## Abstract

Since the discovery of backward-wave materials, people have tried to realize a strong chiral medium, which is traditionally thought impossible mainly for the reason of energy and spatial dispersion. We compare the two most popular descriptions of a chiral medium. After analyzing several possible reasons for the traditional restriction, we show that a strong chirality parameter leads to positive energy without any frequency-band limitation in the weak spatial dispersion. Moreover, strong chirality does not result in a strong spatial dispersion, which occurs only around the traditional limit point. For strong spatial dispersion where higher-order terms of spatial dispersion need to be considered, the energy conservation is also valid. Finally, we show that realization of strong chirality requires the conjugated type of spatial dispersion.

© 2007 Optical Society of America

## 1. Introduction

Chirality is first referred to a kind of asymmetry in geometry and group theory in mathematics. The asymmetry exists broadly in organic molecules, crystal lattices, and liquid crystals, leading to two stereoisomers, dextrorotatory and laevorotatory, as a hot research domain in stereochemistry. If the two stereoisomers coexist in one molecule (mesomer), or equally different steroisomers get mixed (raceme), there will be no special characteristics other than the common magneto-dielectric. When we get one pure steroisomer, however, interesting phenomena occur with an incident linearly-polarized wave, which can be seen as a superposition of two dual circularly-polarized waves. In the case of perpendicular incidence, the two different circularly polarized waves have different phase velocities and their polarized planes rotate oppositely. As a result, the output polarization direction gets rotated, also known as optical activity or natural optical rotation phenomenon, which was first observed by Arago in 1811. For oblique incidence, the two different polarized waves will split even when the medium is isotropic, which was verified by Fresnel using prism series made from dextrorotatory and laevorotatory quartz [1, 2, 3, 4]. Moreover, in elementary particle physics, chirality and asymmetry also play important roles, but they are beyond the scope of this paper.

## 2. Two major electromagnetic models to describe a chiral medium

The electromagnetic theoretical explanation of optical activity is spatial dispersion [5, 6, 7, 8]. Usually, under the weak spatial dispersion, we use the first order (linear) approximation, which is written as

Such a representation is named as Drude-Born-Fedorov (DBF) relation for a natural
result of linearly spatial dispersion. Rotation terms are added to the basic
constitutive relation, standing for the spatial dispersion, whose coefficients
*ε _{DBF}β* or

*μ*can be either positive or negative for two stereoisomer structures. And in this paper, we assume our chiral medium is source free, i.e. no electric or magnetic sources inside the medium. Solving the constitutive relation together with Maxwell’s equations, we can easily get two eigenwaves, which are left and right circularly polarized with different wavevectors.

_{DBF}βThere are also some other representations, including Cotton model, Tellegen-Pasteur model, Boys-Post model, etc. It is shown that these three models are mathematical isomorphic [9]. Among them the most common one is deduced by Pasteur and Tellegen as

in which electromagnetic coupling terms are added to the basic terms. Bi-isotropy or
bi-anisotropy is used to describe such constitutive equations, according to whether
the parameters are scalars or tensors. If *κ*= 0 and
*χ*≠ 0, it is the Tellegen medium; if
*χ*= 0 and *κ*≠
0, as the requirement of reciprocity, it is the Pasteur medium:

We pay more attention to such a chiral medium. Positive and negative
*κ* values differentiate two conjugated stereoisomer
structures. We assume *κ* > 0 in the following
analysis.

Actually, the constitutive relations above are essentially equivalent, with corresponding parameters to be [7]

It is clear that the parameters are different in such two representations. Then a
question may arise: which are the “true” material permittivity
and permeability? The answer is, both. The concepts of permittivity and permeability
are effective coefficients derived from a mathematical model. We actually have
different mathematical models describing the same physical material. Thus there are
different effective parameters describing the proportion of
*D*¯ to *E*¯ and
*B*¯ to *H*¯. The rotation terms
in DBF model include both real and imaginary parts, resulting in a change in the
real part and creating the imaginary chiral terms in the Pasteur model, vice versa.
In other words, the difference in representations of coupling terms lead to
different permittivity and permeability formulations.

It should be noticed that a Faraday gyratory medium can also lead to optical rotation within a plasma or ferrite under an additional DC magnetic field [10, 11]. Hence it is not natural, and is usually referred as “gyratory”, “Faraday optical rotation”, “magneto-optical effect”, etc. However, sometimes people do not differentiate “chiral” and “gyratory”. We need to pay attention to the fact that these two types of optical rotation have different essence and different characteristics [11]. Only natural optical activity is discussed here.

## 3. Energy and spatial dispersion in strong chiral medium

There is a long dispute on a strong chiral medium since it was introduced
theoretically [12]. Traditional electromagnetic conclusions lead to the
limitation that strong chirality, i.e. *κ*
^{2}
> *με* [7, 12] cannot exist (in other words, chirality should be weak,
i.e. *κ*
^{2} <
*με*), until we see the fact that
artificial Veselago’s medium [13] was successfully realized in certain frequency bands [14]. Hence, we have to ask the following question: can a strong
chiral medium exist?

In Ref. [[8, 12]], the reasons for the traditional restriction on chirality parameters were: 1) The wavevector of one eigenwave will be negative; 2) The requirement of a positive definite matrix to keep positive energy:

With the exploration of backward-wave medium, we know that a negative wavevector, or opposite phase and group velocities, are actually realizable. And there is an unfortunate mathematical error in the second reason: in linear algebra, only if it is real and symmetric does a positive definite matrix possess all positive eigenvalues. The matrix (10), however, is a complex one, making the analysis on restriction of positive energy meaningless.

Actually, in a strong bi-isotropic medium with constitutive relations like Eqs. (5) and (6), the complex energy for time-harmonic electromagnetic field can be expressed as

$$\phantom{\rule{1.8em}{0ex}}=\overline{D}\bullet \frac{\overline{E}}{2}+\overline{B}\bullet \frac{\overline{H}}{2}$$

$$\phantom{\rule{10.3em}{0ex}}=\frac{\epsilon {\mid \overline{E}\mid}^{2}}{2}+i\kappa \overline{H}\bullet \overline{E}+\frac{\mu {\mid \overline{H}\mid}^{2}}{2}-i\kappa \overline{E}\bullet \overline{H}$$

$$\phantom{\rule{3.8em}{0ex}}=\frac{\epsilon {\mid \overline{E}\mid}^{2}}{2}+\frac{\mu {\mid \overline{H}\mid}^{2}}{2}.$$

Even if the strong bi-isotropic medium is not frequency dispersive, i.e.
*κ*
^{2} >
*με* for the whole frequency range, the
energy will still remain positive as long as the permittivity and permeability are
positive, under the weak spatial dispersion condition. This is quite different from
Veselago’s medium since there is no bandwidth limitation and the
frequency dispersive resonances are no longer required. In another words, the strong
chiral medium does not contradict energy conservation, at least in the weak spatial
dispersion model.

Therefore, the real reason for traditional strong-chirality limitation is neither negative wavevector nor energy conservation. Next we will point out two other important arguments.

First, with the assumption that *ε*>0,
*μ* > 0,
*κ*> 0 and $\kappa >\sqrt{\mu \epsilon}$, we can easily show that
*ε _{DBF}*,

*μ*and

_{DBF}*β*become negative on transformation between Pasteur constitutive relations and DBF relations shown in Eqs. (7)–(9). This was considered absolutely unacceptable before people discovered the possibility of Veselago’s medium. Actually, strong chiral medium can be equivalent to Veselago’s medium for the right circularly polarized wave [12, 15]. The negative

*ε*and

_{DBF}*μ*have shown such a point. Hence the negative sign in the DBF model is not strange at all, since we realize effective double-negative with a strong chirality parameter instead of simultaneous frequency resonances. For a limiting case, the chiral nihility [12], in which

_{DBF}*ε*→ 0 and

*μ*→ 0 while

*κ*

*≠*0, the parameters in DBF representation become

*ε*→ ∞,

_{DBF}*μ*→ ∞ and

_{DBF}*β*= -1/(

*ωκ*) remains a finite value after a simple mathematical analysis. There is no evidence that strong chirality cannot exist in this aspect.

Second is the effectiveness of linear models. Similar to the case that linear optical
and electromagnetic models can no longer deal with very strong optical intensity and
electromagnetic field, we introduce nonlinear optics to take into account the higher
order terms of polarization. If the spatial dispersion is strong enough, the higher
order coupling terms cannot be neglected as before [7]. People used to mistake strong chirality with strong spatial
dispersion, hence adding a limitation to the chirality parameter that $\kappa <\sqrt{\mu \epsilon}$. We believe that this is the most probable reason. However, the
strong spatial dispersion is embodied in the DBF model, e.g. the value of
*β*, while the strong chirality is represented by the
Pasteur model, e.g. the ratio of *κ* to $\sqrt{\epsilon \mu}$. That is to say, strong chirality does not necessarily lead to
strong spatial dispersion.

Based on Eqs. (7)–(9), we have computed
*β* and
*ε _{DBF}*/

*ε*or

*μ*/μ versus $\frac{\kappa}{\sqrt{\epsilon \mu}}$, as shown in Figs. 1 and 2. When

_{DBF}*κ*is very close to $\sqrt{\mu \epsilon}$, the value of β is quite large, indicating a strong spatial dispersion. Hence the singular point is the very point of traditional limitation. However, with

*κ*continuously increasing, the spatial dispersion strength falls down very quickly. Therefore, if

*κ*is not near $\sqrt{\mu \epsilon}$, e.g. $\kappa <0.7\sqrt{\mu \epsilon}$ or $\kappa >1.3\sqrt{\mu \epsilon}$, we need not take nonlinear terms into consideration at all. Hence the strong spatial dispersion and nonlinearity cannot put an upper limitation to chirality parameters either.

When *κ* is close to $\sqrt{\mu \epsilon}$ where the spatial dispersion is strong, we need to take
higher-order terms in the DBF relations

where *β _{n}* stands for the spatial dispersion of
the

*n*th order. We remark that the above is different from classical nonlinear optics because it is strong spatial dispersion instead of strong field intensity. Hence it is not a power series of

*E*¯ and

*H*¯ fields.

Nevertheless, the Pasteur relations should retain the same form as Eqs. (5) and (6) as long as the medium is lossless and reciprocal, no matter
how strong the spatial dispersion is. The only thing to be changed is the
transformation relation between DBF and Pasteur models, which becomes much more
complicated. That is to say, though there are a lot of higher-order rotation terms,
*D*¯ can still be represented as a real part
proportional to *E*¯ and an imaginary part proportional to
*H*¯ with modified coefficients.
*B*¯ has similar representations to
*D*¯. The nonlinear terms contribute to the alteration of
effective *ε*, *μ* and
*κ* in the Pasteur model, which might be negative,
leading to the energy problem again.

Actually, when introducing higher order terms in the DBF model,
*ε _{DBF}* and

*μ*will be altered. Every rotation term includes real and imaginary components, related to

_{DBF}*E*¯ and

*H*¯, respectively. Comparing to the DBF model, the Pasteur model is relatively stable since its

*ε*stands for the total proportion of

*D*¯ to

*E*¯. Similar conclusions are valid for μ.

## 4. Conclusions

From Fig. 1, it is clear that enhancing spatial dispersion will not lead to strong chirality and will reach the traditional limitation point. This is why we have never succeeded in realizing strong chirality no matter how large the asymmetry and spatial dispersion.

Fortunately, as pointed out earlier, strong chirality does not require strong spatial
dispersion. Hence the most important difference between strong and weak chirality is
that *κ* and *β* have opposite
signs, which necessarily leads to negative
*ε _{DBF}* and

*μ*. Here,

_{DBF}*κ*stands for chirality and β is the coefficient of the first order for spatial dispersion. Strong chirality stems from using one type of spatial dispersion to get the conjugated stereoisomer, or chirality. That is to say, when we manage to use negative

*β*to realize positive

*κ*, or vice versa, there is strong chirality, (seen from Fig. 1). Comparing with the fact that Veselago’s medium requires effective double negativeness from natural double positive materials, getting one type of chirality from the conjugated type of spatial dispersion maybe another substitutive way to support backward-wave propagation.

In conclusion, a strong chiral medium behaves like Veselago’s medium. Under the weak spatial dispersion, the energy is always positive for a chiral medium. We show that strong chirality does not equal strong spatial dispersion, which occurs only around a singular point. Even in this small region with very strong spatial dispersion, the Pasteur model is meaningful. Neither spatial dispersion nor energy will restrict chirality from being stronger, but we cannot realize strong chirality only by increasing the spatial dispersion. The necessary condition for a strong chiral medium is that the chirality and spatial dispersion are of conjugated types.

We remark that strong chiral media have found wide applications in the negative refraction and supporting of backward waves, which have been discussed in details in Refs. [15]–[21].

## Acknowledgement

This work was supported in part by the National Basic Research Program (973) of China under Grant No. 2004CB719802, in part by the National Science Foundation of China under Grant Nos. 60671015, 60496317, 60225001, and 60621002, and in part by the National Doctoral Foundation of China under Grant No. 20040286010.

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