|This article needs additional citations for verification. (August 2006) (Learn how and when to remove this template message)|
Spherical aberration is an optical effect observed in an optical device (lens, mirror, etc.) that occurs due to the increased refraction of light rays when they strike a lens or a reflection of light rays when they strike a mirror near its edge, in comparison with those that strike nearer the centre. It signifies a deviation of the device from the norm, i.e., it results in an imperfection of the produced image.
A spherical lens has an aplanatic point (i.e., no spherical aberration) only at a radius that equals the radius of the sphere divided by the index of refraction of the lens material. A typical value of refractive index for crown glass is 1.5 (see list), which indicates that only about 43% of the area (67% of diameter) of a spherical lens is useful. It is often considered to be an imperfection of telescopes and other instruments which makes their focusing less than ideal due to the spherical shape of lenses and mirrors. This is an important effect, because spherical shapes are much easier to produce than aspherical ones. In many cases, it is cheaper to use multiple spherical elements to compensate for spherical aberration than it is to use a single aspheric lens.
"Positive" spherical aberration means peripheral rays are bent too much. "Negative" spherical aberration means peripheral rays are not bent enough.
The effect is proportional to the fourth power of the diameter and inversely proportional to the third power of the focal length, so it is much more pronounced at short focal ratios, i.e., "fast" lenses.
For simple designs one can sometimes calculate parameters that minimize spherical aberration. For example, in a design consisting of a single lens with spherical surfaces and a given object distance o, image distance i, and refractive index n, one can minimize spherical aberration by adjusting the radii of curvature and of the front and back surfaces of the lens such that
For small telescopes using spherical mirrors with focal ratios shorter than f/10, light from a distant point source (such as a star) is not all focused at the same point. Particularly, light striking the inner part of the mirror focuses farther from the mirror than light striking the outer part. As a result the image cannot be focused as sharply as if the aberration were not present. Because of spherical aberration, telescopes shorter than f/10 are usually made with non-spherical mirrors or with correcting lenses.
Estimation of the aberrated spot diameter
Many ways to estimate the diameter of the focused spot due to spherical aberration are based on ray optics. Ray optics, however, does not consider that light is an electromagnetic wave. Therefore, the results can be wrong due to interference effects.
A rather simple formalism based on ray optics, which holds for thin lenses only, is the Coddington notation. In the following, n is the lens' refractive index, o is the object distance, i is the image distance, h is the distance from the optical axis at which the outermost ray enters the lens, is the first lens radius, is the second lens radius, and f is the lens' focal length. The distance h can be understood as half of the clear aperture.
By using the Coddington factors for shape, s, and position, p,
one can write the longitudinal spherical aberration as 
If the focal length, f, is very much larger then the longitudinal spherical aberration, LSA, then the transverse spherical aberration, TSA, which corresponds to the diameter of the focal spot is given by
- Achromatic lens
- Aspheric lens
- Aberration in optical systems
- Cartesian oval
- Hubble Space Telescope
- Maksutov telescope
- Parabolic reflector
- Ritchey-Chrétien telescope
- Schmidt corrector plate
- Soft focus
- Smith, T. T. (1922). "Spherical Aberration in thin lenses". Scientific Papers of the Bureau of Standards. 18: 559–584.