on the line of sight. It has been suggested that planets with high eccentricities calculated by this method may in fact be two-planet systems of circular or near-circular resonant orbit. 
Detection of exoplanets
The radial velocity method to detect exoplanets is based on the detection of variations in the velocity of the central star, due to the changing direction of the gravitational pull from an (unseen) exoplanet as it orbits the star. When the star moves towards us, its spectrum is blueshifted, while it is redshifted when it moves away from us. By regularly looking at the spectrum of a star—and so, measuring its velocity—it can be determined, if it moves periodically due to the influence of a companion.
From the instrumental perspective, velocities are measured relative to the telescope's motion. So an important first step of the data reduction is to remove the contributions of
- the Earth's elliptic motion around the sun at approximately ± 30 km/s,
- a monthly rotation of ± 13 m/s of the Earth around the center of gravity of the Earth-Moon system,
- the daily rotation of the telescope with the Earth crust around the Earth axis, which is up to ±460 m/s at the equator and proportional to the cosine of the telescope's geographic latitude,
- small contributions from the Earth polar motion at the level of mm/s,
- contributions of 230 km/s from the motion around the Galactic center and associated proper motions.
- in the case of spectroscopic measurements corrections of the order of ±20 cm/s with respect to aberration.
- Dravins, Dainis; Lindegren, Lennart; Madsen, Søren (1999). "Astrometric radial velocities. I. Non-spectroscopic methods for measuring stellar radial velocity". Astron. Astroph. 348: 1040–1051. Bibcode:1999A&A...348.1040D.
- Anglada-Escude, Guillem; Lopez-Morales, Mercedes; Chambers, John E. "How eccentric orbital solutions can hide planetary systems in 2:1 resonant orbits". The Astrophysical Journal Letters. 709 (1): 168–78. arXiv: . Bibcode:2010ApJ...709..168A. doi:10.1088/0004-637X/709/1/168.
- Kürster, Martin; Trifonov, Trifon; Reffert, Sabine; Kostogryz, Nadiia M.; Roder, Florian (2015). "Disentangling 2:1 resonant radial velocity oribts from eccentric ones and a case study for HD 27894". Astron. Astroph. 577: A103. arXiv: . doi:10.1051/0004-6361/201525872.
- Ferraz-Mello, S.; Michtchenko, T. A. (2005). "Extrasolar Planetary Systems". Lect. Not. Phys. 683. pp. 219–271. Bibcode:2005LNP...683..219F. doi:10.1007/10978337_4.
- Reid, M. J.; Dame, T. M. (2016). "On the rotation speed of the Milky Way determined from HI emission". arXiv: .
- Stumpff, P. (1985). "Regiorous treatment of the heliocentric motion of stars". Astron. Astroph. 144: 232. Bibcode:1985A&A...144..232S.