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Spherical aberration
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The bottom example depicts a real lens with spherical surfaces, which produces spherical aberration: The different rays do not meet after the lens in one focal point. The further the rays are from the optical axis, the closer to the lens they intersect the optical axis (positive spherical aberration).
(Drawing is exaggerated.)
In optics, spherical aberration (SA) is a type of aberration found in optical systems that have elements with spherical surfaces. This phenomenon commonly affects lenses and curved mirrors, as these components are often shaped in a spherical manner for ease of manufacturing. Light rays that strike a spherical surface off-centre are refracted or reflected more or less than those that strike close to the centre. This deviation reduces the quality of images produced by optical systems. The effect of spherical aberration was first identified in the 11th century by Ibn al-Haytham who discussed it in his work Kitāb al-Manāẓir.[1]
Overview
[edit]A spherical lens has an aplanatic point (i.e., no spherical aberration) only at a lateral distance from the optical axis that equals the radius of the spherical surface divided by the index of refraction of the lens material.
Spherical aberration makes the focus of telescopes and other instruments less than ideal. 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 rays near the outer edge of a lens are bent more than would be predicted for an ideal lens. "Negative" spherical aberration means such rays are bent less than would be predicted.
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.
Correction
[edit]In lens systems, aberrations can be minimized using combinations of convex and concave lenses, or by using aspheric lenses or aplanatic lenses.
Lens systems with aberration correction are usually designed by numerical ray tracing. For simple designs, one can sometimes analytically 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 R1 and R2 of the front and back surfaces of the lens such that where the signs in this formula follow the Cartesian sign convention, in which a radius of curvature is positive if the center of curvature is to the right of the surface and negative if it is to the left. Similarly the object and image distances are positive if the object or image is to the right of the lens and negative if they are to the left.
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 with focal ratio less than f/10 are usually made with non-spherical mirrors or with correcting lenses.
Spherical aberration can be eliminated by making lenses with an aspheric surface. Descartes showed that lenses whose surfaces are well-chosen Cartesian ovals (revolved around the central symmetry axis) can perfectly image light from a point on the axis or from infinity in the direction of the axis. Such a design yields completely aberration-free focusing of light from a distant source.[2]
In 2018, researchers found a closed formula for a lens surface that eliminates spherical aberration.[3][4][5] Their equation can be applied to specify a shape for one surface of a lens, where the other surface has any given shape.
Estimation of the aberrated spot diameter
[edit]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 arisen from the wave nature of light.
Coddington notation
[edit]A rather simple formalism based on ray optics, which holds for thin lenses only, is the Coddington notation.[6] In the following, n is the lens's 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, R1 is the first lens radius, R2 is the second lens radius, and f is the lens's 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 [6]
![{\displaystyle {\begin{aligned}s&={\frac {R_{2}+R_{1}}{R_{2}-R_{1}}}\\[8pt]p&={\frac {i-o}{i+o}},\end{aligned}}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/153e0891f9c02c41916455af75e53445456ccee3)
If the focal length f is very much larger than the longitudinal spherical aberration LSA, then the transverse spherical aberration, TSA, which corresponds to the diameter of the focal spot, is given by
See also
[edit]References
[edit]- ^ Boudrioua, Azzedine; Rashed, Roshdi; Lakshminarayanan, Vasudevan (2017-08-15). Light-Based Science: Technology and Sustainable Development, The Legacy of Ibn al-Haytham. CRC Press. ISBN 978-1-351-65112-7.
- ^ Villarino, Mark B (2007). "Descartes' perfect lens". arXiv:0704.1059 [math.GM].
- ^ Machuca, Eduardo (July 5, 2019). "Goodbye Aberration: Physicist Solves 2,000-Year-Old Optical Problem". PetaPixel. Retrieved July 10, 2019.
- ^ González-Acuña, Rafael G.; Chaparro-Romo, Héctor A. (2018). "General formula for bi-aspheric singlet lens design free of spherical aberration". Applied Optics. 57 (31): 9341–9345. arXiv:1811.03792. Bibcode:2018ApOpt..57.9341G. doi:10.1364/AO.57.009341. PMID 30461981. S2CID 53695913.
- ^ Liszewski, Andrew (August 7, 2019). "A Mexican Physicist Solved a 2,000-Year Old Problem That Will Lead to Cheaper, Sharper Lenses". Gizmodo. Retrieved August 7, 2019.
- ^ a b Smith, T. T. (1922). "Spherical Aberration in thin lenses". Scientific Papers of the Bureau of Standards. 18: 559–584. doi:10.6028/nbsscipaper.127.
External links
[edit]- Spherical aberration Archived 2012-07-23 at the Wayback Machine at vanwalree.com, PA van Walree, viewed 28 January 2007.
- http://www.telescope-optics.net/spherical1.htm
- Non-English articles on the Acuña-Romo equation: Spanish, German, Italian, Russian
Spherical aberration
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Fundamentals
Definition
Spherical aberration is an optical imperfection that arises in lenses and mirrors with spherical surfaces, where light rays passing through different zones of the optic fail to converge at a single focal point. In the paraxial approximation, which assumes rays are close to the optical axis and uses small-angle simplifications for ray tracing, all rays are idealized to focus precisely at the paraxial focal point; however, real rays farther from the axis deviate due to the geometry of the spherical surface. This aberration is classified as positive when peripheral (marginal) rays focus closer to the optic than paraxial rays, as typically seen in convex lenses, or negative when peripheral rays focus farther away, as in concave lenses.[4][5] The primary impact of spherical aberration is the degradation of image quality, producing blurred spots instead of sharp points, with the unfocused light forming a "disk of confusion" or circle of least confusion in the image plane. This spreading reduces resolution and contrast in imaging systems, such as telescopes and microscopes, particularly noticeable with larger apertures where more peripheral rays contribute. The effect is symmetric about the optical axis and affects on-axis points most directly, limiting the overall performance of uncorrected spherical optics.[4] Spherical aberration was discussed by Isaac Newton in his 1704 work Opticks, where he distinguished it from chromatic effects and noted its relatively minor role in imperfect focusing compared to chromatic aberration.[6]Physical Causes
Spherical aberration arises primarily from the geometry of spherical optical surfaces in lenses and mirrors, where rays incident at different distances from the optical axis experience varying degrees of deviation during refraction or reflection. According to Snell's law, which governs refraction at the interface between media (n sin θ_i = n' sin θ_r), marginal rays—those striking the surface far from the axis—encounter steeper angles of incidence compared to paraxial rays near the axis. This results in greater bending of the marginal rays, causing them to converge at a focal point closer to the surface in converging systems, such as a plano-convex lens with the curved surface facing the incident light.[4] In mirrors, a similar effect occurs during reflection, where the law of reflection (angle of incidence equals angle of reflection) leads to marginal rays in a concave spherical mirror focusing closer to the mirror vertex than paraxial rays.[3] The paraxial approximation underpins ideal thin-lens theory by assuming small angles of incidence, where sin θ ≈ θ in radians, allowing linear simplification of ray paths and a single focal length for all rays. However, in real optical systems with finite apertures, non-paraxial rays violate this approximation because the actual sine function deviates from the linear term, especially at larger angles. This discrepancy causes the effective focal length to shorten for marginal rays in positive (converging) lenses and mirrors, as the increased curvature deviation at the periphery amplifies the ray bending beyond paraxial predictions. For diverging systems, the effect reverses, with marginal rays exhibiting a longer focal length, though the magnitude is typically smaller.[7][8] Spherical aberration is classified as positive when the marginal focus lies closer to the optic than the paraxial focus, which is the typical case for uncorrected converging lenses and concave mirrors, leading to a distribution of focal points along the axis. Conversely, negative aberration occurs when the marginal focus is farther away, as seen in some diverging lenses or overcorrected systems. This behavior stems from the spherical surface's uniform radius of curvature, which provides only an approximation to the ideal aspheric profile required for all rays to converge precisely at one point; the spherical shape introduces higher-order deviations that increase with aperture size. For instance, in a converging lens, paraxial rays parallel to the axis focus at the nominal focal length f, while marginal rays at height h focus at approximately f - Δf, where Δf grows with h due to the nonlinear response in ray deviation.[4][3]Manifestations
In Lenses
In refractive optical systems, spherical aberration arises because parallel light rays passing through different annular zones of a spherical lens surface experience unequal deviations due to varying angles of incidence, leading to distinct focal points along the optical axis. This results from the inherent mismatch between the spherical surface geometry and the ideal conic shape required for perfect focusing, causing peripheral rays to converge closer to the lens than paraxial rays. The effect is exacerbated by differences in optical path lengths through the glass, as marginal rays traverse steeper paths with greater refraction.[9][10] The severity of spherical aberration in lenses increases markedly with aperture diameter, as wider apertures admit more oblique rays that amplify the focal shift. Lenses operating at faster f-numbers (lower f/# values) suffer greater blur, since the relative aperture height scales the aberration roughly with the fourth power of the pupil radius. Reducing the aperture by stopping down mitigates this by limiting ray angles but diminishes light throughput and can introduce diffraction limits at extreme closures.[9][10] Material properties significantly influence aberration magnitude; higher refractive index glasses reduce spherical aberration for a given lens power and shape, as they require less curvature to achieve the same focal length, thereby minimizing ray bending deviations. Crown glass (n ≈ 1.52, e.g., BK7) thus exhibits more pronounced spherical aberration than flint glass (n ≈ 1.62–1.90, e.g., F2), which benefits from its elevated index to yield tighter focus across the aperture in simple refractive designs.[10] This aberration is particularly evident in simple convex lenses, such as those in magnifying glasses, where it produces characteristic halo effects around bright point sources, with outer rays forming a diffuse ring beyond the central focus. In photography, spherical aberration causes blur in images from large-aperture objectives, reducing overall acuity for portraits or landscapes under bright conditions. Microscopy applications suffer from lowered contrast and hazy rendering of specimen details, as the uneven focus spreads intensity asymmetrically, impairing resolution in high-magnification views.[11][9][12]In Mirrors
Spherical aberration in mirrors arises from the geometry of spherical reflective surfaces, where rays striking the mirror farther from the optical axis (marginal rays) focus at a point closer to the mirror than those near the axis (paraxial rays), resulting in a blurred image rather than a single focal point.[5] This effect is particularly evident in concave spherical mirrors used in optical systems, as the spherical shape deviates from the ideal parabolic form that would converge parallel rays to a precise focus on-axis.[13] In reflective systems, the aberration is independent of wavelength, allowing mirrors to avoid the chromatic issues common in refractive optics, though it becomes prominent in designs with large apertures or short focal ratios.[14] In astronomical telescopes, such as early Newtonian reflectors, spherical mirrors were initially favored for their ease of fabrication, but the aberration significantly degrades image quality for large apertures, where marginal rays contribute substantially to the light gathering.[15] For instance, the Hubble Space Telescope's primary mirror, launched in 1990, suffered from severe spherical aberration due to a manufacturing error that deviated from the intended parabolic shape by about 2 micrometers, producing blurry images with multiple focal points and reducing resolution to one-seventh of its design capability.[16] This flaw was corrected in 1993 during Servicing Mission 1 by installing the Corrective Optics Space Telescope Axial Replacement (COSTAR), which added corrective mirrors to restore sharp focus for several instruments. COSTAR was removed in 2009 during Servicing Mission 4, after newer instruments with built-in corrective optics were installed, allowing Hubble to continue high-resolution observations without it.[17][18] Beyond astronomy, spherical aberration manifests in everyday applications like automotive headlight reflectors, where spherical designs lead to uneven illumination and a less concentrated beam, as marginal rays do not align perfectly with paraxial ones, spreading light inefficiently on the road.[5] Parabolic reflectors are preferred in modern headlights to eliminate this on-axis aberration and produce a more uniform, directed beam.[5] The aberration is primarily an on-axis phenomenon in spherical mirrors, affecting central field points most severely, whereas off-axis performance introduces additional aberrations like coma, limiting the usable field of view in wide-angle systems.[19] While reflectors inherently sidestep chromatic aberration—beneficial for broadband light sources such as starlight or white LEDs—they require aspheric shaping or corrective elements to mitigate spherical issues, especially at wide fields where the deviation from paraxial approximation worsens.[13]Correction Methods
Aspheric Surfaces
Aspheric surfaces represent a fundamental approach to correcting spherical aberration by deviating from the traditional spherical curvature of lenses and mirrors, allowing parallel rays to converge at a single focal point without the peripheral blurring characteristic of spherical optics.[20] These surfaces often employ conic sections, such as paraboloids, which inherently eliminate spherical aberration for on-axis rays in reflective systems like telescopes.[21] By adjusting the curvature profile, aspheres minimize the path length differences that cause spherical aberration, enabling sharper imaging across a wider aperture.[22] The design of aspheric surfaces is mathematically described by the sagitta equation, which extends the spherical profile to include higher-order corrections:
where $ z $ is the sag (axial distance from the vertex), $ r $ is the radial distance from the optical axis, $ R $ is the radius of curvature at the vertex, and the coefficients $ A_4, A_6, \ldots $ represent aspheric deviations that fine-tune the focus.[22] This formulation allows optical designers to optimize the surface for specific wavelengths and field angles, ensuring reduced aberration while maintaining manufacturability.[21]
In practical applications, aspheric lenses are integral to modern camera systems, particularly in compact smartphone optics where space constraints demand high performance from fewer elements.[20] They also enhance laser focusing by concentrating beams into tighter spots with minimal distortion, supporting applications in precision cutting and medical devices.[23] Manufacturing aspheres typically involves single-point diamond turning (SPDT) for prototypes and high-precision optics, which uses a diamond tool to machine the surface directly from a rotating blank.[24] For volume production, precision glass molding compresses heated glass against a mold under controlled conditions, enabling cost-effective replication of complex profiles.
Despite their advantages, aspheric surfaces introduce trade-offs in fabrication, as their non-uniform curvature demands advanced tooling and metrology, increasing costs compared to spherical elements.[25] This complexity can limit scalability for very large optics, though it ultimately enables more compact and efficient systems by reducing the need for multiple corrective elements.[26]
Compound Optics
Compound optics refers to the use of multiple spherical lens elements in combination to balance and minimize spherical aberration, achieving better performance than single-element designs without resorting to aspheric surfaces. A foundational approach is the achromatic doublet, which pairs a convex crown glass element with a concave flint glass element to primarily correct chromatic aberration while also reducing spherical aberration through the differential dispersion and refractive indices of the glasses. This configuration, first developed by Chester Moore Hall in 1729, allows marginal rays to converge more closely with paraxial rays, limiting the spread of the focal point.[27] In multi-element systems, lens bending—altering the curvatures of individual elements—and spacing between them play key roles in adjusting the paths of marginal rays to counteract spherical aberration. These techniques modify the incidence angles and path lengths for off-axis rays, distributing the aberration burden across elements rather than concentrating it in one. The Petzval sum, while primarily governing field curvature as the sum of powers divided by refractive indices (∑ φ/n), remains distinct but influences overall design; a positive Petzval sum in compound optics can be managed alongside spherical correction by strategic bending and spacing to maintain a flatter field without exacerbating marginal ray deviations.[28][29] Notable examples include the Cooke triplet, patented in 1893 by H. Dennis Taylor for photographic applications, which employs three cemented spherical elements—a biconvex crown, a biconcave flint, and another biconvex crown—to correct spherical aberration, coma, astigmatism, and other Seidel aberrations over a moderate field of view. For microscopy, apochromatic objectives use multiple fluorite or low-dispersion elements to minimize residual spherical aberration after chromatic correction for three wavelengths, enabling high-resolution imaging with reduced blur at high magnifications.[30] Optimization in compound optics often leverages symmetric configurations to evenly distribute spherical aberration among elements, minimizing its net effect. The Tessar design, introduced by Paul Rudolph in 1902, exemplifies this with four spherical elements in three groups arranged symmetrically around the aperture stop, balancing spherical aberration and other off-axis errors for compact, cost-effective photographic lenses. Such symmetry reduces the sensitivity of marginal rays to individual element contributions, allowing residual aberrations to cancel out through careful glass selection and air spacing.[31]Mathematical Description
Wavefront Aberration
In optical systems, the ideal wavefront emanating from a point source and converging to a focus is spherical, but spherical aberration deforms this wavefront into a rotationally symmetric shape, introducing optical path differences (OPD) that degrade image quality.[32] This deformation is classified as the primary Seidel aberration, characterized by its rotational symmetry around the optical axis and independence from off-axis field position, making it prominent for on-axis imaging in monochromatic light.[32] The wavefront aberration for primary spherical aberration is mathematically represented using Zernike polynomials, specifically the term $ Z_4^0 $, which captures the defocus-like quartic deviation. The aberration function takes the form
where $ \rho $ is the normalized radial pupil coordinate (ranging from 0 at the center to 1 at the edge), and $ A $ is the coefficient determining the aberration strength, typically expressed in waves of optical path difference.[32] This polynomial expansion provides an orthogonal basis for decomposing complex wavefront errors, with the $ \rho^4 $ term isolating the symmetric spherical contribution.[32]
Wavefront errors due to spherical aberration are quantified through interferometric techniques, such as the Twyman-Green interferometer, which compares the aberrated wavefront against a reference spherical wavefront to produce interference fringes revealing the OPD in units of wavelengths ($ \lambda $).[32] For diffraction-limited performance, the peak-to-valley wavefront error must not exceed $ \lambda/4 $, as established by the Rayleigh criterion, ensuring minimal impact on the point spread function.[33]
From a ray optics perspective, the local tilt of the deformed wavefront directly corresponds to the angular deviation of rays, with the $ \rho^4 $ term producing marginal rays that focus closer to the lens than paraxial rays in positive spherical aberration for monochromatic illumination.[32] This wavefront-ray linkage bridges wave and geometric optics descriptions of the primary aberration.[32]
Spot Size Estimation
A foundational geometric optics derivation of the third-order longitudinal spherical aberration is provided by considering a single convex refracting surface separating air from glass ($ n > 1 $), for parallel incident rays at height $ h $ on a spherical surface of radius $ R > 0 $.[32]- Geometry: The incidence angle $ i = \alpha = \arcsin(h/R) $; the sagitta $ z_\mathrm{inc} = R(1 - \cos \alpha) $; the refracted angle $ r = \arcsin(\sin i / n) $; the refracted ray angle to the axis $ u' = i - r $.
- Axial intersection: The total distance from the vertex $ f(h) = z_\mathrm{inc} + h / \tan u' $.
- Paraxial limit (small $ h/R $): $ i \approx h/R $, $ r \approx (h/R)/n $, $ u' \approx h(n-1)/(n R) $, $ f = n R / (n-1) $.
- Third-order expansion (series in $ k = h/R $ using $ \arcsin x \approx x + x^3/6 $, $ \tan x \approx x + x^3/3 $): $ \Delta f = f(h) - f = -h^2 / (2 n (n-1) R) $ or equivalently $ -h^2 / (2 (n-1)^2 f) $; marginal rays focus closer to the surface (negative $ \Delta f $ for positive power); for $ n=1.5 $, $ \Delta f \approx - (2/3) h^2 / R $.[32]
Coddington Factors
The Coddington factors provide a framework for analyzing spherical aberration in thin lenses by parameterizing the lens geometry and object-image configuration. These factors, introduced in the early 19th century, express the aberration as a quadratic function of the aperture height, enabling systematic design to minimize blur. They are particularly useful for single-element lenses, where aberration scales with the cube of the semi-aperture and inversely with the cube of the focal length.[34] The Coddington position factor $ p $ accounts for the object and image distances, defined as $ p = \frac{s' - s}{s' + s} $, where $ s $ is the object distance (negative in the standard sign convention) and $ s' $ is the image distance (positive). For distant objects, $ p \approx -1 $; for objects at the focal point, $ p = 1 $. The Coddington shape factor $ q $ describes the lens curvature, given by $ q = \frac{r_2 - r_1}{r_2 + r_1} $, where $ r_1 $ and $ r_2 $ are the radii of curvature of the first and second surfaces, respectively (positive if the center lies to the right of the surface). An equiconvex lens has $ q = 0 $; a plano-convex lens oriented with the curved surface toward the object has $ q = 1 $. These factors relate to the lensmaker's formula via $ \frac{1}{f} = (n-1) \left( \frac{1}{r_1} - \frac{1}{r_2} \right) $, allowing $ r_1 $ and $ r_2 $ to be expressed in terms of $ f $, $ n $, and $ q $.[37][38] Spherical aberration is quantified using these factors through the longitudinal aberration $ L_s $, the axial shift in focus for marginal rays:
where $ h $ is the semi-aperture height and $ n $ is the refractive index. The transverse aberration, representing lateral blur, follows as $ \Delta y \approx L_s \cdot \frac{h}{f} $. This expression shows aberration as a quadratic form in $ p $ and $ q $, with coefficients depending on $ n n \approx 1.52 $), the shape term dominates for symmetric lenses.[37][38]
To minimize spherical aberration, the shape factor is optimized for a given position factor: $ q_{\text{opt}} = -\frac{2(n^2 - 1)p}{n + 2} $. This bent shape (e.g., meniscus for finite conjugates) reduces aberration by up to a factor of 4 compared to equiconvex forms, though it increases sensitivity to manufacturing errors. For $ p = -1 $ (collimated input), the optimal lens is plano-convex with the curved surface facing the light, minimizing marginal ray deviation. These optimizations guide preliminary lens design before full ray tracing.[37][34]