Hamiltonian optics

From Wikipedia, the free encyclopedia
Jump to: navigation, search

Lagrangian optics[1] and Hamiltonian optics[2] are two formulations of geometrical optics which share much of the mathematical formalism with Lagrangian mechanics and Hamiltonian mechanics.

Hamilton's principle[edit]

Main article: Hamilton's principle

In physics, Hamilton's principle states that the evolution of a system \left(q_1\left(\sigma\right),\cdots,q_N\left(\sigma\right)\right) described by N generalized coordinates between two specified states at two specified parameters σA and σB is a stationary point (a point where the variation is zero), of the action functional, or

\delta S= \delta\int_{\sigma_{A}}^{\sigma_{B}} L\left(q_1,\cdots,q_N,\dot{q}_1,\cdots,\dot{q}_N,\sigma\right)\, d\sigma=0

where \dot{q}_k=dq_k/d\sigma. Condition \delta S=0 \ is valid if and only if the Euler-Lagrange equations are satisfied


\frac{\partial L}{\partial q_k} -
\frac{d}{d\sigma}\frac{\partial L}{\partial \dot q_k} = 0

with k=1,\cdots,N.

The momentum is defined as

 p_k=\frac{\partial L}{\partial \dot q_k}

and the Euler-Lagrange equations can then be rewritten as


\dot p_k = \frac{\partial L}{\partial q_k}

where \dot{p}_k=dp_k/d\sigma.

A different approach to solving this problem consists in defining a Hamiltonian (taking a Legendre transform of the Lagrangian) as

H = \sum_k {\dot q_k} p_k - L

for which a new set of differential equations can be derived by looking at how the total differential of the Lagrangian depends on parameter σ, positions q_i\, and their derivatives \dot q_i relative to σ. This derivation is the same as in Hamiltonian mechanics, only with time t now replaced by a general parameter σ. Those differential equations are the Hamilton's equations

\frac{\partial H}{\partial q_k} =- \dot{p}_k \,, \quad \frac{\partial H}{\partial p_k} = \dot{q}_k \,, \quad \frac{\partial H}{\partial \sigma} = - {\partial L \over \partial \sigma} \,.

with k=1,\cdots,N. Hamilton's equations are first-order differential equations, while Euler-Lagrange's equations are second-order.

Lagrangian and Hamiltonian optics[edit]

The general results presented above for Hamilton's principle can be applied to optics.[3][4] In 3D euclidean space the generalized coordinates are now the coordinates of euclidean space.

Fermat's principle[edit]

Main article: Fermat's principle

Fermat's principle states that the optical length of the path followed by light between two fixed points, A and B, is an extremum. It may be a maximum, a minimum, constant or an inflection point. In general, as light travels, it moves in a medium of variable refractive index which is a scalar field of position in space, that is, n=n\left(x_1,x_2,x_3\right) \ in 3D euclidean space. Assuming now that light travels along the x3 axis, the path of a light ray may be parametrized as s=\left(x_1\left(x_3\right),x_2\left(x_3\right),x_3\right) \ starting at a point \mathbf{A}=\left(x_1\left(x_{3A}\right),x_2\left(x_{3A}\right),x_{3A}\right) \ and ending at a point \mathbf{B}=\left(x_1\left(x_{3B}\right),x_2\left(x_{3B}\right),x_{3B}\right) \ . In this case, when compared to Hamilton's principle above, coordinates x_1 \ and x_2 \ take the role of the generalized coordinates q_k \ while x_3 \ takes the role of parameter \sigma \ , that is, parameter σ =x3 and N=2.

In the context of calculus of variations this can be written as[1]

\delta S= \delta\int_{\mathbf{A}}^{\mathbf{B}} n \, ds = \delta\int_{x_{3A}}^{x_{3B}} n \frac{ds}{dx_3}\, dx_3 = \delta\int_{x_{3A}}^{x_{3B}} L\left(x_1,x_2,\dot{x}_1,\dot{x}_2,x_3\right)\, dx_3=0

where ds is an infinitesimal displacement along the ray given by ds=\sqrt{dx_1^2+dx_2^2+dx_3^2} and

L=n\frac{ds}{dx_3}=n\left(x_1,x_2,x_3\right) \sqrt{1+\dot{x}_1^2+\dot{x}_2^2}

is the optical Lagrangian and \dot{x}_k=dx_k/dx_3.

The optical path length (OPL) is defined as

S= \int_{\mathbf{A}}^{\mathbf{B}} n \, ds= \int_{\mathbf{A}}^{\mathbf{B}} L \, dx_3

where n is the local refractive index as a function of position along the path between points A and B.

The Euler-Lagrange equations[edit]

The general results presented above for Hamilton's principle can be applied to optics using the Lagrangian defined in Fermat's principle. The Euler-Lagrange equations with parameter σ =x3 and N=2 applied to Fermat's principle result in


\frac{\partial L}{\partial x_k} -
\frac{d}{dx_3}\frac{\partial L}{\partial \dot x_k} = 0

with k=1,2 and where L is the optical Lagrangian and \dot{x}_k=dx_k/dx_3.

Optical momentum[edit]

The optical momentum is defined as


p_k=\frac{\partial L}{\partial \dot x_k}

and from the definition of the optical Lagrangian L=n\sqrt{1+\dot{x}_1^2+\dot{x}_2^2} this expression can be rewritten as


p_k=n\frac{\dot{x}_k}{\sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}}
=n\frac{dx_k}{\sqrt{dx_1^2+dx_2^2+dx_3^2}}
=n\frac{dx_k}{ds}
Optical momentum

or in vector form

\mathbf{p}=n\frac{\mathbf{ds}}{ds}=\left(p_1,p_2,p_3\right)
=\left(n \cos \alpha_1,n \cos \alpha_2,n \cos \alpha_3\right)=n\mathbf{\hat{e}}

where \mathbf{\hat{e}} is a unit vector and angles α1, α2 and α3 are the angles p makes to axis x1, x2 and x3 respectively, as shown in figure "optical momentum". Therefore the optical momentum is a vector of norm

\|\mathbf{p}\|=\sqrt{p_1^2+p_2^2+p_3^2}=n

where n is the refractive index at which p is calculated. Vector p points in the direction of propagation of light. If light is propagating in a gradient index optic the path of the light ray is curved and vector p is tangent to the light ray.

The expression for the optical path length can also be written as a function of the optical momentum. Having in consideration that \dot{x}_3=dx_3/dx_3=1 the expression for the optical Lagrangian can be rewritten as

L=n\sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}
=\dot{x}_1\frac{n \dot{x}_1}{\sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}}+\dot{x}_2\frac{n \dot{x}_2}{\sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}}+\frac{n \dot{x}_3}{\sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}}
=\dot{x}_1 p_1+\dot{x}_2 p_2+\dot{x}_3 p_3=\dot{x}_1 p_1+\dot{x}_2 p_2+p_3

and the expression for the optical path length is

S= \int L \, dx_3= \int \mathbf{p} \cdot d\mathbf{s}

Hamilton's equations[edit]

Similarly to what happens in Hamiltonian mechanics, also in optics the Hamiltonian is defined by the expression given above for N=2 corresponding to functions x_1\left(x_3\right) and x_2\left(x_3\right) to be determined

H = \dot{x}_1 p_1+\dot{x}_2 p_2 - L

Comparing this expression with L=\dot{x}_1 p_1+\dot{x}_2 p_2+p_3 for the Lagrangian results in

H =-p_3=-\sqrt{n^2-p_1^2-p_2^2}

And the corresponding Hamilton's equations with parameter σ =x3 and k=1,2 applied to optics are[5][6]

\frac{\partial H}{\partial x_k} =- \dot{p}_k \,, \quad \frac{\partial H}{\partial p_k} = \dot{x}_k

with \dot{x}_k=dx_k/dx_3 and \dot{p}_k=dp_k/dx_3.

Applications[edit]

It is assumed that light travels along the x3 axis, in Hamilton's principle above, coordinates x_1 \ and x_2 \ take the role of the generalized coordinates q_k \ while x_3 \ takes the role of parameter \sigma \ , that is, parameter σ =x3 and N=2.

Refraction and reflection[edit]

Main articles: Snell's law and Specular reflection

If plane x1x2 separates two media of refractive index nA below and nB above it, the refractive index is given by a step function

n(x_3) =
\begin{cases}
n_A & \mbox{if } x_3<0 \\
n_B & \mbox{if } x_3>0 \\
\end{cases}

and from Hamilton's equations

\frac{\partial H}{\partial x_k} =-\frac{\partial }{\partial x_k} \sqrt{n(x_3)^2-p_1^2-p_2^2}=0

and therefore \dot{p}_k=0 or p_k=Constant \ for k=1,2.

An incoming light ray has momentum pA before refraction (below plane x1x2) and momentum pB after refraction (above plane x1x2). The light ray makes an angle θA with axis x3 (the normal to the refractive surface) before refraction and an angle θB with axis x3 after refraction. Since the p1 and p2 components of the momentum are constant, only p3 changes from p3A to p3B.

Refraction

Figure "refraction" shows the geometry of this refraction from which d=\|\mathbf{p}_A\|sin\theta_A=\|\mathbf{p}_B\|sin\theta_B. Since \|\mathbf{p}_A\|=n_A and \|\mathbf{p}_B\|=n_B, this last expression can be written as

n_A sin\theta_A=n_B sin\theta_B \

which is Snell's law of refraction.

In figure "refraction", the normal to the refractive surface points in the direction of axis x3, and also of vector \mathbf{v}=\mathbf{p}_A-\mathbf{p}_B. A unit normal \mathbf{n}=\mathbf{v}/\|\mathbf{v}\| to the refractive surface can then be obtained from the momenta of the incoming and outgoing rays by

\mathbf{n}=\frac{\mathbf{p}_A-\mathbf{p}_B}{\|\mathbf{p}_A-\mathbf{p}_B\|}=\frac{n_A \mathbf{i}-n_B\mathbf{r}}{\|n_A\mathbf{i}-n_B\mathbf{r}\|}

where i and r are a unit vectors in the directions of the incident and refracted rays. Also, the outgoing ray (in the direction of \mathbf{p}_B) is contained in the plane defined by the incoming ray (in the direction of \mathbf{p}_A) and the normal \mathbf{n} \ to the surface.

A similar argument can be used for reflection in deriving the law of specular reflection, only now with nA=nB, resulting in θA=θB. Also, if i and r are unit vectors in the directions of the incident and refracted ray respectively, the corresponding normal to the surface is given by the same expression as for refraction, only with nA=nB

\mathbf{n} =\frac{\mathbf{i}-\mathbf{r}}{\|\mathbf{i}-\mathbf{r}\|}

In vector form, if i is a unit vector pointing in the direction of the incident ray and n is the unit normal to the surface, the direction r of the refracted ray is given by:[3]

\mathbf{r} = \frac{n_A}{n_B} \mathbf{i} + \left (- \left (\mathbf{i} \cdot \mathbf{n} \right ) \frac{n_A}{n_B}  + \sqrt{\Delta} \right ) \mathbf{n}

with

\Delta = 1- \left (\frac{n_A}{n_B} \right)^2 \left (1- \left (\mathbf{i} \cdot \mathbf{n} \right )^2\right)

If i·n<0 then -n should be used in the calculations. When \Delta <0, light suffers total internal reflection and the expression for the reflected ray is that of reflection:

\mathbf{r} = \mathbf{i} -2 \left ( \mathbf{i} \cdot \mathbf{n} \right) \mathbf{n}

Rays and wavefronts[edit]

From the definition of optical path length S= \int L\, dx_3

\frac{\partial S}{\partial x_k}= \int \frac{\partial L}{\partial x_k} \, dx_3 = \int \frac{dp_k}{dx_3} \, dx_3=p_k
Rays and wavefronts

with k=1,2 where the Euler-Lagrange equations \partial L/\partial x_k=dp_k/dx_3 with k=1,2 were used. Also, from the last of Hamilton's equations \partial H/\partial x_3=-\partial L/\partial x_3 and from H=-p_3 \ above

\frac{\partial S}{\partial x_3}= \int \frac{\partial L}{\partial x_3} \, dx_3 = \int \frac{dp_3}{dx_3} \, dx_3=p_3

combining the equations for the components of momentum p results in

\mathbf{p}=\nabla S

Since p is a vector tangent to the light rays, surfaces S=Constant must be perpendicular to those light rays. These surfaces are called wavefronts. Figure "rays and wavefronts" illustrates this relationship. Also shown is optical momentum p, tangent to a light ray and perpendicular to the wavefront.

Vector field \mathbf{p}=\nabla S is conservative vector field. The gradient theorem can then be applied to the optical path length (as given above) resulting in

S= \int_{\mathbf{A}}^{\mathbf{B}} \mathbf{p} \cdot d\mathbf{s}=\int_{\mathbf{A}}^{\mathbf{B}} \nabla S \cdot d\mathbf{s}=S(\mathbf{B})-S(\mathbf{A})

and the optical path length S calculated along a curve C between points A and B is a function of only its end points A and B and not the shape of the curve between them. In particular, if the curve is closed, it starts and ends at the same point, or A=B so that

S= \oint \nabla S \cdot d\mathbf{s}=0

This result may be applied to a closed path ABCDA as in figure "optical path length"

S= \int_{\mathbf{A}}^{\mathbf{B}} \mathbf{p} \cdot d\mathbf{s}
+\int_{\mathbf{B}}^{\mathbf{C}} \mathbf{p} \cdot d\mathbf{s}
+\int_{\mathbf{C}}^{\mathbf{D}} \mathbf{p} \cdot d\mathbf{s}
+\int_{\mathbf{D}}^{\mathbf{A}} \mathbf{p} \cdot d\mathbf{s}=0
Optical path length

for curve segment AB the optical momentum p is perpendicular to a displacement ds along curve AB, or \mathbf{p} \cdot d \mathbf{s}=0. The same is true for segment CD. For segment BC the optical momentum p has the same direction as displacement ds and \mathbf{p} \cdot d \mathbf{s}=nds. For segment DA the optical momentum p has the opposite direction to displacement ds and \mathbf{p} \cdot d \mathbf{s}=-nds. However inverting the direction of the integration so that the integral is taken from A to D, ds inverts direction and \mathbf{p} \cdot d \mathbf{s}=nds. From these considerations

\int_{\mathbf{B}}^{\mathbf{C}} nds=\int_{\mathbf{A}}^{\mathbf{D}} nds

or

S_\mathbf{BC}=S_\mathbf{AD}

and the optical path length SBC between points B and C along the ray connecting them is the same as the optical path length SAD between points A and D along the ray connecting them. The optical path length is constant between wavefronts.

Phase space[edit]

Main article: Phase space

Figure "2D phase space" shows at the top some light rays in a two-dimensional space. Here x2=0 and p2=0 so light travels on the plane x1x3 in directions of increasing x3 values. In this case p_1^2+p_3^2=n^2 and the direction of a light ray is completely specified by the p1 component of momentum \mathbf{p}=(p_1,p_3) since p2=0. If p1 is given, p3 may be calculated (given the value of the refractive index n) and therefore p1 suffices to determine the direction of the light ray. The refractive index of the medium the ray is traveling in is determined by \|\mathbf{p}\|=n.

2D phase space

For example, ray rC crosses axis x1 at coordinate xB with an optical momentum pC, which has its tip on a circle of radius n centered at position xB. Coordinate xB and the horizontal coordinate p1C of momentum pC completely define ray rC as it crosses axis x1. This ray may then be defined by a point rC=(xB,p1C) in space x1p1 as shown at the bottom of the figure. Space x1p1 is called phase space and different light rays may be represented by different points in this space.

As such, ray rD shown at the top is represented by a point rD in phase space at the bottom. All rays crossing axis x1 at coordinate xB contained between rays rC and rD are represented by a vertical line connecting points rC and rD in phase space. Accordingly, all rays crossing axis x1 at coordinate xA contained between rays rA and rB are represented by a vertical line connecting points rA and rB in phase space. In general, all rays crossing axis x1 between xL and xR are represented by a volume R in phase space. The rays at the boundary ∂R of volume R are called edge rays. For example, at position xA of axis x1, rays rA and rB are the edge rays since all other rays are contained between these two.

In three-dimensional geometry the optical momentum is given by \mathbf{p}=(p_1,p_2,p_3) with p_1^2+p_2^2+p_3^2=n^2. If p1 and p2 are given, p3 may be calculated (given the value of the refractive index n) and therefore p1 and p2 suffice to determine the direction of the light ray. A ray traveling along axis x3 is then defined by a point (x1,x2) in plane x1x2 and a direction (p1,p2). It may then be defined by a point in four-dimensional phase space x1x2p1p2.

Conservation of etendue[edit]

Main article: Etendue

Figure "volume variation" shows a volume V bound by an area A. Over time, if the boundary A moves, the volume of V may vary. In particular, an infinitesimal area dA with outward pointing unit normal n moves with a velocity v.

Volume variation

This leads to a volume variation dV = dA(\mathbf{v} \cdot \mathbf{n}) dt. Making use of Gauss's theorem, the variation in time of the total volume V volume moving in space is


\frac{dV}{dt}=\int_A \mathbf{v}\cdot\mathbf{n}dA=\int_V \nabla \cdot \mathbf{v}dV

The rightmost term is a volume integral over the volume V and the middle term is the surface integral over the boundary A of the volume V. Also, v is the velocity with which the points in V are moving.

In optics coordinate x_3 \ takes the role of time. In phase space a light ray is identified by a point (x_1, x_2, p_1, p_2) \ which moves with a "velocity" \mathbf{v}=(\dot{x}_1, \dot{x}_2, \dot{p}_1, \dot{p}_2) \ where the dot represents a derivative relative to x_3 \ . A set of light rays spreading over dx_1 \ in coordinate x_1 \ , dx_2 \ in coordinate x_2 \ , dp_1 \ in coordinate p_1 \ and dp_2 \ in coordinate p_2 \ occupies a volume dV=dx_1dx_2dp_1dp_2 \ in phase space. In general, a large set of rays occupies a large volume V \ in phase space to which Gauss's theorem may be applied


\frac{dV}{dx_3}=\int_V \nabla \cdot \mathbf{v}dV

and using Hamilton's equations


\nabla \cdot \mathbf{v}=
\frac{\partial \dot{x}_1}{\partial x_1}
+\frac{\partial \dot{x}_2}{\partial x_2}
+\frac{\partial \dot{p}_1}{\partial p_1}
+\frac{\partial \dot{p}_2}{\partial p_2}
=\frac{\partial }{\partial x_1}\frac{\partial H}{\partial p_1}
+\frac{\partial }{\partial x_2}\frac{\partial H}{\partial p_2}
-\frac{\partial }{\partial p_1}\frac{\partial H}{\partial x_1}
-\frac{\partial }{\partial p_2}\frac{\partial H}{\partial x_2}
=0

or dV/dx_3=0 \ and dV=dx_1dx_2dp_1dp_2=Constant \ which means that the phase space volume is conserved as light travels along an optical system.

The volume occupied by a set of rays in phase space is called etendue, which is conserved as light rays progress in the optical system along direction x3. This corresponds to Liouville's theorem, which also applies to Hamiltonian mechanics.

However, the meaning of Liouville’s theorem in mechanics is rather different from the theorem of conservation of étendue. Liouville’s theorem is essentially statistical in nature, and it refers to the evolution in time of an ensemble of mechanical systems of identical properties but with different initial conditions. Each system is represented by a single point in phase space, and the theorem states that the average density of points in phase space is constant in time. An example would be the molecules of a perfect classical gas in equilibrium in a container. Each point in phase space, which in this example has 2N dimensions, where N is the number of molecules, represents one of an ensemble of identical containers, an ensemble large enough to permit taking a statistical average of the density of representative points. Liouville’s theorem states that if all the containers remain in equilibrium, the average density of points remains constant.[4]

Imaging and nonimaging optics[edit]

Main article: Nonimaging optics

Figure "conservation of etendue" shows on the left a diagrammatic two-dimensional optical system in which x2=0 and p2=0 so light travels on the plane x1x3 in directions of increasing x3 values.

Conservation of etendue

Light rays crossing the input aperture of the optic at point x1=xI are contained between edge rays rA and rB represented by a vertical line between points rA and rB at the phase space of the input aperture (right, bottom corner of the figure). All rays crossing the input aperture are represented in phase space by a region RI.

Also, light rays crossing the output aperture of the optic at point x1=xO are contained between edge rays rA and rB represented by a vertical line between points rA and rB at the phase space of the output aperture (right, top corner of the figure). All rays crossing the output aperture are represented in phase space by a region RO.

Conservation of etendue in the optical system means that the volume (or area in this two-dimensional case) in phase space occupied by RI at the input aperture must be the same as the volume in phase space occupied by RO at the output aperture.

In imaging optics, all light rays crossing the input aperture at x1=xI are redirected by it towards the output aperture at x1=xO where xI=m xO. This ensures that an image of the input of formed at the output with a magnification m. In phase space, this means that vertical lines in the phase space at the input are transformed into vertical lines at the output. That would be the case of vertical line rA rB in RI transformed to vertical line rA rB in RO.

In nonimaging optics, the goal is not to form an image but simply to transfer all light from the input aperture to the output aperture. This is accomplished by transforming the edge rays ∂RI of RI to edge rays ∂RO of RO. This is known as the edge ray principle.

Generalizations[edit]

Above it was assumed that light travels along the x3 axis, in Hamilton's principle above, coordinates x_1 \ and x_2 \ take the role of the generalized coordinates q_k \ while x_3 \ takes the role of parameter \sigma \ , that is, parameter σ =x3 and N=2. However, different parametrizations of the light rays are possible, as well as the use of generalized coordinates.

General ray parametrization[edit]

A more general situation can be considered in which the path of a light ray is parametrized as s=\left(x_1\left(\sigma\right),x_2\left(\sigma\right),x_3\left(\sigma\right)\right) \ in which σ is a general parameter. In this case, when compared to Hamilton's principle above, coordinates x_1 \ , x_2 \ and x_3 \ take the role of the generalized coordinates q_k \ with N=3. Applying Hamilton's principle to optics in this case leads to

\delta S= \delta\int_{\mathbf{A}}^{\mathbf{B}} n \, ds = \delta\int_{\sigma_A}^{\sigma_B} n \frac{ds}{d\sigma}\, d\sigma
= \delta\int_{\sigma_A}^{\sigma_B} L\left(x_1,x_2,x_3,\dot{x}_1,\dot{x}_2,\dot{x}_3,\sigma\right)\, d\sigma=0

where now L=nds/d\sigma \ and \dot{x}_k=dx_k/d\sigma and for which the Euler-Lagrange equations applied to this form of Fermat's principle result in


\frac{\partial L}{\partial x_k} -
\frac{d}{d\sigma}\frac{\partial L}{\partial \dot x_k} = 0

with k=1,2,3 and where L is the optical Lagrangian. Also in this case the optical momentum is defined as

 p_k=\frac{\partial L}{\partial \dot x_k}

and the Hamiltonian P is defined by the expression given above for N=3 corresponding to functions x_1\left(\sigma\right), x_2\left(\sigma\right) and x_3\left(\sigma\right) to be determined

P = \dot{x}_1 p_1+\dot{x}_2 p_2+\dot{x}_3 p_3 - L

And the corresponding Hamilton's equations with k=1,2,3 applied optics are

\frac{\partial H}{\partial x_k} =- \dot{p}_k \,, \quad \frac{\partial H}{\partial p_k} = \dot{x}_k

with \dot{x}_k=dx_k/d\sigma and \dot{p}_k=dp_k/d\sigma.

The optical Lagrangian is given by

L=n\frac{ds}{d\sigma}=n\left(x_1,x_2,x_3\right) \sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}=L\left(x_1,x_2,x_3,\dot{x}_1,\dot{x}_2,\dot{x}_3\right)

and does not explicitly depend on parameter σ. For that reason not all solutions of the Euler-Lagrange equations will be possible light rays, since their derivation assumed an explicit dependence of L on σ which does not happen in optics.

The optical momentum components can be obtained from


p_k=n\frac{\dot{x}_k}{\sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}}
=n\frac{dx_k}{\sqrt{dx_1^2+dx_2^2+dx_3^2}}
=n\frac{dx_k}{ds}

where \dot{x}_k=dx_k/d\sigma. The expression for the Lagrangian can be rewritten as

L=n\sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}
=\dot{x}_1\frac{n \dot{x}_1}{\sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}}+\dot{x}_2\frac{n \dot{x}_2}{\sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}}+\dot{x}_3\frac{n \dot{x}_3}{\sqrt{\dot{x}_1^2+\dot{x}_2^2+\dot{x}_3^2}}
=\dot{x}_1 p_1+\dot{x}_2 p_2+\dot{x}_3 p_3

Comparing this expression for L with that for the Hamiltonian P it can be concluded that

P=0 \

From the expressions for the components p_k \ of the optical momentum results

p_1^2+p_2^2+p_3^2-n^2\left(x_1,x_2,x_3\right)=0

The optical Hamiltonian is chosen as

P=p_1^2+p_2^2+p_3^2-n^2\left(x_1,x_2,x_3\right)=0

although other choices could be made.[3][4] The Hamilton's equations with k=1,2,3 defined above together with P=0 \ define the possible light rays.

Generalized coordinates[edit]

As in Hamiltonian mechanics, it is also possible to write the equations of Hamiltonian optics in terms of generalized coordinates \left(q_1\left(\sigma\right),q_2\left(\sigma\right),q_3\left(\sigma\right)\right) \ , generalized momenta \left(u_1\left(\sigma\right),u_2\left(\sigma\right),u_3\left(\sigma\right)\right) \ and Hamiltonian P as[3][4]

\frac{dq_1}{d\sigma} =\frac{\partial P}{\partial u_1} \quad \quad \frac{du_1}{d\sigma} =-\frac{\partial P}{\partial q_1}
\frac{dq_2}{d\sigma} =\frac{\partial P}{\partial u_2} \quad \quad \frac{du_2}{d\sigma} =-\frac{\partial P}{\partial q_2}
\frac{dq_3}{d\sigma} =\frac{\partial P}{\partial u_3} \quad \quad \frac{du_3}{d\sigma} =-\frac{\partial P}{\partial q_3}
P=\mathbf{p}\cdot\mathbf{p}-n^2=0

where the optical momentum is given by

\mathbf{p}=u_1 \nabla q_1+u_2 \nabla q_2+u_3 \nabla q_3
=u_1 \|\nabla q_1 \| \frac{\nabla q_1}{\|\nabla q_1 \|}
+u_2 \|\nabla q_2 \| \frac{\nabla q_2}{\|\nabla q_2 \|}
+u_3 \|\nabla q_3 \| \frac{\nabla q_3}{\|\nabla q_3 \|}
=u_1 a_1 \mathbf{\hat{e}}_1
+u_2 a_2 \mathbf{\hat{e}}_2
+u_3 a_3 \mathbf{\hat{e}}_3

and \mathbf{\hat{e}}_1, \mathbf{\hat{e}}_2 and \mathbf{\hat{e}}_3 are unit vectors. A particular case is obtained when these vectors form an orthonormal basis, that is, they are all perpendicular to each other. In that case, u_k a_k/n \ is the cosine of the angle the optical momentum \mathbf{p} makes to unit vector \mathbf{\hat{e}}_k.

See also[edit]

Learning materials related to a simple one-dimensional derivation of Hamiltonian optics at Wikiversity

References[edit]

  1. ^ a b Vasudevan Lakshminarayanan et al., Lagrangian Optics, Springer Netherlands, 2011 [ISBN 978-0792375821]
  2. ^ H. A. Buchdahl, An Introduction to Hamiltonian Optics, Dover Publications, 1993 [ISBN 978-0486675978]
  3. ^ a b c d Julio Chaves, Introduction to Nonimaging Optics, CRC Press, 2008 [ISBN 978-1420054293]
  4. ^ a b c d Roland Winston et al., Nonimaging Optics, Academic Press, 2004 [ISBN 978-0127597515]
  5. ^ Dietrich Marcuse, Light Transmission Optics, Van Nostrand Reinhold Company, New York, 1972 [ISBN 978-0894643057]
  6. ^ Rudolf Karl Luneburg,Mathematical Theory of Optics, University of California Press, Berkeley, CA, 1964, p. 90.