Optical properties of analogs of Titan’s aerosols produced by dusty plasma
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Analogs of Titan’s aerosols are produced in the laboratory as grains in a gas mixture, or as layers on a substrate. This production procedure enables the methane-nitrogen mixture composition to be changed. The aim of this paper is to understand the variations observed on the linear polarization of the scattered light as a function of the production conditions. The influence of the concentration of methane injected in the plasma will be discussed and compared with the previous work of Hadamcik et al. (2009a). The diameter of the grains are measured by SEM-FEG images. The decrease of absorption with increasing wavelength, measured by spectroscopic ellipsometry on layers, is observed for a decreasing initial methane ratio and analyzed in terms of an increasing ‘amine’ content in the materials. The phase function parameters of the linear polarization of the scattered light are discussed in terms of the diameters of the aggregates and of the constituent grains, and the variation of the refractive indices (mainly absorption). The polarization is found to be highly correlated with the constituent grain size. Finally, the experimental results are compared to polarization measurements from space of the Titan’s atmosphere.
Key wordsLight scattering polarization refractive indices tholins Titan aerosol
Titan’s atmosphere is mainly composed of nitrogen N2 and methane CH4. The CH4/N2 ratio varies with altitude. Energetic particles from Saturn’s magnetosphere and photochemical reactions dissociate N2 and CH4. The subsequent chemistry produces solid aerosols in the upper atmosphere which are widespread all around Titan through the atmospheric general circulation, giving the characteristic yellow color to the satellite.
Some physical properties of these aerosols have been deduced from the solar light scattered by the particles and its linear polarization. The observations have been performed by different space probes: Pioneer 11, Voyager 2 and Huygens (Tomasko and Smith, 1982; West et al., 1983; Tomasko et al., 2005). From a comparison between observations and numerical simulations of the particles and the light they scatter, fractal cluster-cluster aggregates with 3000 to 4500 constituent grains of 80-nm mean diameter seem to best describe Titan’s aerosols structure (Tomasko et al., (2008), (2009). The input parameters for the simulations (e.g. refractive indices) are obtained by measurements on analogs called tholins, which are produced in the laboratory by photochemical reactions or plasma discharges (Khare et al., 1984; Imanaka et al., 2004; Mahjoub et al., 2012; Sciamma-O’Brien et al., 2012).
The aim of this paper is to study the influence of the methane content of the plasma discharge on the linear polarization of the light scattered by tholins produced by the PAMPRE set-up (described in detail in Szopa et al., 2006).
This work completes an initial study carried out by Hadamcik et al. (2009a) on this type of tholins. The experiment produces tholins in the gas phase as dust particles, or as thin films on substrates. The linear polarization P of the light scattered by the dust particles is measured with the PROGRA2 instrument (see Renard et al., 2002, for further description). P depends on the geometry of observations, which is expressed by the phase angle á (the angle between the direction of the incident light and the line of sight of the detector, as seen from the dust particle), on the morphology and size distribution of the particles. P also depends on the light wavelength, λ, by the size parameter dependence (X = πd/λ, d is the diameter). It was first defined for spherical particles in the Mie theory. For irregular particles, an effective diameter is defined as the diameter of the sphere with an equivalent volume. The real and imaginary refractive indices n(λ) and k(λ), reflect the chemical composition of the materials. In Hadamcik et al. (2009a), the influence of k on scattered light polarization was tentatively interpreted through k(λ) values in the visible range taken from the literature with tholins other than those produced by the PAMPRE set-up.
Since Hadamcik et al. (2009a), new samples have been produced allowing the variations of the tholins’ properties to be characterized more precisely, as a function of the injected methane percentage (hereafter, CH4 ratio), such as the sizes and size distributions of the particles. Furthermore, the refractive indices in the 340–1000 nm range were measured on proper PAMPRE samples (Mahjoub et al., 2012), enabling the polarization results to be interpreted. The evolution of the chemical composition of the material according to the initial methane amount was studied by infrared absorption spectroscopy giving an insight into the change in albedo of the materials. Finally, the variation of the linear polarization, P, as a function of the different characteristics of tholins, is presented, and P is compared with the results obtained by the different space missions.
2. Production of Tholins by the PAMPRE Set-Up
Tholins are produced in the PAMPRE experiment, a CCP (Capacitively Coupled Plasma) radio frequency discharge at 13.6 MHz in a N2 and CH4 gas mixture, which is described in detail in Szopa et al. (2006) and Sciamma-O’Brien et al. (2010). The pressure is 0.9 hPa for all the experimental conditions presented here.
The discharge induces the formation of ions, atoms and radicals by the dissociation of methane CH4 and nitrogen N2 molecules by electronic collisions. These reactive species recombine, forming heavy gas species and tholins. The discharge can work in CWC (Continuous Working Conditions) for hours, or in a pulsed mode in order to produce tholins with a different reduced discharge duration.
3. Morphology and Size of the Dust Grains (SEM Analysis)
Hadamcik et al. (2009a) have presented a first study of the morphology of the grains obtained from SEM-FEG images. The grains are quasi-spherical. Their surface is not completely smooth. Some grains are broken and show radial structures corresponding to the surface irregularities, which fill up each grain suggesting that the grains grow radially. Some aggregates appear on the images, with just touching grains or with sintered ones. The aggregation may occur in the discharge or when the grains stick to the glass vessel or inside the microvials (Fig. 1). In the present paper, the word ‘grain’ is used for the individual grains (often called monomers in other papers) and the association of grains are referred to as particles or aggregates.
4. Refractive Indices Measurements
The light scattering experiments are performed at two wavelengths: green light at 543.5 nm (G) and red light at 632.8 nm (R) (see below Sections 6.1 and 6.6). The optical indices, n and k, of the various samples are therefore needed for these two wavelengths.
The chemical composition of tholins changes with the CH4 ratio, as shown by elemental analysis (Sciamma-O’Brien et al., 2010). This change can be a clue for understanding the evolution of the refractive indices with the CH4 ratio. Mid-infrared spectroscopy is therefore used to further characterize some molecular bands in the materials.
5. Mid-Infrared Absorption Spectroscopy
The intensity maxima of the aliphatic and the amine bands are seen to depend on the CH4 ratio. To further quantify these variations, the amine bands are directly considered, whereas the aliphatic bands are corrected from the amine contribution (Fig. 5(b)).
The absorption by particles in the visible wavelength range, represented numerically by the imaginary refractive index, is mainly due to the chemical composition. The structure of aggregates and the size of the constituent grains influence also the scattered light and its linear polarization.
6. Light Scattering on Lifted Particles
6.1 PROGRA2-vis instrument and experimental method
The particles in the field of view are aggregates (Hadamcik et al., 2009a). They are generated when the samples are lifted. They are inhomogeneous, made of small aggregates of sintered grains and of individual grains by contact.
The material in the aggregates is sparse. Their size is measured on the polarization maps. The size distribution of the lifted particles can be generally fitted by a Gaussian function. The average size is usually between 50 μm and 100 μm with particles between 20 μm and 1 mm. If the size distribution of the particles cannot be fitted by a Gaussian function, the polarization results are not considered.
First, P is determined for the whole sample, by integration of the polarized intensities on the whole set of particles and parameters of the phase curves are measured. P can also be studied as a function of the size of the particles in the 20–500 μm range. The image of the particles on the camera corresponds to the projection of the field section, with a sin(α) coefficient. Therefore, the spatial resolution of the particles’ images decreases when α decreases. For α ≤ 30°, it becomes impossible to measure the size distribution of the particles. For each size range, and phase angle, the polarized intensities are added and P calculated using Eq. (1). Phase curves are produced for each size range.
6.2 Polarization phase curves
6.3 Influence of the size of the grains on the negative branch
These results can be compared with space observations. From outside the atmosphere, the negative polarization on the phase curves is small, with an important scatter of the data (West et al., 1983). From DISR measurements, Tomasko et al. (2009) built a single-scattering polarization phase curve in green light, from a model of fractal cluster-cluster aggregates of 4300 grains with an elemental grain size of 80-nm-diameter mean size. They took into account the radiative transfer in the atmosphere. Pmin is about −2%, which is close to the values found with the experiment for grains with an average diameter smaller than 100 nm (Fig. 8(a)). The inversion angle α0 from the Pioneer 11 (Tomasko and Smith, 1982) and DISR/Huygens (Tomasko et al., 2009) seems to be smaller than 10?, which again indicates a grain diameter smaller than 90 nm (Fig. 8(b)). In order to achieve a more accurate comparison with observations, it is necessary to consider the maximum polarization.
6.4 Influence of the size of aggregates on the positive branch
6.5 Influence of the size of the grains on Pmax
Comparison between laboratory and space measurements (extrapolated to R = 632.8 nm and G = 543.5 nm). The average diameter of the grains in the aggregates is 75 nm. Values updated from Hadamcik et al. (2009a). Measurements for the small aggregates with 2% CH4.
Aggregates ≥ 20 μm
53 ± 2
38 ± 2
Aggregates ≤ 10 μm
54 ± 3
55 ± 3
Integrated from outside
Upward from inside (DISR)
6.6 Influence of the wavelength on Pmax
The positive polarization and its maximum Pmax change with a change of the incident wavelength (Figs. 9 and 11). For large aggregates, the positive polarization decreases when the wavelength increases. For aggregates with a diameter smaller than 10 μm, the opposite behavior occurs with an increase of the positive polarization.
The size parameter depends on d/λ: an increase of λ is equivalent to a decrease of the size. The refractive indices are also dependent on the wavelength (Section 4). These different parameters will be discussed to disentangle their respective influence. When λ decreases from 632.8 nm to 543.5 nm, it is equivalent to multiplying the sizes by about 1.16. When the size parameter of the large aggregates increases, Pmax increases (Fig. 10) by 1.5% on average for sizes in the 50–100 μm range. When the size parameter of the grains increases, Pmax decreases (Fig. 11), the variation is smaller for large grains (1.4% on average for grains with a 80-nm diameter to 1.1% for grains with a 400-nm diameter). As a consequence, Pmax increases slightly, or is constant, when the wavelength decreases for large aggregates. For small aggregates (micrometer sized), numerical simulations suggest an increase of Pmax when the aggregate and constituent grain sizes decrease, if n and k are in the range found for tholins (Petrova et al., 2004). As a consequence, the decrease of the size parameter from green to red can explain the increase of positive polarization for aggregates smaller than 10 μm with the increase of wavelength. This behavior is different for larger aggregates (Fig. 9).
The polarization depends also on the refractive indices. When λ decreases, n(λ) and k(λ) increases. Numerical models are limited in the size of the particles to equivalent diameters of some micrometers: they are used in the present paper to give trends. When n(λ) increases from 1.5 to 1.9, Pmax decreases for aggregates with an equivalent diameter smaller than about 10 μm (Petrova et al., 2004) and a constant absorption k. For a constant value of n (λ), when k (λ) increases, Pmax increases. Zubko et al. (2009) aggregates’ size parameter is in the 5 to 30 range (equivalent particle size in the 1 to 6 μm range), they consider the variation of Pmax as a function of ‘k’ with a fixed n at 1.5. For k ≤ 0.05, corresponding to tholins, the increase of Pmax with increasing k is very important for the largest aggregates. In that case, Pmax (543.5) is higher than Pmax (632.8), as observed for the tholins for large aggregates, but it keeps the same value or slightly decreases for the smallest ones. The variation of Pmax seems to be dominated by the absorption for the large aggregates.
Internal interactions depolarize the light, as is well observed for transparent particles with small k(λ) values (Hadamcik et al., 2009c); it is also found in numerical simulations on small aggregates (Kimura et al., 2003; Petrova et al., 2004). As the size of the aggregate increases, more light is absorbed. For sufficiently large relatively absorbing particles, the emergent light is mainly scattered by the external grains and the polarization has a maximum value due to the absence of depolarization by multiple scattering, e.g. in green light (Hadamcik et al., 2009a).
Similar conclusions can be deduced for the grains’ size from the PROGRA2 experiment and from the space observations (Tomasko et al., 2009). The polarization values obtained for the green light is about the same for large and small aggregates. They are similar when measured from outside the atmosphere by integrating the fluxes (mainly sensitive to particles in the upper atmosphere) and from inside the atmosphere by the DISR/Huygens experiment looking upward (Table 1). In red light, the maximum polarization values are smaller for large aggregates than for small ones (more internal interactions due to the smaller absorption). Similarly, the external observations of Titan’s atmosphere from Pioneer 11 and Voyager 2 space probes give smaller values because of multiple scattering in the atmosphere, compared with measurements carried out inside the atmosphere looking upward by the DISR, when extrapolated to the wavelength used in the experiment. The integration over the whole atmosphere increases the depolarization by multiple scattering for larger wavelengths (Hadamcik et al., 2009a).
The influence of the wavelength on the maximum polarization is an important factor to consider for a comparison with space observations. However, the quantitative effect on Pmax is small as compared with the grain size influence (Fig. 11).
6.7 Conclusion on the influence of the CH4 ratio
The minimum polarization, Pmin, the maximum polarization, Pmax, and the inversion angle, α0, for the different samples have been found to mainly depend on the size of the constituent grains. However, the samples produced with various methane ratios show different average grain sizes (Fig. 3).
7. Summary and Conclusion
Tholins optical properties have been studied emphasizing their variation as a function of the CH4/N2 ratio with the PAMPRE set-up. SEM analysis has enabled the constituent grain-size distribution to be measured for each sample. A minimum size is obtained for CH4/N2 ratios between 4% and 5%. The linear polarization phase curves are dominated by the variation in the size of the constituent grains. An anti-correlation is observed between the grain-size variation and the maximum polarization, Pmax. The negative branch is also dependent on the CH4/N2 ratio by the grain-size dependence. An initial investigation has been conducted and future investigations are needed for low phase angles because of the critical signal-to-noise ratio values in this region. Pmin, α0 and Pmax values for grain sizes smaller than, or equal to, 90-nm diameters are similar to those found by the different space missions (when the values are extrapolated to the same wavelengths). The large aggregates values correspond to values integrated over the whole satellite atmosphere, as measured by Pioneer 11 and Voyager 2, and the values observed by DISR/Huygens looking upward to values obtained for aggregates in the micrometer-size range.
EH would like to thank H. Kimura and the CPS for organizing the Cosmic Dust workshop and for their help, allowing her to participate. The authors thank S. Borensztajn (Univ. Paris-Sorbonne, UPR 15) for the SEM-FEG images. CNES is acknowledged for funding the PROGRA2 experiment. Financial support for A. M. post-doc (ANR-09-JCJC-0038 contract).
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