On the rotational stability of nonspherical particles driven by the radiation torque

doi:10.1364/OE.15.008960

« Show journal navigation

On the rotational stability of nonspherical particles driven by the radiation torque

Ferdinando Borghese, Paolo Denti, Rosalba Saija, and Maria Antonia Iati »View Author Affiliations

Optics Express, Vol. 15, Issue 14, pp. 8960-8971 (2007)
http://dx.doi.org/10.1364/OE.15.008960

View Full Text Article

Acrobat PDF (2050 KB)

Journal Search
Article Lookup

Article Tools

Citations

Alert me when this article is cited
Export Citation/Save

Article Navigation

▸ Article Outline
– Abstract
1. Introduction
2. Radiation torque
3. Radiation torque on aggregated spheres
4. Axial averages
5. Conclusive remarks
– References and links

Article Tools
Full Text
Article Info
References
Cited By
Figures
Metrics
Download PDF

Viewing Equations in the
HTML Article

Optimal Viewing Recommendations

Full Text
Article Info
References (29)
Cited By
Figures (8)
Metrics

Abstract

We calculate the radiation torque exerted by a monochromatic plane wave, either unpolarized or linearly polarized, on aggregates of spheres and investigate the stability of the resulting rotational motion. In fact, neglecting any braking momenta we calculate the component of the electromagnetic torque orthogonal to the principal axis of maximum moment of inertia through the center of mass (transverse torque), as a function of the direction of propagation of the incident field. The aggregates we study are composed of homogeneous spheres, possibly of different materials. The electromagnetic torque is calculated through the transition matrix approach along the lines of the theory reported in our recent paper [F. Borghese, P. Denti, R. Saija and M. A. Iatì, Opt. Express 14, 9508 (2006)]. When the transverse component of the electromagnetic torque is small or vanishes the rotational motion driven by the component along the principal axis of inertia may be nearly stable.

1. Introduction

The conservation of the angular momentum for the combined system of radiation field and particles implies that an electromagnetic wave impinging on a particle exerts a mechanical torque on the latter [1

J. D. Jackson, Classical electrodynamics , 2d edition (Wiley, New York, 1975).

]. This fact has found useful applications in the manipulation of micro- and nano-particles [2

M. E. J. Friese, T.A. Nieminen, N. R. Heckenberg, and H. Rubinsztein-Dunlop, “Optical alignment and spinning of laser-trapped microscopic particles,” Nature 394, 348–349 (1998). [CrossRef]

, 3

M. E. J. Friese, T.A. Nieminen, N. R. Heckenberg, and H. Rubinsztein-Dunlop, “Erratum: Optical alignment and spinning of laser-trapped microscopic particles,” Nature 395, 621 (1998). [CrossRef]

]. For instance, the torque experienced by propeller-shaped particles embedded into a viscous fluid and trapped by optical tweezers induces rotations that through microrheo-logic studies give information on the properties both of the fluid and of the particles themselves [4

P. Galajda and P. Ormos, “Rotation of microscopic propellers in laser tweezers,” J. Opt. B: Quantum Semiclass. Opt. 4, S78–S81 (2002). [CrossRef]

]. The electromagnetic torque is also of interest for astrophysicists, because, according to the suggestion of Purcell [5

E. M. Purcell, “Suprathermal rotation of interstellar grains,” Astrophys. J. 231, 404–416 (1979). [CrossRef]

], it is considered as a relevant agent for the alignment of cosmic dust grains, that is required to explain the linearly polarized component of the starlight [6

A. Lazarian, “Physics of grain alignment,” in Cosmic evolution and galaxy formation, AIP Conference series 3, (1999).

The actual evaluation of the radiation torque requires calculating the radiation field in the presence of the particles. For instance, Draine and Weingartner [7

B. T. Draine and J. C. Weingartner, “Radiative torques on interstellar grains. I. Superthermal spin-up,” Astrophys. J. 470, 551–565 (1996). [CrossRef]

, 8

B. T. Draine and J. C. Weingartner, “Radiative torques on interstellar grains. II. Grain alignment,” Astrophys. J. 480, 633–646 (1997). [CrossRef]

] calculated through the discrete dipole approximation (DDA) [9

E. M. Purcell and C. R. Pennypacker, “Scattering and absorption of light by nonspherical dielectric grains,” Astrophys. J. 186, 705–714 (1973). [CrossRef]

, 10

B. T. Draine and P. J. Flatau, “Discrete dipole approximation for scattering calculations,” J. Opt. Soc. Am. A 11, 1491–1499 (1994). [CrossRef]

] the field scattered by model cosmic grains and the torque experienced by the latter. Unfortunately, due to the large amount of calculations required by the DDA, it is not surprising that the above authors dealt with a few simple model particles only.

The computational effort is more sustainable, even for particles with a complex structure, by using the multipole expansion of the field in the framework of the transition matrix approach [11

P. C. Waterman, “Symmetry, unitarity and geometry in electromagnetic scattering,” Phys. Rev. D4, 825–839 (1971).

]. As far as we know, the first complete solution to the problem of radiation torque in terms of multipole fields is due to Marston and Crichton [12

P. L. Marston and J. H. Crichton, “Radiation torque on a sphere caused by a circularly-polarized electromagnetic wave,” Phys. Rev. A 30, 2508–2516 (1984). [CrossRef]

] who dealt with the torque exerted by an elliptically polarized plane wave on a homogeneous sphere. More recently, the multipole field expansion has been exploited by de Abajo [13

F. J. García de Abajo, “Electromagnetic forces and torques in nanoparticles irradiated by plane waves,” J. Quant. Spectrosc. Radiat. Trasfer 89, 3–9 (2004). [CrossRef]

, 14

F. J. García de Abajo, “Momentum transfer to small particles by passing electron beams,” Phys. Rev. B 70, 115422 (2004). [CrossRef]

] to calculate the radiation torque on model nonspherical particles. The transition matrix approach was further extended by the present authors to the case of particles shaped as aggregates of spherical scatterers [15

F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism,” Opt. Express 14, 9508–9521 (2006). [CrossRef] [PubMed]

, 16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

, 21

F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism: erratum,” Opt. Express 15, 6946 (2007). [CrossRef] [PubMed]

, 22

The Erratum to Ref. [16] can be found at http://dfmtfa.unime.it/profs/borghese/ferdinandoborghese.html.

], the stability of whose induced rotations has also been discussed to some extent. Our main conclusion was that when a circularly polarized plane wave impinges on a cluster composed of identical spheres along one of the principal axes of inertia through the center of mass the induced rotations are nearly stable even when the cluster lacks any symmetry.

Nevertheless, in laboratory experiments linearly polarized light is mostly used, whereas in an astrophysical environment the light is mainly unpolarized. Moreover, the rotations driven by radiation torque may be unstable, whatever the polarization, when the dielectric properties of the aggregated spheres are not equal to each other. In fact, the mechanical properties of the clusters, such as the moment of inertia tensor, are determined by the distribution of the masses, whereas the electromagnetic torque is determined by the distribution of the dielectric properties, mainly by the absorptivity of the component spheres. Therefore, the purpose of this paper is to report a study of the rotational stability of clusters composed of spheres with different dielectric properties, when the electromagnetic torque is due to an unpolarized plane wave or to a linearly polarized plane wave.

Indeed, the problem of rotational stability has already been faced by Draine and Weingartner in an astrophysical context by solving numerically the equations of rotational motion of a particle of known morphology and refractive index [8

B. T. Draine and J. C. Weingartner, “Radiative torques on interstellar grains. II. Grain alignment,” Astrophys. J. 480, 633–646 (1997). [CrossRef]

]. Here, we adopt a simpler approach: we calculate the electromagnetic torque exerted on the particles by a plane wave. Then, we calculate the component of the torque in a plane orthogonal to the central axis of maximum moment of inertia as a function of the direction of incidence of the incoming radiation. It is intuitive that a nearly stable rotation around this axis cannot occur unless the transverse torque is small.

2. Radiation torque

In this section we report the essentials of the theory of the torque exerted by a monochromatic plane wave on aggregated spheres. The interested reader is referred to our recent paper [15

F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism,” Opt. Express 14, 9508–9521 (2006). [CrossRef] [PubMed]

] and to Ref. [16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

] for further details.

We assume that the particle of interest is embedded into a homogeneous medium of refractive index n. Then, a monochromatic wave exerts a torque on the particle given by

{\vec{Γ}}_{rad} = - \oint \hat{n} \cdot 〈 Т_{M} 〉 \times r d S,

(1)

where

\hat{n}

is the unit outward normal to an arbitrarily chosen closed surface S that surrounds the particle and

〈 Т_{M} 〉 = \frac{1}{8 π} Re [n^{2} E \otimes E^{*} + B \otimes B^{*} - \frac{1}{2} (n^{2} E \cdot E^{*} + B \cdot B^{*}) ∣]

(2)

is the time averaged Maxwell stress tensor, I being the unit dyadic. Of course, in Eq. (2)

E = E_{I} + E_{S}, B = B_{I} + B_{S},

i.e., E and B are the superposition of the incident and of the scattered fields.

We found convenient to choose the integration surface S to be a sphere of arbitrary radius with its center within the particle, so that Eq. (1) becomes

{\vec{Γ}}_{rad} = - r^{3} \int_{Ω} \hat{r} \cdot 〈 Т_{M} 〉 \times \hat{r} dΩ .

(3)

Since

\hat{r} \cdot I \times \hat{r} = 0

, the last two terms in Eq. (2) give no contribution to the integral, and by choosing the radius of the integration sphere to be large, possibly infinite, we can resort to the asymptotic expression of the fields. Nevertheless, it should be borne in mind that using the customary far zone expression of the scattered field in terms of the scattering amplitude

E_{S} = \frac{\exp (ikr)}{r} f ({\hat{k}}_{S}, {\hat{k}}_{I})

yields a vanishing result because

\hat{r}

∙ f = 0 [23

M. I. Mishchenko, “Radiation force caused by scattering, absorption and emission of light by nonspherical particles,” J. Quant. Spectrosc. Radiat. Transfer 70, 811–816 (2001). [CrossRef]

]. Therefore, the correct procedure requires that, after solving the problem of scattering, the fields be expanded for large r and all terms that give contributions of order 1/r ³ to the integrand in Eq. (3) be retained.

Since the polarization of the field is relevant, we introduce a pair of mutually orthogonal unit vectors, say

\hat{u}

_η, such that

{\hat{u}}_{1} \times {\hat{u}}_{2} = {\hat{k}}_{I},

where

\hat{k}

_I is the direction of the propagation of the incident plane wave. Note that the vectors

\hat{u}

_η may be either real (linear polarization basis) or complex (circular polarization basis). In case the linear polarization basis is used the subscripts η = 1, 2 denote polarization parallel and perpendicular to a fixed plane of reference through

\hat{k}

_I, respectively, whereas, when the circular basis is used, η = 1, 2 denote left and right polarization, respectively.

Both the incident and the scattered field are expanded in a series of vector multipole fields [16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

]. Accordingly,

E_{I} = \sum_{η} E_{0 η} {\hat{u}}_{η} \exp (i k \cdot r) = \sum_{η} E_{0 η} \sum_{plm} J_{l m}^{(p)} (r, k) W_{Iη l m}^{(p)},

(4a)

E_{S} = \sum_{η} E_{0 η} \sum_{plm} H_{l m}^{(p)} (r, k) A_{η l m}^{(p)},

(4b)

where k = nk _v, with k _v = ω/c, is the propagation constant of the incident plane wave. We also define the multipole fields in (4a) according to

J_{l m}^{(1)} (r, k) = j_{l} (k r) X_{lm} (\hat{r}), J_{l m}^{(2)} (r, k) = \frac{1}{k} \nabla \times J_{l m}^{(1)} (r, k),

(5)

where X _lm(

\hat{r}

) denotes vector spherical harmonics [1

J. D. Jackson, Classical electrodynamics , 2d edition (Wiley, New York, 1975).

]. The multipole fields

H_{l m}^{(p)}

(r,k) in (4b) are identical to the

J_{l m}^{(p)}

(r, k) fields (5) except for the substitution of the spherical Hankel functions of the first kind h_l (kr) in place of the spherical Bessel functions j_l (kr). The (known) multipole amplitudes of the incident field

W_{I η l m}^{(p)}

are defined in [15

F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism,” Opt. Express 14, 9508–9521 (2006). [CrossRef] [PubMed]

, 16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

], whereas the amplitudes of the scattered field

A_{η l m}^{(p)}

are calculated by imposing the customary boundary conditions across the surface of the particle. The amplitudes

A_{η l m}^{(p)}

bear the index η to recall the polarization of the incident field, and are related to the

W_{I η l m}^{(p)}

by [16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

]

A_{η l m}^{(p)} = \sum_{p' l' m'} 𝓢_{l m l ′m'}^{(p p')} W_{I η l' m'}^{(p')} .

(6)

Equation (6) defines the elements

𝓢_{l m l ′m'}^{(p p')}

of the so-called transition matrix of the particle [11

P. C. Waterman, “Symmetry, unitarity and geometry in electromagnetic scattering,” Phys. Rev. D4, 825–839 (1971).

]. Now, the particles the present study is going to deal with either actually are, or can be modeled as aggregates of spheres. We calculate

𝓢_{l m l ′m'}^{(p p')}

for such aggregates always starting with the inversion of the matrix of the linear system that is obtained by imposing to the fields the boundary conditions across each of the spherical surfaces [17

R. Saija, M. A. Iatì, P. Denti, F. Borghese, A. Giusto, and O. I. Sindoni, “Efficient light-scattering calculations for aggregates of large spheres,” Appl. Opt. 42, 2785–2793 (2003). [CrossRef] [PubMed]

, 18

R. Saija, M. A. Iatì, F. Borghese, P. Denti, S. Aiello, and C. Cecchi-Pestellini, “Beyond Mie theory: the transition matrix approach in interstellar dust modeling,” Astrophys. J. 559, 993–1004 (2001). [CrossRef]

]. The order of the matrix to be inverted is 2Nl _M(l _M + 2), where N is the number of the spheres of the aggregate and l _M is the maximum value of l to be retained in the multipole expansions of the fields (4) in order to get convergence for the quantities of interest. The convergence of such kind of calculations is studied in Ref. [17

]. A comprehensive treatment of all the abovementioned topics related to the calculation of the transition matrix can be found in Ref. [16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

]. Anyway, we are well aware that other procedures for calculating the transition matrix elements have been devised, such as the iterative procedures of Xu [19

Y.-L. Xu, “Electromagnetic scattering by an aggregate of spheres,” Appl. Opt. 34, 4573–4588 (1995). [CrossRef] [PubMed]

] and of Chew [20

W. C. Chew, Waves and fields in inhomogeneous media , IEEE Press Series on Eletromagnetic Waves (Institute of Electrical and Electronic Engineers, Piscataway, N.J., 1990).

], but we never used them for reasons that are fully expounded in Ref. [17

Let us now define the vector

\vec{Γ}

such that

{\vec{Γ}}_{Rad} = Re (\vec{Γ})

and in terms of whose spherical components [24

E. M. Rose, Elementary theory of angular momentum , (Wiley, New York, 1956).

] the cartesian components of

{\vec{Γ}}_{Rad}

read

Γ_{Rad x} = Re [\frac{1}{\sqrt{2}} (Γ_{- 1} - Γ_{1})], Γ_{Rad y} = Re [\frac{i}{\sqrt{2}} (Γ_{- 1} + Γ_{1})], Γ_{Rad z} = Re (Γ_{0}),

(7)

where

Γ_{μ} = \sum_{η \bar{η}} I_{I \bar{η} η} Γ_{μ; \bar{η} η},

(8)

with

I_{I \bar{η} η} = E_{0 \bar{η}}^{*} E_{0 η}

. At this stage, the procedure fully expounded in [15

F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism,” Opt. Express 14, 9508–9521 (2006). [CrossRef] [PubMed]

] and [16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

] yields for

Γ_{μ; η \bar{η}}

the expression

Γ_{μ; \bar{η} η} = Γ_{μ; \bar{η} η}^{(ext)} - Γ_{μ; \bar{η} η}^{(sca)},

(9)

where

Γ_{μ; \bar{η} η}^{(ext)} = c_{Γ} \sum_{plm} s_{μ; l m} W_{Iη l, m - μ}^{(p)} A_{\bar{η} l m}^{(p) *},

(10)

whereas the quantities

Γ_{μ; η \bar{η}}^{(sca)}

are identical to the

Γ_{μ; η \bar{η}}^{(ext)}

above, except for the substitution of

A_{η l m}^{(p)}

in place of

W_{I η l m}^{(p)}

and for the change of the sign. In Eq. (10) we define c _Γ = n ²/8πk ³ and

s_{- 1; l m} = - \sqrt{\frac{(l - m) (l + 1 + m)}{2}}, s_{0; l m} = - m, s_{1; l m} = \sqrt{\frac{(l + m) (l + 1 - m)}{2}} .

(11)

In [15

F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism,” Opt. Express 14, 9508–9521 (2006). [CrossRef] [PubMed]

] we demonstrated that Eqs. (7)–(11), when applied to a homogeneous sphere, reproduce the results of Marston and Crichton [12

P. L. Marston and J. H. Crichton, “Radiation torque on a sphere caused by a circularly-polarized electromagnetic wave,” Phys. Rev. A 30, 2508–2516 (1984). [CrossRef]

Let us assume that the particles we consider are freely rotating at a temperature T. Then, their angular velocity is given by

ω_{T} = \sqrt{\frac{k_{B} T}{I}},

where k _B is the Boltzman constant and I is the moment of inertia around the axis of rotation; ω_T ≈ 10⁴sec^-1 at T = 100K for the particles we deal with. Therefore, according to the suggestion of Draine and Weingartner [7

B. T. Draine and J. C. Weingartner, “Radiative torques on interstellar grains. I. Superthermal spin-up,” Astrophys. J. 470, 551–565 (1996). [CrossRef]

, 8

B. T. Draine and J. C. Weingartner, “Radiative torques on interstellar grains. II. Grain alignment,” Astrophys. J. 480, 633–646 (1997). [CrossRef]

], it is reasonable to assume that at such an angular velocity the particles should experience only a torque averaged over a complete rotation. In Ref. [15

F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism,” Opt. Express 14, 9508–9521 (2006). [CrossRef] [PubMed]

] we explained as such average of the radiation torque can be calculated through an analytic procedure, to which we will refer as axial averaging. The relevant formulas are

〈 Γ_{μ; \overset{}{\bar{η}} η}^{(ext)} 〉 = c_{Γ} \sum_{plm} s_{μ; l m} \sum_{\overset{}{\bar{p}} \overset{}{\bar{l}}} W_{I η l, m - μ}^{(p)} {\overset{}{\bar{𝓢}}}_{lm \bar{l} m}^{(p \overset{}{\bar{p}}) *} W_{I \overset{}{\bar{η}} \overset{}{\bar{l}} m}^{(\overset{}{\bar{p}}) *},

〈 Γ_{μ; \overset{}{\bar{η}} η}^{(sca)} 〉 = - c_{Γ} \sum_{plm} s_{μ; l m} \sum_{\overset{}{\bar{p}} \overset{}{\bar{p}'}} \sum_{\overset{}{\bar{l} \bar{l}'}} \sum_{m'} {\overset{}{\bar{𝓢}}}_{l, m - μ, \overset{}{\bar{l}}, m' - μ}^{(p \overset{}{\bar{p}})} W_{I η \bar{l}, m' - μ}^{(\overset{}{\bar{p}})} {\overset{}{\bar{𝓢}}}_{l m \bar{l}' m'}^{(p \overset{}{\bar{p}'}) *} W_{I \overset{}{η} \bar{l}' m'}^{(\overset{}{p}) *},

(12)

where the bar over the elements of the transition matrix indicates that they are calculated in a frame of reference fixed to the cluster. We stress that the formulas corresponding to (12) reported in Refs. [15

F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism,” Opt. Express 14, 9508–9521 (2006). [CrossRef] [PubMed]

, 16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

] were written with wrong indices but that the calculations were performed using the correct expressions above [21

F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism: erratum,” Opt. Express 15, 6946 (2007). [CrossRef] [PubMed]

, 22

The Erratum to Ref. [16] can be found at http://dfmtfa.unime.it/profs/borghese/ferdinandoborghese.html.

3. Radiation torque on aggregated spheres

Since in this paper we focus on the stability of the rotation driven by the radiation torque, we resolved to neglect any other torque. For instance, we neglect the frictional torque due to the surrounding medium and the braking torques due to magnetic fields. In the present case, we assumed that the particles are embedded in vacuo and, accordingly, we set n = 1. We stress, however, that the mechanical effects of the embedding medium as well as those of magnetic fields should be taken into account when a realistic description of the dynamics of the particles is required. In this respect let us recall that a steady rotation of a free particle can occur only around one of the principal axes of inertia through the center of mass and that in case braking momenta are applied a stable rotation may occur only around the principal axis of maximum moment of inertia [25

H. Goldstein, C. Poole, and J. Safko, Classical Mechanics , 3d edition (Addison-Wesley, Reading, Mass., 2002).

The quantity which we actually calculated is the adimensional vector

T_{η} = \frac{8 π k}{I_{I} σ_{T η}} {\vec{Γ}}_{Rad η},

where

{\vec{Γ}}_{Rad η}

is the radiation torque calculated for incident light with polarization η and σ _Tη is the extinction cross section of the particle concerned for polarization η. All the aggregates that we consider hereafter are composed of five spherical homogeneous scatterers whose space arrangement is chosen so that no symmetry is present, but each of the aggregated spheres in contact with at least one other sphere of the aggregate. The materials we chose to build the aggregates under study are the so-called astronomical silicates and amorphous carbon [26

B. T. Draine and H. M. Lee, “Optical properties of interstellar graphite and silicate grains,” Astrophys. J. 285, 89–108 (1984). [CrossRef]

] to which we added aluminum [27

P. H. Berning, G. Hass, and P. R. Madden, “Reflectance-increasing coatings for the vacuum ultraviolet and their applications,” J. Opt. Soc. Am. 50, 586–597 (1960). [CrossRef]

] and silver [28

U. Kreibig, “Electronic properties of small silver particles: the optical constants and their temperature dependence,” J. Phys. F: Metal Phys. 4, 999–1014 (1974). [CrossRef]

] because their density and/or dielectric function are the most different from those of the other materials. The composition of the aggregates is given in Table 2 where the radii of the component spheres are also reported. In this respect we stress that in cluster D the radius of the sphere of Ag is 28 nm, so that its mass equals that of a sphere of carbon. Table 3 reports, for all the clusters we investigated, the coordinates in nm of the centers of the spheres, with respect to a frame of reference with origin in the center of is mass and the axes along the principal axes of inertia, the z axis being chosen along the axis of maximum moment of inertia. We also report the values of the principal moments of inertia.

Table 1. Densities in g/cm³ and dielectric constants at λ = 380nm of the materials that compose the clusters

	ρ	ε _r	ε _i
Si	3.30	3.012	0.1005
C	1.85	2.773	2.766
Al	2.70	-16.49	2.856
Ag	10.49	-3.2	1.65

Table 2. Composition of the clusters and radii of the component spheres in nm

A	4Si	b _Si=50	1Al	b _Al=50
B	4C	b _C=50	1Al	b _Al=50
C	4C	b _C=50	1Ag	b _Ag=50
D	4C	b _C=50	1Ag	b _Ag=28

Table 3. Coordinates of the centers of the spheres (in nm) with respect to the frame of reference with origin at the center of mass. The principal moments of inertia are also given in g∙cm² × 10²⁸

Cluster A
x	37.945	37.771	-52.580	-141.093	124.855	I_xx = 3.056
y	102.858	2.876	-37.061	-3.717	-46.254	I_yy = 8.011
z	-3.041	-1.160	-19.663	-14.312	9.000	I_zz = 10.000
Cluster B
x	41.771	32.317	-61.312	-146.417	114.447	I_xx = 2.336
y	87.298	-12.249	-43.445	-2.367	-69.346	I_yy = 4.652
z	-1.741	-0.860	-19.856	14.357	8.901	I_zz = 6.327
Cluster C
x	-45.118	12.972	109.499	162.765	-29.401	I_xx = 4.013
y	-30.826	50.570	30.477	-47.477	141.221	I_yy = 5.949
z	-0.457	-0.563	-20.447	14.400	8.802	I_zz = 8.892
Cluster D
x	36.207	36.414	-53.759	-142.421	123.711	I_xx = 1.456
y	81.736	3.757	-36.662	-3.545	-44.941	I_yy = 4.465
z	-3.983	-1.148	-19.471	14.447	9.252	I_zz = 5.372

All our calculations were performed using l _M = 12 in order to ensure the complete cover-gence of the quantities of interest [16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

, 17

The results of our calculations for the transverse component of the radiation torque on clusters A–D are reported in Figs. 1–4, both for unpolarized light and for linearly polarized light. More precisely, panels (a) of each figure show a sketch of the geometry whereas panels (b) report

T_{⊥} = {(T_{x}^{2} + T_{y}^{2})}^{1 / 2}

for unpolarized light and panels (c) and (d) for linearly polarized light with η = 1,2, respectively, as a function of the direction of incidence of the incoming radiation, given by the polar angles ϑ _I and φ _I. The plane of reference for the linear polarization is the meridional plane defined by k _I and the z axis.

First, we note that the transverse component T _⊥ does not vanish for incidence either parallel (ϑ _I = 0°) or antiparallel (ϑ _I = 180°) to the axis of maximum moment of inertia, and that, in linear polarization, it is not constant as φ _I varies. On the other hand, all the graphs show a minimum for some value of ϑ _I. In our opinion, the first feature stems from the mismatch between the distribution of the masses and the distribution of the dielectric properties. In fact, we already stressed in Ref. [16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

] that the vanishing of the transverse torque can occur only when the aggregate has a cylindrical symmetry axis coincident with the axis of rotation and the incident wavevector is along this axis. In turn, the existence of the minima for ϑ _I ≠ 0 suggests that the rotation may be stable when the incidence is not along a principal axis of inertia.

4. Axial averages

The graphs presented in Sect. 3 give the dependence of the transverse torque T _⊥ as a function of the direction of incidence of the field. As regards the dependence on φ _I, it may be useful to remark that it gives information on the behaviour of T⊥ as a function of the orientation of the particle around the axis of maximum moment of inertia (z axis). Therefore, provided the particle is rotating around the z axis with a sufficiently high speed, it makes sense to consider the axial averages around the axis of rotation. Accordingly, in Figs. 5–8 we present the axial averages

〈 T_{⊥} 〉 = \sqrt{{〈 T_{x} 〉}^{2} + {〈 T_{y} 〉}^{2}}

and 〈T_z 〉 for the aggregates considered so far, both for unpolarized light and for linearly polarized light with η = 1,2. 〈T_z 〉 gives the torque that actually drives the rotational motion of the aggregate around the z axis.

Fig. 1. T _⊥ as a function of the angles of incidence ϑ _I and φ _I for cluster A of four spheres of astronomical silicates (gray) and one sphere of aluminum (blue) whose geometry is shown in (a). The light is unpolarized in (b), and linearly polarized with η = 1, 2 in (c) and (d), respectively.

Fig. 2. Same of Fig. 1 for cluster B of four spheres of amorphous carbon (gray) and one sphere of aluminum (blue) whose geometry is shown in (a).

Fig. 3. Same of Fig. 1 for cluster C of four spheres of amorphous carbon (gray) and one sphere of silver (blue) whose geometry is shown in (a).

Fig. 4. Same of Fig. 1 for cluster D of four spheres of amorphous carbon (gray) and one sphere of silver (blue) whose geometry is shown in (a). The radius of the silver sphere is 28nm so that its mass is equal to the mass of a sphere of carbon.

Fig. 5. Axial averages 〈T⊥〉 and 〈T _∥〉 as a function of θ _I for cluster A.

We first note that in all the cases we considered the transverse torque vanishes for ϑ _I = 0° and for ϑ _I = 180°, i.e., for incidence along the axis of maximum moment of inertia. For this incidence 〈T_z 〉 never vanishes thus indicating that the particle is driven to accelerate its rotational motion. This result is not surprising because, according to Ref. [16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

], performing the axial average is equivalent to consider an average particle that is akin to an axially symmetric particle. When the axis around which the average is performed coincides with the direction of k _I the result quoted in Ref. [16

F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).

] follows at once. Moreover, the average of the transverse torque has a deep, nearly vanishing minimum also for values of ϑ _I that depend on the morphology of the cluster and on the polarization. At these values of ϑ _I the driving torque 〈T_z 〉, may be small but never vanishing.

It may be interesting to compare the results for cluster C and cluster D reported in Figs. 7 and 8, respectively. Actually both clusters have the same composition but the spheres of cluster C are all of the same volume, whereas those of cluster D all have the same mass. In view of the high density of silver, this implies that the principal moments of inertia of cluster C and D are quite different from each other and, as a result, the values of ϑ _I at which the average transverse torque becomes nearly vanishing are different. In particular, we note that 〈T _⊥〉 for cluster C nearly vanishes at ϑ _I ≈ 100° for whatever polarization, whereas 〈T _⊥〉 for cluster D does not show an analogous deep minimum when the incident light is linearly polarized with η = 2. For both clusters, however, the average driving torque does not vanish neither for incidence along the axis of maximum moment of inertia nor at incidence at which the transverse torque vanishes. We also notice that the driving torque is larger for cluster C that contains more silver and has thus a higher absorptivity.

Fig. 6. Same as Fig. 5 for cluster B.

Fig. 7. Same as Fig. 5 for cluster C.

5. Conclusive remarks

The results that we presented in Sects. 3 and 4 show that, at least for the cases we considered, the rotational stability under the affect of the radiation torque may be attained for incidence either parallel or antiparallel to the axis of maximum moment of inertia (z axis). In fact, although the instantaneous transverse torque does not vanish, its axial average does. Thus, provided the initial rotational speed around the z axis is large enough, one could expect that the torque exerted by the incident radiation has the only effect of increasing the angular speed. Of course, this increase of rotational speed cannot go on indefinitely. Nevertheless, we recall that any braking torque has been neglected, and that the presence of braking torques increases the stability of the rotational motion [25

H. Goldstein, C. Poole, and J. Safko, Classical Mechanics , 3d edition (Addison-Wesley, Reading, Mass., 2002).

]. This problem has been already discussed by Marston and Crichton [12

P. L. Marston and J. H. Crichton, “Radiation torque on a sphere caused by a circularly-polarized electromagnetic wave,” Phys. Rev. A 30, 2508–2516 (1984). [CrossRef]

Fig. 8. Same as Fig. 5 for cluster D.

We do not pretend that our present results apply to particles of any shape. Nevertheless, the choice of the cluster model may help approximating the shape of particles that are often met in practice. In this respect, let us recall that several particles of astrophysical interest are believed to be composed of aggregated spheres, possibly of different dielectric properties, and that the stability of alignment of the particles is relevant both for the dichroic polarization of the starlight (see, e.g., [29

G. Wurm and M. Schneiter, “Coagulation as a unifying element for interstellar polarization,” Astrophys. J. 567, 370–375 (2002). [CrossRef]

]) and for the occurrence of photochemical reactions both on their surface and in their interior.

References and links

1.	J. D. Jackson, Classical electrodynamics , 2d edition (Wiley, New York, 1975).
2.	M. E. J. Friese, T.A. Nieminen, N. R. Heckenberg, and H. Rubinsztein-Dunlop, “Optical alignment and spinning of laser-trapped microscopic particles,” Nature 394, 348–349 (1998). [CrossRef]
3.	M. E. J. Friese, T.A. Nieminen, N. R. Heckenberg, and H. Rubinsztein-Dunlop, “Erratum: Optical alignment and spinning of laser-trapped microscopic particles,” Nature 395, 621 (1998). [CrossRef]
4.	P. Galajda and P. Ormos, “Rotation of microscopic propellers in laser tweezers,” J. Opt. B: Quantum Semiclass. Opt. 4, S78–S81 (2002). [CrossRef]
5.	E. M. Purcell, “Suprathermal rotation of interstellar grains,” Astrophys. J. 231, 404–416 (1979). [CrossRef]
6.	A. Lazarian, “Physics of grain alignment,” in Cosmic evolution and galaxy formation, AIP Conference series 3, (1999).
7.	B. T. Draine and J. C. Weingartner, “Radiative torques on interstellar grains. I. Superthermal spin-up,” Astrophys. J. 470, 551–565 (1996). [CrossRef]
8.	B. T. Draine and J. C. Weingartner, “Radiative torques on interstellar grains. II. Grain alignment,” Astrophys. J. 480, 633–646 (1997). [CrossRef]
9.	E. M. Purcell and C. R. Pennypacker, “Scattering and absorption of light by nonspherical dielectric grains,” Astrophys. J. 186, 705–714 (1973). [CrossRef]
10.	B. T. Draine and P. J. Flatau, “Discrete dipole approximation for scattering calculations,” J. Opt. Soc. Am. A 11, 1491–1499 (1994). [CrossRef]
11.	P. C. Waterman, “Symmetry, unitarity and geometry in electromagnetic scattering,” Phys. Rev. D4, 825–839 (1971).
12.	P. L. Marston and J. H. Crichton, “Radiation torque on a sphere caused by a circularly-polarized electromagnetic wave,” Phys. Rev. A 30, 2508–2516 (1984). [CrossRef]
13.	F. J. García de Abajo, “Electromagnetic forces and torques in nanoparticles irradiated by plane waves,” J. Quant. Spectrosc. Radiat. Trasfer 89, 3–9 (2004). [CrossRef]
14.	F. J. García de Abajo, “Momentum transfer to small particles by passing electron beams,” Phys. Rev. B 70, 115422 (2004). [CrossRef]
15.	F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism,” Opt. Express 14, 9508–9521 (2006). [CrossRef] [PubMed]
16.	F. Borghese, P. Denti, and R. Saija, Scattering from model nonspherical particles , 2nd edition (Springer, Berlin, 2007).
17.	R. Saija, M. A. Iatì, P. Denti, F. Borghese, A. Giusto, and O. I. Sindoni, “Efficient light-scattering calculations for aggregates of large spheres,” Appl. Opt. 42, 2785–2793 (2003). [CrossRef] [PubMed]
18.	R. Saija, M. A. Iatì, F. Borghese, P. Denti, S. Aiello, and C. Cecchi-Pestellini, “Beyond Mie theory: the transition matrix approach in interstellar dust modeling,” Astrophys. J. 559, 993–1004 (2001). [CrossRef]
19.	Y.-L. Xu, “Electromagnetic scattering by an aggregate of spheres,” Appl. Opt. 34, 4573–4588 (1995). [CrossRef] [PubMed]
20.	W. C. Chew, Waves and fields in inhomogeneous media , IEEE Press Series on Eletromagnetic Waves (Institute of Electrical and Electronic Engineers, Piscataway, N.J., 1990).
21.	F. Borghese, P. Denti, R. Saija, and M. A. Iatì, “Radiation torque on nonspherical particles in the transition matrix formalism: erratum,” Opt. Express 15, 6946 (2007). [CrossRef] [PubMed]
22.	The Erratum to Ref. [16] can be found at http://dfmtfa.unime.it/profs/borghese/ferdinandoborghese.html.
23.	M. I. Mishchenko, “Radiation force caused by scattering, absorption and emission of light by nonspherical particles,” J. Quant. Spectrosc. Radiat. Transfer 70, 811–816 (2001). [CrossRef]
24.	E. M. Rose, Elementary theory of angular momentum , (Wiley, New York, 1956).
25.	H. Goldstein, C. Poole, and J. Safko, Classical Mechanics , 3d edition (Addison-Wesley, Reading, Mass., 2002).
26.	B. T. Draine and H. M. Lee, “Optical properties of interstellar graphite and silicate grains,” Astrophys. J. 285, 89–108 (1984). [CrossRef]
27.	P. H. Berning, G. Hass, and P. R. Madden, “Reflectance-increasing coatings for the vacuum ultraviolet and their applications,” J. Opt. Soc. Am. 50, 586–597 (1960). [CrossRef]
28.	U. Kreibig, “Electronic properties of small silver particles: the optical constants and their temperature dependence,” J. Phys. F: Metal Phys. 4, 999–1014 (1974). [CrossRef]
29.	G. Wurm and M. Schneiter, “Coagulation as a unifying element for interstellar polarization,” Astrophys. J. 567, 370–375 (2002). [CrossRef]

OCIS Codes
(260.2110) Physical optics : Electromagnetic optics
(260.2160) Physical optics : Energy transfer
(290.0290) Scattering : Scattering

ToC Category:
Physical Optics

History
Original Manuscript: May 7, 2007
Revised Manuscript: June 28, 2007
Manuscript Accepted: June 28, 2007
Published: July 5, 2007

Virtual Issues
Vol. 2, Iss. 8 Virtual Journal for Biomedical Optics

Citation
Ferdinando Borghese, Paolo Denti, Rosalba Saija, and Maria Antonia Iati, "On the rotational stability of nonspherical particles driven by the radiation torque," Opt. Express 15, 8960-8971 (2007)
http://www.opticsinfobase.org/oe/abstract.cfm?URI=oe-15-14-8960

Sort: Author | Year | Journal | Reset

References

J. D. Jackson, Classical Electrodynamics, 2nd ed., (Wiley, New York, 1975).
M. E. J. Friese, T. A. Nieminen, N. R. Heckenberg, and H. Rubinsztein-Dunlop, "Optical alignment and spinning of laser-trapped microscopic particles," Nature 394, 348-349 (1998). [CrossRef]
M. E. J. Friese, T. A. Nieminen, N. R. Heckenberg and H. Rubinsztein-Dunlop, "Erratum: Optical alignment and spinning of laser-trapped microscopic particles," Nature 395, 621 (1998). [CrossRef]
P. Galajda and P. Ormos, "Rotation of microscopic propellers in laser tweezers," J. Opt. B: Quantum Semiclassical Opt. 4, S78-S81 (2002). [CrossRef]
E. M. Purcell, "Suprathermal rotation of interstellar grains," Astrophys. J. 231, 404-416 (1979). [CrossRef]
A. Lazarian, "Physics of grain alignment," in Cosmic evolution and galaxy formation, AIP Conference series 3, (1999).
B. T. Draine and J. C. Weingartner, "Radiative torques on interstellar grains. I. Superthermal spin-up," Astrophys. J. 470, 551-565 (1996). [CrossRef]
B. T. Draine and J. C. Weingartner, "Radiative torques on interstellar grains. II. Grain alignment," Astrophys. J. 480, 633-646 (1997). [CrossRef]
E. M. Purcell and C. R. Pennypacker, "Scattering and absorption of light by nonspherical dielectric grains," Astrophys. J. 186, 705-714 (1973). [CrossRef]
B. T. Draine and P. J. Flatau, "Discrete dipole approximation for scattering calculations," J. Opt. Soc. Am. A 11, 1491-1499 (1994). [CrossRef]
P. C. Waterman, "Symmetry, unitarity and geometry in electromagnetic scattering," Phys. Rev. D 4, 825-839 (1971).
P. L. Marston and J. H. Crichton, "Radiation torque on a sphere caused by a circularly-polarized electromagnetic wave," Phys. Rev. A 30, 2508-2516 (1984). [CrossRef]
F. J. García de Abajo, "Electromagnetic forces and torques in nanoparticles irradiated by plane waves," J. Quant. Spectrosc. Radiat. Trasfer 89, 3-9 (2004). [CrossRef]
F. J. García de Abajo, "Momentum transfer to small particles by passing electron beams," Phys. Rev. B 70, 115422 (2004). [CrossRef]
F. Borghese, P. Denti, R. Saija and M. A. Iatì, "Radiation torque on nonspherical particles in the transition matrix formalism," Opt. Express 14, 9508-9521 (2006). [CrossRef] [PubMed]
F. Borghese, P. Denti and R. Saija, Scattering from Model Nonspherical Particles, 2nd ed., (Springer, Berlin, 2007).
R. Saija, M. A. Iatì, P. Denti, F. Borghese, A. Giusto and O. I. Sindoni, "Efficient light-scattering calculations for aggregates of large spheres," Appl. Opt. 42, 2785-2793 (2003). [CrossRef] [PubMed]
R. Saija, M. A. Iatì, F. Borghese, P. Denti, S. Aiello and C. Cecchi-Pestellini, "Beyond Mie Theory: The transition matrix approach in interstellar dust modeling," Astrophys. J. 559, 993-1004 (2001). [CrossRef]
Y.-L. Xu, "Electromagnetic scattering by an aggregate of spheres," Appl. Opt. 34, 4573-4588 (1995). [CrossRef] [PubMed]
W. C. Chew, Waves and Fields in Inhomogeneous Media, IEEE Press Series on Eletromagnetic Waves (IEEE, Piscataway, N. J., 1990).
F. Borghese, P. Denti, R. Saija and M. A. Iatì, "Radiation torque on nonspherical particles in the transition matrix formalism: erratum," Opt. Express 15, 6946 (2007). [CrossRef] [PubMed]
The Erratum to Ref. [16] can be found at http://dfmtfa.unime.it/profs/borghese/ferdinandoborghese.html.
M. I. Mishchenko, "Radiation force caused by scattering, absorption and emission of light by nonspherical particles," J. Quant. Spectrosc. Radiat. Transf. 70, 811-816 (2001). [CrossRef]
E. M. Rose, Elementary Theory of Angular Momentum, (Wiley, New York, 1956).
H. Goldstein, C. Poole, and J. Safko, Classical Mechanics, 3rd ed., (Addison-Wesley, Reading, Mass., 2002).
B. T. Draine and H. M. Lee, "Optical properties of interstellar graphite and silicate grains," Astrophys. J. 285, 89-108 (1984). [CrossRef]
P. H. Berning, G. Hass and P. R. Madden, "Reflectance-increasing coatings for the vacuum ultraviolet and their applications," J. Opt. Soc. Am. 50, 586-597 (1960). [CrossRef]
U. Kreibig, "Electronic properties of small silver particles: the optical constants and their temperature dependence," J. Phys. F: Metal Phys. 4, 999-1014 (1974). [CrossRef]
G. Wurm and M. Schneiter, "Coagulation as a unifying element for interstellar polarization," Astrophys. J. 567, 370-375 (2002). [CrossRef]

Cited By

Alert me when this paper is cited

OSA is able to provide readers links to articles that cite this paper by participating in CrossRef's Cited-By Linking service. CrossRef includes content from more than 3000 publishers and societies. In addition to listing OSA journal articles that cite this paper, citing articles from other participating publishers will also be listed.

Click here to see a list of articles that cite this paper