# Laboratory Simulations of Haze Formation in the Atmospheres of Super-Earths and Mini-Neptunes: Particle Color and Size Distribution

Chao He, Sarah M. Hörst, Nikole K. Lewis, Xinting Yu, Julianne I. Moses, Eliza M. -R. Kempton, Patricia Mcguiggan, Caroline V. Morley, Jeff A. Valenti, Véronique Vuitton

► To cite this version:

Chao He, Sarah M. Hörst, Nikole K. Lewis, Xinting Yu, Julianne I. Moses, et al., Laboratory Simulations of Haze Formation in the Atmospheres of Super-Earths and Mini-Neptunes: Particle Color and Size Distribution. The Astrophysical Journal Letters, 2018, 856, 10.3847/2041-8213/aab42b. insu-03693573

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# Laboratory Simulations of Haze Formation in the Atmospheres of Super-Earths and Mini-Neptunes: Particle Color and Size Distribution

Chao He¹, Sarah M. Hörst¹, Nikole K. Lewis¹,², Xinting Yu¹, Julianne I. Moses³, Eliza M.-R. Kempton⁴, Patricia McGuiggan⁵, Caroline V. Morley⁶, Jeff A. Valenti², and Véronique Vuitton⁷

¹Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD, USA; che13@jhu.edu

²Space Telescope Science Institute, Baltimore, MD, USA

³Space Science Institute, Boulder, CO, USA

⁴Grinnell College, Grinnell, IA, USA

⁵Department of Materials Science and Engineering, Johns Hopkins University, Baltimore, MD, USA

⁶Harvard University, Cambridge, MA, USA

⁷Univ. Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

Received 2017 November 27; revised 2018 March 1; accepted 2018 March 3; published 2018 March 19

## Abstract

Super-Earths and mini-Neptunes are the most abundant types of planets among the ~3500 confirmed exoplanets, and are expected to exhibit a wide variety of atmospheric compositions. Recent transmission spectra of super-Earths and mini-Neptunes have demonstrated the possibility that exoplanets have haze/cloud layers at high altitudes in their atmospheres. However, the compositions, size distributions, and optical properties of these particles in exoplanet atmospheres are poorly understood. Here, we present the results of experimental laboratory investigations of photochemical haze formation within a range of planetary atmospheric conditions, as well as observations of the color and size of produced haze particles. We find that atmospheric temperature and metallicity strongly affect particle color and size, thus altering the particles' optical properties (e.g., absorptivity, scattering, etc.); on a larger scale, this affects the atmospheric and surface temperature of the exoplanets, and their potential habitability. Our results provide constraints on haze formation and particle properties that can serve as critical inputs for exoplanet atmosphere modeling, and guide future observations of super-Earths and mini-Neptunes with the *Transiting Exoplanet Survey Satellite*, the *James Webb Space Telescope*, and the *Wide-Field Infrared Survey Telescope*.

**Key words:** planets and satellites: atmospheres

## 1. Introduction

The *Kepler* mission has shown that among the ~3500 confirmed exoplanets, the most numerous types of planets are super-Earths ($1.25 R_{\text{Earth}} < R_{\text{p}} < 2.0 R_{\text{Earth}}$) and mini-Neptunes ($2.0 R_{\text{Earth}} < R_{\text{p}} < 4.0 R_{\text{Earth}}$) (e.g., Borucki et al. 2011; Fressin et al. 2013). The *Transiting Exoplanet Survey Satellite (TESS)* mission will further increase the number of super-Earths and mini-Neptunes, including a sample of rocky worlds in the habitable zones of their host stars. These types of exoplanets are expected to exhibit a wide variety of atmospheric compositions (e.g., Elkins-Tanton & Seager 2008; Miller-Ricci et al. 2009; Schaefer et al. 2012; Moses et al. 2013; Hu & Seager 2014; Ito et al. 2015; Venot et al. 2015), and *TESS* will seek out targets for atmospheric characterization by the *James Webb Space Telescope (JWST)*, as well as other large ground-based and space-based telescopes in the future. Clouds and hazes are likely to be present in exoplanet atmospheres, as they are ubiquitous in the atmospheres of solar system worlds. Recent transmission spectra have demonstrated that clouds and/or hazes could play a significant role in atmospheres of Neptune-sized GJ 436b (Knutson et al. 2014a), and super-Earth/mini-Neptune-sized planets GJ 1214b (Kreidberg et al. 2014) and HD 97658b (Knutson et al. 2014b). Condensate cloud and photochemical haze particles affect the chemistry, dynamics, and radiation flux in planetary atmospheres, and can therefore influence surface temperature and habitability. However, little is known about the composition, size distributions, and optical properties of the particles that may form in exoplanet atmospheres, which largely exist outside the size and temperature regimes of solar system

planets. Laboratory studies of exoplanet haze particles are essential to interpreting future spectroscopic observations and characterizing the atmospheres of these worlds. We have reported the formation of hazes in laboratory simulations of the atmospheres expected for super-Earths and mini-Neptunes (Hörst et al. 2018), and here we present the haze colors and the particle sizes measured with atomic force microscopy (AFM). Besides dramatically different production rates and haze colors, the AFM images show that the particle size varies with initial gas composition.

Particle size affects the scattering and absorption of light, and thus impacts the temperature structure of exoplanet atmospheres, as well as their observed spectra. Remote and in situ measurements have provided useful information on particle sizes in planetary atmospheres of solar system bodies; for example, the *Cassini–Huygens and New Horizons* missions have put important constraints on the haze particle sizes of Titan and Pluto (Tomasko et al. 2005, 2008; Gladstone et al. 2016). However, very little is known about particle sizes in exoplanet atmospheres. Laboratory study of exoplanet haze analogs could place some constraints on the particle sizes. Such studies of Titan haze analogs (tholins) have helped explain the size and growth of the haze particles in Titan's atmosphere. The particle sizes of Titan tholins prepared in laboratories have been measured through several different techniques, including scanning mobility particle sizer (see, e.g., Trainer et al. 2006; Hörst & Tolbert 2013, 2014), scanning electron microscopy (SEM, see e.g., Szopa et al. 2006; Carrasco et al. 2009; Hadamcik et al. 2009; Sciamma-O'Brien et al. 2017),
<figure><img src="image_3.png" /><figcaption>**Figure 1.** Schematic of the experimental setup used for this work. Gas mixtures for each experiment excluding water vapor (and ammonia for the 300 K-100× metallicity experiment) are prepared in respective ratios as listed in Table 1 and mix overnight in the mixing cylinder. Water vapor (and ammonia for the 300 K-100× metallicity experiment) is supplied by water (or ammonia water solution) at the desired temperature maintained by a dry ice/methanol/water cold bath. The prepared gas mixture and water vapor (and ammonia for the 300 K-100× metallicity experiment) flow through a heating coil, where the gases are heated to the experimental temperature, and into the reaction chamber, where they are exposed to an AC glow discharge, initiating chemical processes that lead to the formation of new gas-phase products and particles.</figcaption></figure>

transmission electron microscopy (TEM, see e.g., Trainer et al. 2006; Curtis et al. 2008; Quirico et al. 2008), and AFM (Li et al. 2010; Hasenkopf et al. 2011). SEM and TEM usually require a conductive coating on the sample and could also cause thermal damage to the sample. We use AFM in this study because it can image the original sample surface without coating an additional layer or exposing the sample to electron radiation.

## 2. Materials and Experimental Methods

### 2.1. Haze Production Setup

Figure 1 shows a schematic of the Planetary Haze Research (PHAZER) experimental setup at Johns Hopkins University (He et al. 2017; Hörst et al. 2018). The initial gas mixtures for our experiments are calculated from the chemical-equilibrium models of Moses et al. (2013), who examined the possible thermochemistry and photochemistry in the atmospheres of Neptune-sized and sub-Neptune-sized exoplanets. Most of the known super-Earth and mini-Neptune size planets known to date were discovered by the *Kepler* mission (Borucki et al. 2011; Fressin et al. 2013). However, follow-up of *Kepler* targets to determine planetary mass and atmospheric characterization has been limited due to the brightness of their host stars. The *TESS* mission (Ricker et al. 2014) will target stars that are 10–100 times brighter than those targeted with the *Kepler* mission and yield a large sample of super-Earth and mini-Neptune class planets with equilibrium temperatures ($T_{eq}$) < 1000 K (Sullivan et al. 2015). This planetary size ($R_p$ < 4 $R_{Earth}$) and temperature ($T_{eq}$ < 1000 K) phase space has been recently explored by exoplanet atmospheric characterization efforts for a handful of planets such as GJ 1214b, HD 97658b, GJ 436b, and GJ 3470b, which all indicate that aerosols are shaping the planetary spectrum (e.g., Knutson et al. 2014a, 2014b; Kreidberg et al. 2014; Dragomir et al. 2015). Theoretical studies predict a diverse range of possibilities for the composition of atmospheric envelopes of mini-Neptunes and super-Earths (e.g., Fortney et al. 2013; Howe & Burrows 2015; Wolfgang & Lopez 2015). Broadly speaking, we expect that our hydrogen-rich gas mixtures are more relevant to larger mini-Neptune class planets and carbon dioxide-rich gas mixtures are more relevant to smaller super-Earth class planets, with water-rich gas mixtures being relevant to both classes

<table><caption>**Table 1**
Initial Gas Mixtures Used in the Experiments</caption><thead><tr><th></th><th>100×</th><th>1000×</th><th>10,000×</th></tr></thead><tbody><tr><td rowspan="6">600 K</td><td>72.0% H<sub>2</sub></td><td>42.0% H<sub>2</sub></td><td>66.0% CO<sub>2</sub></td></tr><tr><td>6.3% H<sub>2</sub>O</td><td>20.0% CO<sub>2</sub></td><td>12.0% N<sub>2</sub></td></tr><tr><td>3.4% CH<sub>4</sub></td><td>16.0% H<sub>2</sub>O</td><td>8.6% H<sub>2</sub></td></tr><tr><td>18.3% He</td><td>5.1% N<sub>2</sub></td><td>5.9% H<sub>2</sub>O</td></tr><tr><td></td><td>1.9% CO</td><td>3.4% CO</td></tr><tr><td></td><td>1.7% CH<sub>4</sub></td><td>4.1% He</td></tr><tr><td></td><td>13.3% He</td><td></td></tr><tr><td rowspan="4">400 K</td><td>70.0% H<sub>2</sub></td><td>56.0% H<sub>2</sub>O</td><td>67.0% CO<sub>2</sub></td></tr><tr><td>8.3% H<sub>2</sub>O</td><td>11.0% CH<sub>4</sub></td><td>15.0% H<sub>2</sub>O</td></tr><tr><td>4.5% CH<sub>4</sub></td><td>10.0% CO<sub>2</sub></td><td>13.0% N<sub>2</sub></td></tr><tr><td>17.2% He</td><td>6.4% N<sub>2</sub></td><td>5.0% He</td></tr><tr><td></td><td>1.9% H<sub>2</sub></td><td></td></tr><tr><td></td><td>14.7% He</td><td></td></tr><tr><td rowspan="5">300 K</td><td>68.6% H<sub>2</sub></td><td>66.0% H<sub>2</sub>O</td><td>67.3% CO<sub>2</sub></td></tr><tr><td>8.4% H<sub>2</sub>O</td><td>6.6% CH<sub>4</sub></td><td>15.6% H<sub>2</sub>O</td></tr><tr><td>4.5% CH<sub>4</sub></td><td>6.5% N<sub>2</sub></td><td>13.0% N<sub>2</sub></td></tr><tr><td>1.2% NH<sub>3</sub></td><td>4.9% CO<sub>2</sub></td><td>4.1% He</td></tr><tr><td>17.3% He</td><td>16.0% He</td><td></td></tr></tbody></table>

**Note.** Our experimental phase space spans 100–10,000× solar metallicity and temperatures ranging from 300 to 600 K.

of planets. However, further observational, theoretical, and laboratory work will be required to confirm or refute the potential diversity in atmospheric compositions for these classes of planets that do not exist in our solar system. The equilibrium calculations relevant to this investigation were performed at conditions of 300, 400, and 600 K at 1 mbar for 100×, 1000×, and 10,000× solar metallicity. Smaller planets are less efficient at accreting the H- and He-rich gas from the protoplanetary disk, and the lighter elements have a greater chance of escaping from smaller planets, which enhances the overall metallicity of planets that are Neptune-sized and smaller. As an example, the O/H metallicity on Uranus and Neptune is estimated to be <160 and 540 times solar, respectively (Cavalié et al. 2017). Various evolutionary processes could drive the relative abundances of the heavy elements away from solar, but these high-metallicity chemical-equilibrium models provide a reasonable starting point for our study. As listed in Table 1, we included gases with a calculated
abundance of 1% or higher to maintain a manageable level of experimental complexity; this resulted in no nitrogen-bearing species in two cases and the exclusion of sulfur-bearing species. Sulfur-bearing species, like H₂S, could be important for haze formation (Gao et al. 2017) and will be an avenue of future work. The pressure, temperature, and gas compositions used in the experiments are self-consistent based on the model calculations.

Gas mixtures for each experiment, excluding water vapor (and ammonia for the 300 K-100× metallicity experiment), were prepared in the ratios as listed in Table 1, respectively, and mixed overnight in the mixing cylinder. High-purity gases purchased from Airgas were used to prepare the mixture (H₂-99.9999%, He-99.9995%, N₂-99.9997%, CH₄-99.999%, CO₂-99.999%, CO-99.99%). A liquid nitrogen cold trap was used to remove known contaminants from CO before mixing it with the other gases (see e.g., Hörst & Tolbert 2014; He et al. 2017). The total flow rate is 10 standard cubic centimeters per minute (sccm), thus we flow the gas mixture (without water and ammonia) at a proportional rate of 10 sccm based on the ratio in Table 1, and measure the pressure (P₁) at the same time. The pressure (P₂) of water vapor is then calculated (P₂/P₁ = the mixing ratio of water to other gases as in Table 1). For instance, in the 600 K-100× metallicity experiment, P₁ is 4.90 Torr when the flow rate of the gas mixture is 9.37 sccm, thus P₂ is calculated to be 0.33 Torr. The gas mixture is controlled by a mass flow controller (MKS Instrument, GM50A) and water vapor is supplied by HPLC water (Fisher Chemical) at a desired temperature maintained by a dry ice/methanol/water cold bath. The temperature of the cold bath is adjusted by varying the methanol/water ratio. For the 300 K-100× metallicity experiment, a 0.5 wt% ammonia water solution (prepared with HPLC water and 28% NH₃ in H₂O, EMD) at 246 K provides water and ammonia vapor (Field & Combs 2002). The prepared gas mixture and water vapor (and ammonia for the 300 K-100× metallicity experiment) flow through a 15 m stainless-steel heating coil where the gases are heated to the experimental temperature (600 K, 400 K, or 300 K), and then into a stainless-steel reaction chamber where they are exposed to an AC glow discharge, initiating chemical processes that lead to the formation of new gas-phase products and solid particles. The plasma produced by the AC glow discharge is not analogous to any specific process in planetary upper atmospheres; we use it as a proxy for energetic processes occurring in planetary upper atmospheres, because it is sufficiently energetic to directly dissociate very stable molecules such as N₂ or CO. AC glow discharge, as a cold plasma source, does not alter the neutral gas temperature significantly, and is often used as an analog for the relatively energetic environment of planetary upper atmospheres (Cable et al. 2012). During 72 hr of discharge flow, produced solid particles (tholin) are deposited on the wall of the reaction chamber and quartz substrate disks (purchased from Ted Pella, Inc., and made from high-quality fused quartz and optical-grade clear polished on both sides) at the bottom of the chamber. We ran our previous Titan experiments for 72 hr to get sufficient samples (He et al. 2017), thus we followed the same procedure here for comparison. The chamber is further kept under vacuum for 48 hr to remove the volatile components, and then transferred to a dry (<0.1 ppm H₂O), oxygen free (<0.1 ppm O₂) N₂ glove box (Inert Technology Inc., I-lab 2GB) where the tholin films on quartz disks and tholin powders from the wall

are collected under the dry N₂ atmosphere. Both the powders and films are kept in the glove box and wrapped in foil to avoid exposure to air and light, respectively.

## 2.2. AFM Measurement

The surface morphology of the tholin films is examined using a Bruker Dimension 3100 atomic force microscope (Bruker Nano, Santa Barbara, CA). A silicon probe (Tap300-G, Ted Pella, Inc.) is used, its tip radius is less than 10 nm, and the conical angle at the apex is less than 20°. The AFM images are acquired by scanning the sample under ambient laboratory conditions (298 K) at a scan rate of 1.5 Hz using the tapping mode.

# 3. Results and Discussion

## 3.1. Tholin Films and Production Rate

Figure 2 shows pictures of the tholin films deposited on quartz disks (1" diameter) in visible light. The color of the films varies significantly as a function of metallicity and temperature. For comparison, we include the picture of a Titan tholin film on a quartz disk from our standard Titan experiment (5% CH₄ in 95% N₂) using an identical setup (He et al. 2017). The production rates of the haze particles produced from the nine experiments (Hörst et al. 2018) and our previous Titan experiment (He et al. 2017) are also included in Figure 2. Among the nine films in Figure 2, those from the 1000× metallicity at 400 and 300 K experiments are dark gold, and the one at 300 K is slightly lighter than that, at 400 K. The colors of those two films look very similar to those of our standard Titan experiment. As we reported previously (Hörst et al. 2018), the production rate of these two cases is also compatible with our standard Titan experiment (~10 mg hr⁻¹ versus 7.4 mg hr⁻¹). The production rate and color may suggest similarities in the chemical processes leading to the particle formation and the resulting compositions, so further work is needed to understand the complex chemical systems.

For 100× metallicity, the film from the 600 K experiment is olive green, while the one from 400 K looks chocolate brown. In these two cases, the production rate is relatively low (0.04 and 0.25 mg hr⁻¹, Hörst et al. 2018), thus the relatively dark films are probably derived from dark-colored particles rather than thick films. Two distinct colors suggest a compositional difference for the two films. Considering the similarity of the gas mixtures in these two cases, the temperature (600 K versus 400 K) could play an important role in the atmospheric chemistry that leads to the different compositions of the hazes. The films from 100× metallicity at 300 K, 1000× metallicity at 600 K, and 10,000× metallicity at 600 K experiments are all light yellow in color, consistent with the low production rate in these cases (Hörst et al. 2018). Both films from 10,000× metallicity at 400 and 300 K show no obvious difference with the clear blank quartz disk, suggesting very few particles deposited on the substrate in these two cases.

The films shown in Figure 2 demonstrate large variations in particle color at different temperatures for varying metallicity. The haze particles in different colors will absorb and scatter visible light differently, and thus affect the thermal structure of the exoplanet atmospheres and the potential habitability. To better understand these effects, optical constant measurements (at a wide range of wavelengths) of these analog materials are underway.
<figure><img src="image_4.png" /><figcaption>**Figure 2.** Pictures of the tholin films deposited on quartz disks [diameter: 1"(2.54 cm)]. The image labeled “Blank” is a picture of a clean blank quartz disk, and “Titan tholin” is a picture of the Titan tholin film on a quartz disk from our standard Titan experiment (5% CH₄ in 95% N₂). The average red, green, and blue (RGB) colors of the pictures are shown in the brackets under the pictures. The production rates (mg h⁻¹), of the haze particles produced from the nine experiments (Hörst et al. 2018) and our previous Titan experiment (He et al. 2017) are shown under the pictures in red. N/A indicates that the solid sample was not enough to collect and weigh.</figcaption></figure>

## 3.2. AFM Images of the Tholin Films and the Particle Size Distribution

Figure 3 shows AFM three-dimensional (3D) images of the tholin films deposited on quartz disks, displaying a 1 µm × 1 µm scanning area for each film. An AFM image of a clean blank quartz disk is also included in Figure 3, showing a smooth, clean surface. Compared to the clear blank disk, we

observe obvious spherical particles on the disks from nine experiments, confirming that haze particles are produced in all nine diverse atmospheres. This is particularly important for the 10,000× metallicity at 400 and 300 K experiments, because it is difficult to determine whether or not haze particles are formed by visual examination of these disks (Figure 2). Figure 3 shows that the particles sparsely spread on these two disks, indicating the relatively low production rate in these two
<figure><img src="image_5.png" /><figcaption>**Figure 3.** AFM 3D images of the tholin films deposited on quartz disks. The scan area is 1 µm × 1 µm. “Blank” is the AFM image of a clean blank quartz disk, and “Titan tholin” is the AFM image of the Titan tholin film on a quartz disk from our standard Titan experiment (5% CH₄ in 95% N₂). The height scale of the images is 30 nm, as shown in the blank disk, except the one for the 400 K, 10,000× metallicity experiment, which has an 80 nm height scale to better show the large particles. The root mean square (rms) roughness (Rq) of the film (1 µm × 1 µm) is shown under the images. The roughness (<5 nm) indicates that the films are smooth. The mean diameters (Dmean, nm) of the haze particles are also shown under the images (in red).</figcaption></figure>

cases. In contrast to these two cases, there are more particles produced for the 10,000× metallicity at 600 K experiment, consistent with the measured production rates (Hörst et al. 2018). The formation of hazes in the absence of methane suggests other carbon sources for the organics, such as CO and CO₂. The dissociation of CO or CO₂ produces atomic carbon, which can be used to build organic molecules. Previous studies

have shown that reactions (irradiated by UV or plasma) beginning with the gas mixture of CO/N₂/H₂O or CO₂/N₂/H₂O produce a variety of organic compounds (see, e.g., Bar-Nun & Chang 1983; Plankensteiner et al. 2004; Cleaves et al. 2008). This result here demonstrates that there are multiple pathways for organic haze formation and that CH₄ is not necessarily required.
<figure><img src="image_6.png" /><figcaption>**Figure 4.** Size distribution of the tholin particles formed in the nine experiments. The haze particles are more uniform for the 100× metallicity experiments (20–55 nm), while the particle sizes for the 1000× and 10,000× metallicity experiments have wider distributions (25–180 nm).</figcaption></figure>

We measured the diameter based on the particle’s projection on the x–y plane. This method gives an accurate result (measurement errors are less than 3 nm) in the size range we measured (Villarrubia 1997; Klapetek et al. 2011). The AFM image of the Titan tholin film in Figure 3 shows that numerous small particles (diameter 30–100 nm) are densely deposited on the quartz disk. Similarly, there are a large number of particles closely packed on the disks for the 100× and 1000× metallicity experiments at all three temperatures (Figure 3). The particles are of different sizes for different cases. The number of particles is consistent with a higher production rate in these cases. For the 100× metallicity cases, small particles (diameter 20–55 nm) are against each other tightly, while the particle sizes have wider distributions (25–130 nm) for the 1000× metallicity cases. It is noteworthy that the particles appear to array into linear structures for 1000× metallicity at 400 and 300 K, while these two cases have highest production rate (~10 mg hr⁻¹, Hörst et al. 2018). In these two cases, a great many particles are produced and deposited on the quartz disks in multiple layers. The AFM images only display the top layer of the particles. During the reactions, the particle interactions are governed by interparticle forces, such as van der Waals, hydrogen bonds, and weak polar forces. This may lead to the newly deposited particles forming the linear structures as in Figure 3, which could be similar to the self-assembly of nanoparticle chains of organic polymers due to hydrogen bonding (see e.g., Grzelczak et al. 2010; Kao et al. 2012). The size ranges of the haze particles in these two cases (30–90 nm in diameter) are also similar to the size range of the Titan tholin (25–80 nm). However, the linear structures are not observed on the Titan tholin film from our standard Titan experiment (Figure 3), which has a comparable production rate. Since water (present in the 1000× metallicity 300 and 400 K experiments at 66% and 56%, respectively) is a polar molecule, it could contribute to the interparticle forces that caused the formation of the linear structures.

The AFM images (Figure 3) show that the particle size varies from 20 to 180 nm. In order to better reveal the size distribution of the haze particles, we analyzed the particle size in a larger

scanning area (10 µm × 10 µm) of each film, and plotted the percentage of particles (N/N$_{total}$ × 100%) in 1 nm bins (Figure 4). The haze particles are the most uniform in size for the 100× metallicity experiments; the particles formed at 600 K are between 20 and 40 nm in diameter, those at 400 K are between 30 and 55 nm, and those at 300 K vary from 25 to 55 nm. The particles from the 1000× metallicity experiments have wider size distributions; the particles at 600 K are between 25 and 130 nm, those at 400 K are from 40 to 90 nm, and those at 300 K are from 30 to 85 nm. For the 1000× metallicity experiment at 600 K, the production rate is low (0.15 mg hr⁻¹, Hörst et al. 2018), thus there are few nucleation centers in the system and the particle growth rates are slow. However, gas-solid heterogeneous reactions could happen on the particle surfaces and lead to the formation of a wider range of particles. In the two high-production-rate cases (400 and 300 K), the bigger particles could have formed via small particle aggregation. The two high-production-rate cases produce sufficient numbers of small particles and they may grow into fractal aggregates, such as those observed in the detached haze layer in Titan’s atmosphere (see, e.g., Lavvas et al. 2009; Cours et al. 2011). The aggregates in the detached haze layer have an effective diameter around 300 nm, and are probably formed from 80 nm (diameter) monomers (Lavvas et al. 2009; Cours et al. 2011). If similar processes happened in our two high-production-rate cases, both the monomers (~30 nm in diameter) and the aggregates (~90 nm) would be smaller than those in Titan’s detached haze layer. For the 10,000× metallicity experiments, the particles at 600 K are smaller and more uniform in size (30–80 nm) compared to those at 400 and 300 K (50–180 nm). For those at 400 and 300 K, the broader range of particle sizes could be caused by the low production rate, similar to the 1000× metallicity experiment at 600 K. In these cases, few nucleation centers and heterogeneous reactions lead to the formation of more diverse particles. In Figure 4, several particle size distributions (the 1000× metallicity experiments at three temperatures, and the 10,000× metallicity experiments at 400 K) appear to have a bimodal distribution. As we discussed above, the bimodal
distribution could be caused by small particle aggregation for the high-production-rate cases (the 1000× metallicity experiments at 400 and 300 K), or by heterogeneous reactions with few nucleation centers for the low-production-rate cases (the 1000× metallicity experiment at 600 K and the 10,000× metallicity experiment at 400 K). Both the AFM images and the size distribution indicate that most of the particles are monomers, except for a few aggregates for the higher-production-rate cases (1000× metallicity experiments).

Studies show that the particle size of Titan haze analogs varies with the initial gas composition (Hadamcik et al. 2009; Hörst & Tolbert 2014; Sciamma-O’Brien et al. 2017). Our experimental matrix varied in temperature and metallicity and all nine initial gas mixtures are compositionally distinct, which may cause the differences in particle size. Future investigations are required to fully understand how the gas compositions affect the particle size. Particle size affects the interaction of haze particles with radiation, such as scattering and absorption, and thus impacts the energy budget and the temperature structure of exoplanet atmospheres. For all nine exoplanet atmospheric scenarios investigated here, the size ranges of the particles (20–180 nm) lie in the Rayleigh scattering regime for visible and infrared (IR) photons. In this regime, the small particles will scatter short wavelengths more efficiently. The existence of haze particles would drastically change the geometric albedo of the exoplanet in visible and near-IR regions (0.4–1.0 µm) (McCullough et al. 2014; Morley et al. 2015; Sing et al. 2016; Gao et al. 2017), which could affect the detectability of directly imaged exoplanets by the Coronagraph Instrument on the Wide-Field Infrared Survey Telescope (WFIRST; Spergel et al. 2015). The haze particles have different absorption features at different wavelengths, depending on their composition. Thus, these features are helpful for identifying the composition of the haze particles. However, these features could also reduce the detectability of atmospheric chemical species. To fully understand the effect of the haze particles on observations, their optical and compositional properties are required. These measurements of the analog materials are underway.

Currently, wide ranges of particle sizes, from 5 to 10,000 nm, are used in exoplanet atmospheric models (see, e.g., Howe & Burrows 2012; Arney et al. 2016; Gao et al. 2017). However, it is difficult to constrain particle sizes by modeling. For instance, a variety of models is used to reproduce the featureless transit spectrum of GJ 1214b, where we see strong evidence for aerosols, but the results from different models are not consistent in the particle sizes. Morley et al. (2015) showed that photochemical hazes with a range of particle sizes (10–300 nm) can create featureless transmission spectra, while Charnay et al. (2015) found that the predicted transit spectrum matches with observations when particle radii are around 500 nm. The particles (20–180 nm) formed in our experiments fall within the size range discussed by Morley et al. (2015), suggesting that small particles are more likely in the atmosphere of GJ 1214b.

Our result shows that the haze particles are more uniform for the 100× metallicity experiments (20–55 nm), while the particle sizes for the 1000× and 10,000× metallicity experiments have wider distributions (25–180 nm). Laboratory experimental simulations cannot perfectly replicate photochemical processes that occur in exoplanet atmospheres, thus the

size ranges we measured may not represent the actual haze particle sizes in exoplanet atmospheres. However, laboratory studies can provide insights into the size and growth of the haze particles in planetary atmospheres; for instance, the size of Titan tholin monomers is consistent with that of the actual haze monomers observed in Titan's atmosphere (Tomasko et al. 2005, 2008; Trainer et al. 2006; Hörst & Tolbert 2013), and the tholin aggregates also match those observed in the detached haze layer in Titan's atmosphere (see, e.g., Tomasko et al. 2008; Hadamcik et al. 2009; Cours et al. 2011). We measured the particle sizes for both monomers and aggregates (only a few for the higher-production-rate cases, the 1000× metallicity experiments). The size distribution can be used as a guide for modeling super-Earth and mini-Neptune atmospheres with haze layers, and the size difference for different metallicities and temperatures should be considered. The size distribution of the haze particles, along with the production rate (Hörst et al. 2018), provides critical inputs for modeling the atmospheres of exoplanets, and useful data for interpreting and guiding current and future observations of super-Earths and mini-Neptunes. Further optical constant measurements and compositional analyses of these haze particles are in progress, and will guide future observations of super-Earths and mini-Neptunes atmospheres.

## 4. Conclusions

We conducted a series of laboratory experimental simulations to investigate haze formation in a range of planetary atmospheres using the PHAZER chamber (He et al. 2017), and found that haze particles are formed in all nine experiments, but the haze production rates are dramatically different for different cases (Hörst et al. 2018). We examined the colors and particle sizes of the tholin films deposited on quartz disks. The results demonstrate large variation in particle color at different temperatures for different metallicities. The AFM images reveal that the particle size varies from 20 to 180 nm. The haze particles are more uniform for the 100× solar metallicity experiments (20–55 nm), while the particle sizes for the 1000× and 10,000× solar metallicity experiments have wider distributions (25–180 nm). The formation of haze particles in different colors and sizes will have an impact on light absorption and scattering, thus influencing the atmospheric and surface temperature of the exoplanets and their potential habitability. The size distribution of the haze particles measured here, along with the production rate (Hörst et al. 2018), fills critical gaps in our ability to model exoplanet atmospheres and provides useful laboratory data for interpreting and guiding current and future observations of super-Earths and mini-Neptunes, especially for TESS, JWST, and WFIRST.

This work was supported by the NASA Exoplanets Research Program Grant NNX16AB45G. C.H. was supported by the Morton K. and Jane Blaustein Foundation.

## ORCID iDs

Chao He https://orcid.org/0000-0002-6694-0965
Sarah M. Hörst https://orcid.org/0000-0003-4596-0702
Nikole K. Lewis https://orcid.org/0000-0002-8507-1304
Julianne I. Moses https://orcid.org/0000-0002-8837-0035
Caroline V. Morley https://orcid.org/0000-0002-4404-0456
Véronique Vuitton https://orcid.org/0000-0001-7273-1898
References

Arney, G., Domagal-Goldman, S. D., Meadows, V. S., et al. 2016, AsBio, 16, 873

Bar-Nun, A., & Chang, S. 1983, JGRC, 88, 6662

Borucki, W. J., Koch, D. G., Basri, G., et al. 2011, ApJ, 736, 19

Cable, M. L., Hörst, S. M., Hodyss, R., et al. 2012, ChRv, 112, 1882

Carrasco, N., Schmitz-Afonso, I., Bonnet, J.-Y., et al. 2009, JPCA, 113, 11195

Cavalié, T., Venot, O., Selsis, F., et al. 2017, Icar, 291, 1

Charnay, B., Meadows, V., Leconte, J., & Misra, A. 2015, ApJL, 813, L1

Cleaves, H. J., Chalmers, J. H., Lazcano, A., Miller, S. L., & Bada, J. L. 2008, OLEB, 38, 105

Cours, T., Burgalat, J., Rannou, P., et al. 2011, ApJL, 741, L32

Curtis, D. B., Hatch, C. D., Hasenkopf, C. A., et al. 2008, Icar, 195, 792

Dragomir, D., Benneke, B., Pearson, K. A., et al. 2015, ApJ, 814, 102

Elkins-Tanton, L. T., & Seager, S. 2008, ApJ, 685, 1237

Field, P. E., & Combs, R. J. 2002, J. Solution Chem., 31, 719

Fortney, J. J., Mordasini, C., Nettelmann, N., et al. 2013, ApJ, 775, 80

Fressin, F., Torres, G., Charbonneau, D., et al. 2013, ApJ, 766, 81

Gao, P., Marley, M. S., Zahnle, K., Robinson, T. D., & Lewis, N. K. 2017, AJ, 153, 139

Gladstone, G. R., Stern, S. A., Enrico, K., et al. 2016, Sci, 351, 1280

Grzelczak, M., Vermant, J., Furst, E. M., & Liz-Marzán, L. M. 2010, ACS Nano, 4, 3591

Hadamcik, E., Renard, J.-B., Alcouffe, G., et al. 2009, PSS, 57, 1631

Hasenkopf, C. A., Freedman, M. A., Beaver, M. R., Toon, O. B., & Tolbert, M. A. 2011, AsBio, 11, 135

He, C., Hörst, S. M., Riemer, S., et al. 2017, ApJL, 841, L31

Hörst, S. M., He, C., Lewis, N. K., et al. 2018, NatAs, in press (doi:10.1038/s41550-018-0397-0)

Hörst, S. M., & Tolbert, M. A. 2013, ApJL, 770, L10

Hörst, S. M., & Tolbert, M. A. 2014, ApJ, 781, 53

Howe, A. R., & Burrows, A. S. 2012, ApJ, 756, 176

Howe, A. R., & Burrows, A. S. 2015, ApJ, 808, 150

Hu, R., & Seager, S. 2014, ApJ, 784, 63

Ito, Y., Ikoma, M., Kawahara, H., et al. 2015, ApJ, 801, 144

Kao, J., Bai, P., Chuang, V. P., et al. 2012, NanoL, 12, 2610

Klapetek, P., Valtr, M., Neečas, D., Salyk, O., & Dzik, P. 2011, NRL, 6, 514

Knutson, H. A., Benneke, B., Deming, D., & Homeier, D. 2014a, Natur, 505, 66

Knutson, H. A., Dragomir, D., Kreidberg, L., et al. 2014b, ApJ, 794, 155

Kreidberg, L., Bean, J. L., Désert, J.-M., et al. 2014, Natur, 505, 69

Lavvas, P., Yelle, R. V., & Vuitton, V. 2009, Icar, 201, 626

Li, L., Zhao, H., Vidali, G., et al. 2010, JPCA, 114, 10575

McCullough, P. R., Crouzet, N., Deming, D., & Madhusudhan, N. 2014, ApJ, 791, 55

Miller-Ricci, E., Seager, S., & Sasselov, D. 2009, ApJ, 690, 1056

Morley, C. V., Fortney, J. J., Marley, M. S., et al. 2015, ApJ, 815, 110

Moses, J. I., Line, M. R., Visscher, C., et al. 2013, ApJ, 777, 34

Plankensteiner, K., Reiner, H., Schranz, B., & Rode, B. M. 2004, Angew. Chem. Int. Ed., 43, 1886

Quirico, E., Montagnac, G., Lees, V., et al. 2008, Icar, 198, 218

Ricker, G. R., Winn, J. N., Vanderspek, R., et al. 2014, Proc. SPIE, 9143, 914320

Schaefer, L., Lodders, K., & Fegley, B., Jr. 2012, ApJ, 755, 41

Sciamma-O'Brien, E., Upton, K. T., & Salama, F. 2017, Icar, 289, 214

Sing, D. K., Fortney, J. J., Nikolov, N., et al. 2016, Natur, 529, 59

Spergel, D., Gehrels, N., Baltay, C., et al. 2015, arXiv:1503.03757v2

Sullivan, P. W., Winn, J. N., Berta-Thompson, Z. K., et al. 2015, ApJ, 809, 77

Szopa, C., Cernogora, G., Boufendi, L., Correia, J. J., & Coll, P. 2006, PSS, 54, 394

Tomasko, M. G., Archinal, B., Becker, T., et al. 2005, Natur, 438, 765

Tomasko, M. G., Doose, L., Engel, S., et al. 2008, PSS, 56, 669

Trainer, M. G., Pavlov, A. A., DeWitt, H. L., et al. 2006, PNAS, 103, 18035

Venot, O., Hébrard, E., Agúndez, M., Decin, L., & Bounaceur, R. 2015, A&A, 577, A332

Villarrubia, J. S. 1997, J. Res. Natl. Inst. Stand Technol., 102, 425

Wolfgang, A., & Lopez, E. 2015, ApJ, 806, 183