The radial velocity or line-of-sight velocity of a target with respect to an observer is the rate of change of the vector displacement between the two points. It is formulated as the vector projection of the target-observer relative velocity onto the relative direction or line-of-sight (LOS) connecting the two points.
The radial speed or range rate is the temporal rate of the distance or range between the two points. It is a signed scalar quantity, formulated as the scalar projection of the relative velocity vector onto the LOS direction. Equivalently, radial speed equals the norm of the radial velocity, modulo the sign.
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 the Earth (or approaches it, for a negative radial velocity).
Given a differentiable vector
r\inR3
Let the instantaneous relative velocity of the target with respect to the observer be
The magnitude of the position vector
r
The quantity range rate is the time derivative of the magnitude (norm) of
r
Substituting into
| r |
=
| d\langler,r\rangle1/2 | |
| dt |
Evaluating the derivative of the right-hand-side by the chain rule
| r |
=
| 1 | |
| 2 |
| d\langler,r\rangle | |
| dt |
| 1 | |
| r |
| r |
=
| 1 | |
| 2 |
| ||||||||||
| r |
using the expression becomes
| r |
=
| 1 | |
| 2 |
| \langlev,r\rangle+\langler,v\rangle | |
| r |
By reciprocity,[1]
\langlev,r\rangle=\langler,v\rangle
\hat{r}=r/{r}
| r |
=
| \langler,v\rangle | |
| r |
=\langle\hat{r},v\rangle
i.e., the projection of the relative velocity vector onto the LOS direction.
Further defining the velocity direction
\hat{v}=v/{v}
v=\|v\|
| r |
=v\langle\hat{r},\hat{v}\rangle=v\langle\hat{r},\hat{v}\rangle
A singularity exists for coincident observer target, i.e.,
r=0
In astronomy, radial velocity is often measured to the first order of approximation by Doppler spectroscopy. The quantity obtained by this method may be called the barycentric radial-velocity measure or spectroscopic radial velocity.[2] However, due to relativistic and cosmological effects over the great distances that light typically travels to reach the observer from an astronomical object, this measure cannot be accurately transformed to a geometric radial velocity without additional assumptions about the object and the space between it and the observer.[3] By contrast, astrometric radial velocity is determined by astrometric observations (for example, a secular change in the annual parallax).[3] [4] [5]
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.
William Huggins ventured in 1868 to estimate the radial velocity of Sirius with respect to the Sun, based on observed redshift of the star's light.[6]
In many binary stars, the orbital motion usually causes radial velocity variations of several kilometres 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.[7] [8]
See main article: Doppler spectroscopy. 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 an exoplanet 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