Danica Adams
Yangcheng Luo1- 1Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA, United States
- 2Jet Propulsion Laboratory, La Cañada Flintridge, CA, United States
Hosting a ∼1.5 bar N2 atmosphere and reducing atmospheric composition, Titan has the energy sources needed to drive disequilibrium chemistry and hosts an aerosol layer which shields the surface from incident UV radiation. This world draws parallels to an early Earth-like world (although ∼200 K cooler), and the atmospheric chemistry may be capable of forming relevant prebiotic species. Exo-Titan worlds at close-in orbits host photochemistry relevant to habitability with rich hydrocarbon chemistry. We investigate the effect of stellar type of the host star, equilibrium temperature, incident radiation, and vertical transport efficiency on the production of higher-order hydrocarbons. We find a greater incident radiation (a closer orbit) increases the rate of methane photolysis as well as photolysis of hydrocarbons. A larger H2 abundance and warmer temperature increases the rate of the back reaction H2 + CH3 → CH4 + H, and the temperature dependence is so great that CH3 recycles back into CH4 instead of forming C2H6. A larger H2 abundance and warmer temperature also encourages interesting cycling between C2H2, C2H3, and C2H4 via reactions with atomic H.
1 Introduction
Titan is the only solar system body demonstrated to have complex organic chemistry occurring in an Earth-like atmospheric envelope (∼1.5 bar), which is a result of its unique atmospheric properties: A N2 atmosphere with a reducing composition, energy sources to drive disequilibrium chemistry, and an aerosol layer to shield the surface from solar UV radiation (e.g., Yung et al., 1984; Wilson and Atreya, 2004; Willacy et al., 2016). This world draws parallels to an early Earth-like world which may have been reducing (e.g., Lunine 2005; Lorenz and Mitton 2008), and these characteristics make it an appealing object of study when exploring planetary habitability.
To date, over 5,000 exoplanets have been discovered, primarily due to NASA’s Kepler mission which searched for and discovered transiting exoplanets. Hot-Jupiters were the easiest planets to detect at first, but today small (1–4 Re), low mass (<20 Me) and short period (of less than 100 days) planets are the most common type of exoplanet known today (e.g., Bean et al., 2020). The atmospheres of small close-in planets are vulnerable to rapid escape; however, it has been recently suggested that during planet formation of super-Earth planets, H2 may not have accumulated as a thick gaseous envelope, but instead would dissolve in the interior magma (Chachan and Stevenson, 2018; Kite et al., 2020). Outgassing of a reduced secondary atmosphere may be plausible and has been suggested to explain the observed atmospheric spectra of GJ 1132b, a super-Earth orbiting an M-Dwarf at a close-in orbit at 0.01 AU, a super-Earth orbiting an M-Dwarf at a close-in orbit at 0.01 AU (Swain et al., 2021). Recent Hubble Space Telescope (HST) observations suggest a surface pressure between 1 and 10 bars, a surface temperature of 950 K, a stratospheric temperature of ∼480 K, and an H2-dominated atmosphere with nitrogen and hydrocarbon chemistry (Swain et al., 2021). Although, recent works have also disputed the observations, suggesting either that photochemical hazes muted the spectral features or that no atmosphere was present (Libby-Roberts et al., 2021; Mikal-Evans et al., 2021).
The photochemistry in the reduced atmospheres of close-in, rocky planets may be unique from the solar system worlds. Previous studies have primarily examined the surface climate and atmospheric circulation of Earth-like exoplanets (e.g., Merlis and Shneider 2010; Kopparapu et al., 2013; Shields et al., 2013; Kaspi and Showman 2015; Shields et al., 2016), but fewer investigations have explored the range of possible conditions at exoplanets with photochemical hazes, reduced atmospheres, and/or different equilibrium temperatures. Morley et al. (2015) considers the photochemical production of aerosol precursors, as well as cloud distribution and synthetic spectra, over a wide range of stellar irradiances, metallicities, and aerosol sedimentation rates. Lora et al. (2018) examines the response of a Titan-like atmosphere to different host stars and finds (in agreement with results presented here in Section 3) that the greater shortwave activity but lower luminosity of M-Dwarves both result in a lesser production of hydrocarbons. Motivated by GJ 1132b, here we investigate the response of a Titan-like atmosphere to a larger swath of planetary parameters than previously considered in order to more closely adapt known atmospheric chemistry to the conditions of close-in super-Earths: to a warmer temperature, larger irradiation flux, different stellar type, and different background H2:N2 ratios. We term these planets exo-Titan due to their similarities in atmospheric composition (reduced, N-bearing chemistry), although we acknowledge the differences in interior composition, planetary radius, and temperature.
2 Materials and methods
We adapt the Titan KINETICS model presented in Willacy et al. (2022) to various Exo-Titan atmospheres orbiting Sun-like and M-Dwarf host stars. The model considers 111 species linked by 1,143 reactions in order to calculate the chemical production and loss rates at each altitude as well as the diffusive flux between each altitude grid by solving the 1D continuity equation.
We consider Titan and GJ 1132b as our two end members, and consider a swath of theoretical intermediates between in order to examine the photochemical response to four parameters: 1) The stellar type, M-Dwarf vs. K-star vs. Sun-like host star; 2) close-in orbit, ranged from a Titan-like distance of 9.55–0.01 AU; 3) temperature, from a Titan temperature (94 K at the surface and 170 K in the stratosphere) to a GJ 1132b temperature (950 K at the surface and 480 K in the stratosphere); and 4) initial H2:N2 ratio, varied from Titan-like (or <1% H2) to GJ 1132b-like (10% N2 and 90% H2).
The temperature-pressure (T-P) profile at Titan comes from Willacy et al. (2022), and for orbits at the same equilibrium temperature at different host stars we maintain the same T-P profile. Note however that the stellar spectrum is known to influence the T-P profile through Rayleigh scattering, near-infrared absorption, and convection, and for details about these effects we refer the reader to Eager et al. (2020). The T-P profile at the 9.5 AU at dimmer stars is scaled according to the differing equilibrium temperatures. The T-P profile of GJ 1132b comes from Swain et al. (2021).
The stellar type (M-Dwarf) and properties of GJ 1132 are very similar to those of GJ 1214 (with a temperature of 3000 K and mass of 0.15 solar masses), which is a stellar spectrum that has been well studied. Figure 1 compares the incident radiation at 1 AU of this star and the Sun.
FIGURE 1. Stellar spectra of the Sun (black), an M4.5 host star (red), and a K star (blue), all shown at 1 AU. Photon flux is shown in photons/cm2/s. We obtain the K and M star spectra from the MUSCLES database (France et al., 2016), and we adapt the solar flux from Gladstone et al. (2010). In all cases shown, we have binned to a coarser resolution than the original datasets to minimize model runtime.
We compute synthetic spectra of the predicted photochemical results in order to consider potential detectability. We use Exo-Transmit (Kempton et al., 2017), an open-source radiative transfer code, that calculates atmospheric transmission spectrum of transiting exoplanets. In this study, we include eleven species—C, CH4, C2H2, C2H4, C2H6, H, HCN, H2, N, N2, and NH3. Then, Exo-Transmit finds atmospheric opacity by interpolating between single-molecule cross section data for CH4, C2H2, C2H4, C2H6, HCN, N2, and NH3 between a predefined temperature-pressure grid (temperature ranging from 100 K to 3000 K with a spacing of 100 K, pressure ranging from 10−4 Pa–108 Pa with a spacing of one order of magnitude) and collision-induced-absorption opacity data for CH4–CH4, H2–H2, H2–H, H2–CH4, N2–CH4, N2–H2, and N2–N2 between the same temperature grid, solves the radiative transfer equation line by line, and generates wavelength-dependent transit depths. The wavelength range is 300–30 μm. Exo-Transmit considers the oblique path of light through the planetary atmosphere along a distant observer’s light of sight. It also accounts for opacity caused by Rayleigh scattering. All opacity data in Exo-Transmit is taken from Freedman et al. (2008), Freedman et al. (2014), and Lupu et al. (2014).
We carry out Exo-Transmit calculations for 10−5–103 mbar of the modelled atmosphere. Exo-Transmit has a resolving power λ/Δλ of 1,000. For visual clarity, we perform a running average with a resolving power of 50. It is worth noting that some of the modelled atmospheres have altitude ranges with temperatures lower than 100 K where Exo-Transmit does not have opacity data. We manually set the opacity for 70–100 K the same as that for 100 K. Sensitivity tests show that the transmission spectra are robust against different approaches of extrapolation.
3 Results
3.1 Stellar irradiance on hydrocarbon chemistry
The production of hydrocarbons is driven by methane photolysis, which makes the incident photon flux a critical driver of hydrocarbon chemistry. An M-Dwarf host star is more active in the shortwave region than longwave, compared to the Sun. However, the star is less luminous making the total incident radiation at 2 AU orbit comparable to the 9.5 AU orbit around the Sun.
Here, we consider the hydrocarbon chemistry at five worlds: Titan around the Sun, Titan around an M-Dwarf at an orbit of 2 AU and 9.5 AU, and Titan around a K star at an orbit of 5.6 AU and 9.5 AU. The resulting mixing ratios of relevant hydrocarbon species for these cases is shown in Figure 2, and the following sections explain the chemistry driving these results. A similar investigation is presented in Lora et al. (2018), and our results presented in this section largely agree with theirs. Understanding these cases is imperative to understanding the novel results presented later in this work.
FIGURE 2. Response to stellar type and irradiation; all cases are at a Titan-like temperature and N2-dominated atmosphere. Black line: Sun-like star at 9.55 AU; solid red line: M-Dwarf star at 2.0 AU; dashed red line: M-Dwarf star at 9.5 AU; solid blue line: K star at 5.6 AU; dashed blue line: K star at 9.5 AU. Note that the total irradiation at 2.0 AU from an M-Dwarf host star and 5.6 AU from a K star are both comparable to the total irradiation a world experiences at 9.55 AU from a Sun-like star. From left to right, the panels show CH4, C2H2, C2H4, C2H6, HCN, HC3N, and C2H3CN.
3.1.1 Ethane, C2H6
At all cases, the production of C2H6 is dominated by 2CH3+M, where M is the third body (Figure 3). At the same equilibrium temperatures (close-in orbits of 5.6 AU and 2.0 AU around the K and M star respectively), the photolysis of methane is comparable to that of Titan around the Sun (Figure 3). However, the enhanced flux of short wavelength (
FIGURE 3. Reaction rates (cm−3·s−1) of dominant production and destruction reactions for C2H6. Black lines represent solar system Titan, solid red lines represent Titan around an M-Dwarf at 2 AU, dashed red lines represent Titan around and M-Dwarf at 9.5 AU, solid blue lines represent Titan around a K star at 5.6 AU, and dashed blue lines represent Titan around a K star at 9.5 AU.
At all cases, the dominant loss of ethane are reactions to C2H and C3N. At a distant orbit of 9.5 AU around an M-Dwarf, methane photolysis is slowed but N2 photolysis is still enhanced, and thus production of ethane is limited. Methane photolysis results from slightly longer wavelength photons (770–1600 A) than N2 photons (680–980 A). A distant orbit means all photon fluxes are reduced compared to a close-in orbit. However, since M Dwarves emit more photons in the smaller wavelengths (relative to longer wavelengths), the slowed photolysis effect is lesser for N2 photolysis. At a distant orbit around a K star, however, dimmer emission at short wavelengths limits N2 photolysis at depth and thereby severely limits N. This slower loss of CH3 allows the C2H6 production and steady state concentration at a K-star-hosted planet to be more comparable to that at solar system Titan.
3.1.2 Acetylene, C2H2, and ethylene, C2H4
At Titan, the concentration of acetylene is influenced by production via C2H+CH4, and CH2+CH2 balanced by destruction via photolysis which yields C2H+H. However, in the upper atmosphere, H+C2H3 and CH3+C2H3 and CH3+C3H2 become increasingly relevant as the host star becomes dimmer, where the cycling among C2H2, C2H3, and C3H2 balances the C2H2 concentration. Additionally, at planets around an M-Dwarf, upper atmospheric C2H2 is lost to reactions with CN (due to the faster photolysis of N2), while photolysis of C2H2 remains as the dominant lower atmosphere destruction reaction.
At all cases CH+CH4 is the dominant production, and photolysis is the dominant destruction. At a comparable effective temperature (2 AU around the M-Dwarf), the greater flux of energetic photons results in faster methane photolysis and thereby a faster production of ethylene. From the same distance (9.5 AU), photolysis of both methane (production) and C2H4 (loss) are slowed and therefore the steady state mixing ratios at Titan and the 9.5 orbit around an M-Dwarf are comparable. Similar trends occur for planets around a K-star; however, the slowing of photolysis rates between the constant effective temperature case and 9.5 AU case is less severe due to the more similar orbit distances presented (only a 4.1 AU change around a K star, but 7.5 AU change around an M Dwarf). The rates of these reactions are compared in Figure 4.
FIGURE 4. Reaction rates (cm−3·s−1) of dominant production and destruction reactions for C2H2 and C2H4. Black lines represent solar system Titan, solid red lines represent Titan around an M-Dwarf at 2 AU, dashed red lines represent Titan around an M-Dwarf at 9.5 AU, solid blue lines represent Titan around a K star at 5.6 AU, and dashed red lines represent Titan around a K star at 9.5 AU.
3.1.3 -CN species
The greater photon flux in the shortwave spectral region emitted by the M and K stars yields a greater abundance of N and thereby a faster column production of HCN. At the same effective temperature, the planet around the K star hosts the fastest column production of HCN (noticing the fast rate in the upper most region which dominates the column rate). HCN photolysis is driven by lyman-alpha photons, and at the same effective temperatures, the difference in photon flux at these wavelengths causes HCN destruction to be largest at the K star, intermediate at the sun, and smaller at the M star. Generally, HCN is fairly stable to photolysis, so the larger steady state concentration occurs in the case where production is fastest: at the 5.6 AU K star orbit. This planet hosts an ideal combination of fast N2 destruction and abundant hydrocarbons (for N radicals to destroy). Dissociation of N2 and HCN are both faster around the M star than around the sun (see Figure 5), and these effects balance each other out, yielding a comparable HCN concentration as that at solar system Titan.
FIGURE 5. Reaction rates (cm−3·s−1) of dominant production and destruction reactions for -CN species. Black lines represent solar system Titan, solid red lines represent Titan around an M-Dwarf at 2 AU, dashed red lines represent Titan around an M-Dwarf at 9.5 AU, solid blue lines represent Titan around a K star at 5.6 AU, and dashed red lines represent Titan around a K star at 9.5 AU.
Photolysis of HCN, the primary loss mechanism, results in CN which may form C2H3CN via reactions with C2H4; although, CN may also cycle back to HCN via reactions with the hydrocarbons. For the same reasons that HCN is larger around the K star at the same equilibrium temperature as solar system Titan (5.6 AU), HC3N and C2H3CN are largest around the K star. Meanwhile, in the 9 AU orbit around the M star, slowed photolysis due to a lower photon flux in total, limits the presence of N and CH3. HCN loss to photolysis is similarly slowed, however, resulting in a similar steady state concentration.
3.2 Temperature and H2 composition on hydrocarbon chemistry
With the same solar host star and at the same orbit of 9.5 AU, we now investigate the hydrocarbon chemistry in a cold N2 atmosphere (Titan), a cold H2 dominated atmosphere, and a warm H2 dominated atmosphere (e.g., a sub-Neptune or close-in super Earth). The H2-dominated atmospheres are motivated by the recognized H2-dominated atmosphere of GJ 1132b (Swain et al., 2021) and predicted reduced interiors of close-in super Earths described in Section 1. The temperature-pressure-altitude profiles are shown in Figure 6. The resulting steady state mixing ratios for these cases are shown in Figure 7, and the following sections investigate the chemistry involved.
FIGURE 6. Temperature-pressure-altitude profiles of the cold solar system Titan N2 atmosphere (black) and warm Exo-Titan H2 atmosphere (red). Notice the altitude scale changes for the Exo-Titan, which is a result of the warmer temperature and puffy nature (large scale height) of H2 atmospheres.
FIGURE 7. Response to temperature and H2 content; all cases are around a Sun-like star at 9.5 AU. Solid black lines: Titan temperature, N2 dominated atmosphere; red lines: warm, H2 dominated atmosphere; blue lines: Titan temperature (cold), H2 dominated atmosphere. From left to right, the panels show CH4, C2H2, C2H4, and C2H6.
3.2.1 Methane, CH4, and ethane, C2H6
The reaction H+CH4 → CH3+H2 is well known to be a mechanism for methane destruction at Titan, other than methane photolysis. Both this reaction and its back reaction, H2+CH3 → CH4+H, are highly temperature dependent, and in the warmer atmosphere these reactions recycle CH3 back into CH4, which will limit hydrocarbon production. H+CH3+M is a second important reaction to destroy CH3, and this reaction also becomes faster in the H2 atmospheres due to the greater concentrations of H (see Figure 8).
FIGURE 8. Reaction rates (cm−3·s−1) of CH4-CH3 recycling and dominant production and destruction reactions for C2H6. Black lines represent a cold N2 atmosphere (Titan), blue lines represent a cold H2 atmosphere, and red lines represent a warm H2 atmosphere.
In the N2-dominated atmosphere, photolysis of methane becomes severely photon limited above 0.1 mbar since shortwave photons are lost to N2. In both H2-dominated atmospheres, however, the atmosphere is less opaque to incident stellar photons and photolysis of methane extends down to the near-surface. The CH3 produced from methane photolysis recycles back into methane. However, the photolysis branch of CH2+H acts as a longer-lived sink of methane, and this CH2 may then be photolyzed to CH to kick off subsequent hydrocarbon chemistry described in the following sections.
This cycling does not directly affect the methane profile, but the faster destruction of CH3 is important to the larger hydrocarbons that are shown next.
For all three cases, the production of C2H6 is dominated by the reaction 2CH3 → C2H6. At Titan, ethane is largely destroyed to reactions with C2H and secondly to reactions with C3N. However, in an H2-dominated atmosphere, loss is dominated by H+C2H6 → C2H5+H2. The slower production in the warm case in combination with a faster loss rate to atomic hydrogen in both cases (see Figure 8) results in a depleted C2H6 profile in the H2-dominated atmospheres (as in Figure 7).
3.2.2 Acetylene, C2H2
At Titan, C2H2 is known to form from C2H+CH4 in the upper atmosphere and is destroyed via photolysis to form C2H+H, and these reactions lead to the autocatalytic destruction of methane. Importantly, C2H is a chemical product of destruction of larger hydrocarbons, so we note another relevant production of C2H2 directly from methane photochemical products is CH+CH2 → C2H2+H. In an H2-dominated atmosphere, the main production of C2H2 occurs via C2H+H2 instead of with CH4 (as at Titan), and the main destruction is again via photolysis to form C2H+H occurs in the upper atmosphere.
In the H2-dominated atmospheres, faster production and loss reactions occur in an inner cycle between C2H2, C2H3, and C2H4 via reactions with H and H2. Importantly, this exchange is imperfect; in the full profile C2H2 reacts to form C2H3, which cycles back into C2H2 only in the upper atmosphere. In the middle and lower atmospheres C2H3 reacts with H2 to build C2H4 instead of C2H2. C2H4 photolysis sources C2H2 in the middle atmosphere.
In the middle atmosphere, most of these inner cycle reaction rates are comparable to the rates at Titan. However, the photolysis of C2H2 is faster at Titan due to a larger steady state concentration of C2H2, and the production of C2H2 via C2H+CH4 is faster than C2H4 photolysis (see Figure 9). Therefore, the inner cycle reactions are small compared to the main production/destruction reactions at Titan. At the H2 dominated atmospheres though, the inner cycle is more important, where the photolysis rate is comparable to the inner cycle reaction rates.
FIGURE 9. Rates (cm−3·s−1) of dominant production and loss reactions for C2H2 in the top panel. Rates of exchange reactions between C2H2-C2H3-C2H4 in the bottom panel. Black lines represent a cold N2 atmosphere (Titan), blue lines represent a cold H2 atmosphere, and red lines represent a warm H2 atmosphere.
3.2.3 -CN species
In the mid-atmosphere, HCN loss to C2H3 becomes faster in the H2-dominated warm atmosphere due to the faster formation of this radical via H+C2H2 (Figure 10), resulting in a lower concentration ∼1 mbar. Photolysis of HCN still yields CN, yet in the H2-dominated atmospheres, reactions to C2H2 act as the primary production pathway to HC3N and C2H3CN, resulting in a narrower production peak near 0.1 μbar (due to the results of C2H2 shown in 3.2.3).
FIGURE 10. Rates (cm−3·s−1) of dominant production and loss reactions for -CN species. Black lines represent a cold N2 atmosphere (Titan), blue lines represent a cold H2 atmosphere, and red lines represent a warm H2 atmosphere.
3.2.4 Ethylene, C2H4
At Titan, C2H4 is formed from the reaction CH+CH4 and lost to photolysis which yields C2H2 and either H2 or 2H. The CH3-CH4 exchange described in 3.2.1 encourages the production of CH, thereby increasing the production rate of C2H4 in the warm H2 atmosphere.
In addition to photolysis, in the H2 atmospheres, C2H4 is lost to reactions with H2 to form C2H5, and in the upper atmosphere, the latter reacts with H to form 2CH3. In the warm H2 atmosphere, the CH3 may cycle back to methane, photolyze, and further encourage the production reaction CH+CH4. The rates of these reactions are shown in Figure 11.
FIGURE 11. Rates (cm−3·s−1) of dominant production and loss reactions for C2H4. Black lines represent a cold N2 atmosphere (Titan), blue lines represent a cold H2 atmosphere, and red lines represent a warm H2 atmosphere.
4 GJ 1132b: A warm H2 atmosphere at a close-in orbit around an M-Dwarf
Thus far we have examined, individually, the effect of changing the temperature, host star, semi-major axis, and stellar type. GJ 1132b is an interesting world with all of these parameters differing from the solar system Titan. Hubble Space Telescope (HST) observations revealed a warm (stratospheric T of 480 K), H2-dominated atmosphere in an otherwise Titan-like atmosphere (90% H2, 8.9% N2, 0.3% HCN, 0.3% CH4, 0.3% CO; Swain et al., 2021), and the world orbits an M-Dwarf at a close-in orbit of 0.01 AU (Bonfils et al., 2018).
Figure 12 shows that the C2H2 profile peaks just above 0.1 mbar, or near 1,000 km. Above the peak, the rate of formation is limited by the rate of methane photolysis of (due to a low number density). Centered near the peak, the fate C2H2 is photolysis to C2H, which may cycle back into C2H2. But, below the peak C2H2 is lost to reactions with H to yield C2H3, which may either cycle back to C2H2 or build larger hydrocarbons. The latter means reactions with H act as a more efficient net loss of C2H2 than photolysis, hence decreasing the mixing ratio profile of C2H2 in the regions below.
FIGURE 12. GJ 1132b (red lines; warm, H2 dominated atmosphere at 0.01 AU away from an M-Dwarf host star) vs. Titan (black lines; cold, N2 dominated atmosphere at 9.55 AU away from the Sun). From left to right, the panels show C2H2, C2H4, and C2H6.
The C2H4 profile is comparable to that at Titan as shown in Figure 12. At a close-in orbit around an M-Dwarf, photolysis of methane is efficient and thus synthesis of C2H4 via CH+CH4 is fast. Meanwhile, photolysis of C2H4 (the main loss) is also efficient. Hence, the production and loss rates have been altered comparably and hence the steady state abundance of C2H4 is not majorly changed.
We find a depletion in the C2H6 profile due to the CH3-H2 exchange reactions which efficiently recycle CH3 back to methane before two CH3 molecules may react to form C2H6. Figure 13 summarizes the new chemical pathways found, starting from Titan (black arrows) and modifying to different host stars, orbital distances, temperatures, and H2:N2 compositions (colored arrows).
FIGURE 13. Diagram of important reactions relevant to hydrocarbon chemistry at Exo-Titans, based off the Titan chemistry presented in Yung et al. (1984). Reactions highlighted in blue show those with a large temperature dependence, thus dominating the chemistry in warmer atmospheres. Reactions highlighted in red show those which become significant in H2-dominant atmospheres. Reactions highlighted in green show those which become significant at worlds around M-Dwarves.
5 Discussion
5.1 Model validation
In this work, we extrapolate the known photochemistry of Titan (e.g., Willacy et al., accepted) to putative super-Earth conditions which will become testable in the new JWST era. In order to ensure valid predictions, we validate our model against atmospheric observations of the Titan atmosphere (Figure 14). Our lower boundary conditions of CH4 are based on observations, forcing the lower atmosphere to agree with near-surface observations. The resulting photochemically produced hydrocarbons and N-bearing species roughly agree with the measurements from ALMA and Cassini. Our model overestimates the HCN profile in the lower atmosphere, which we speculate may be related to condensation processes, but the profile roughly matches in the upper atmosphere. Overall, the success of our model reproducing the observations in most regions demonstrates that our predictions of putative super-Earth atmospheres are grounded in a complete photochemical model.
FIGURE 14. Mixing ratio profiles of CH4, C2H2, C2H4, C2H6, HCN, and HC3N at Titan. Model results are in black and overplotted dots show a comparison to recent observations in the literature: (1) Niemann et al. (2010); (2) Koskinen et al. (2011); (3) Nixon et al. (2013); (4) Magee et al. (2009); (5) Lombardo et al. (2019); (6) Adriani et al. (2011); (7) Kim et al. (2005); (8) Shemansky et al. (2005); (9) Vervack et al. (2004); (10) Vinatier et al. (2010); (11) Cordiner et al. (2014); (12) Cui et al. (2009); (13) Marten et al. (2002)
5.2 Aerosols
Photochemical hazes are common in reducing atmospheres, as a result of methane and hydrocarbon destruction by solar UV photons and high-energy ions and neutrals, followed by polymerization of the radical species products. Hazes play important roles in radiative transfer, atmospheric dynamics, and atmospheric composition (e.g., Zhang et al., 2017), and they are predicted in atmospheres cooler than ∼1000 K (e.g., Gao et al., 2017). Therefore, hazes are common at solar system worlds with reduced atmospheric chemistry, having been revealed at Titan by Voyager (West et al., 1983; West and Smith, 1991) and Cassini (e.g., Tomasko et al., 2008; Lavvas et al., 2009; 2010), Pluto by New Horizons (e.g., Gao et al., 2017; Cheng et al., 2017; Fan et al., 2021), and Triton (e.g., Ohno et al., 2021). Photochemical hazes are also common at exoplanets and influence observables by acting as grey absorbers and muting spectral features (e.g., Adams et al., 2019; Kawashima and Ikoma, 2019; Zahnle et al., 2016; Marley et al., 2013).
Our photochemical models predict notable photochemical production rates of haze material, assuming a soot (hydrocarbon-based) or tholin (N-bearing, hydrocarbon-based) composition. We find rates similar to the production rate at Titan regardless of stellar type or H2 atmospheric content: 2.2e9 molecules cm−2·s−1 at Titan; 2.5e9 molecules cm−2·s−1 at a 2 AU orbit around an M Dwarf; 1.2e9 molecules cm−2·s−1 at a 5.6 AU orbit around a K star; 3.4e9 molecules cm−2·s−1 for a warm H2 atmosphere; and 3.4e9 molecules cm−2·s−1 for a cool H2 atmosphere. However, the close-in orbits (e.g., GJ 1132b) host large photolysis rates of 8.0e13 molecules cm−2·s−1 due to the greater flux of incident photons. The particle sizes are known to scale with production rate (controlled by this preceding photochemistry), which the role of hazes on radiative transfer is dependent on. A larger production rate could lead to more particles available to coagulate, resulting in larger particles. This result may skew observations by muting spectral features, although we note that other parameters may influence the microphysics of particle growth (such as gravity influencing sedimentation, dynamics influencing upward diffusion, and particle fractal dimensions influencing radiative transfer).
5.3 Relevance to laboratory measurements
Photochemically derived tholin-like hazes are predicted in the atmosphere of Titan and Titan-like worlds. While haze properties have been derived from atmospheric measurements and compared to numerical models (e.g., Tomasko et al., 2008), the chemical composition of these hazes has not yet been measured at Titan. Laboratory experiments have attempted to constrain the composition by varying parameters including the bulk atmospheric composition, energy sources, trace gases present, temperature (e.g., Khare et al., 1981; Imanaka et al., 2004, 2012; Yoon et al., 2014). Importantly, these works find that tholin-like hazes are meaningful to astrobiology, acting as precursors to amino acids and prebiotic chemistry (e.g., Cable et al., 2012; references therein). For example, after creating tholins in a laboratory environment with a Titan-like background gas composition, hydrolysis was found to yield amino acids including alanine, glutamine, glycine, aspartic acid, and glutamic acid on timescales of a few months (Neish et al., 2010). Similarly, Horst et al. (2012) detected nucleobases and amino acids (including adenine, guanine, uracil, thymine, and cytosine) when exposing a Titan-like laboratory environment to electric discharges. Urea and glycine were also produced in a lab with reducing conditions exposed to electric discharge and plasma impact (Civis et al., 2017). Note that HCN is thought to be an important intermediate which may lead to the formation of nucleobases. Ferus et al. (2017a) find large amounts of HCN and formamide, and the latter is an unstable intermediate likely to decompose to yield HCN (e.g., Ferus et al., 2017b). The results of our work suggest that close-in exo-Titans (such as GJ 1132b) may form Titan-like hazes much quicker than Titan, and the laboratory results discussed suggest this result may imply a greater production of these prebiotic species.
5.4 Predicted observability
The new era of JWST begs the question of whether the predicted concentrations and chemistry found in this work are potentially testable. We find that the predicted concentrations at solar system Titan and Titan around an M-Dwarf are both not likely to be detected due to their atmospheres’ small scale height. However, the larger scale height of the H2 dominated atmospheres encourage a more feasible detection of the hydrocarbons and nitrile species. GJ 1132b is an especially interesting world: the large scale height, close-in orbit to a relatively smaller star, and greater concentration of HCN makes for potentially more feasible detections. We find that solar system Titan would yield spectral features of order ∼1 ppm, while GJ 1132b could yield spectral features of up to >150 ppm in a hazy sky and up to 1,000 ppm in a clear sky.
We present results assuming both a hazy sky and clear sky at all worlds. As discussed in Section 5.2, observations of Titan reveal tholin-like hazes which would mute spectral features, and our photochemical model predicts a haze production rate several orders of magnitude larger at GJ 1132b thereby worsening the outlook for detectability. A flat or sloped spectrum may be capable of muting the large spectral features predicted for GJ 1132b shown in Figure 15. In these results, we do not solve for the haze parameters, but instead assume an optically thick haze layer whose top is located at 10 Pa (motivated by the vertical extent of Titan’s hazes; e.g., Rages and Pollack, 1983; West et al., 2018). Exo-Transmit only considers extinction caused by the atmosphere above this pressure level. However, we note that the larger haze production rate at GJ 1132b (see Section 5.2) may influence the haze properties to deviate from those at Titan.
FIGURE 15. Computed transmission spectra for the bookend exo-Titan cases presented in this paper (upper) solar system Titan vs. a 2 AU orbit around an M star; (middle) solar system Titan vs. a cold H2-dominated atmosphere (blue) vs. a warm H2 dominated atmosphere (red); (lower) solar system Titan vs. GJ 1132b. Notice the different y-axis scales, where the spectral features in the upper panel are well below detection thresholds and spectral features in the middle and the lower panels are much larger and potentially detectable with JWST. The absorption regions of detectable species are labeled above the uppermost panel. CIA, collision-induced absorption.
We adapted PandExo, an open source code which determines the noise floor of JWST observations (Batalha et al., 2017), to GJ 1132b, and we find a noise floor of ∼400 ppm for NIRCAM’s G395H instrument (acknowledging this value varies with wavelength dependences). Comparing to Figure 15 (bottom left panel), we predict the aerosols would mute spectral features below the noise floor for potential detection at GJ 1132b. The molecular features for the species presented in our work would be detectable in a clear sky at GJ 1132b (bottom right panel); however, we find those conditions to be unlikely provided the large haze production rate (see Section 5.2). While JWST detections of these predictions may be challenging, detection of these signals will likely be possible with future instruments dedicated for atmospheric characterization of transiting exoplanets.
6 Conclusion
A larger H2 abundance and warmer temperature increases the rate of the back reaction H2+CH3 → CH4+H, and the temperature dependence is so great that CH3 recycles back into CH4 instead of forming C2H6. A larger H2 abundance and warmer temperature also encourages interesting cycling between C2H2, C2H3, and C2H4 via reactions with atomic H. This results in a decreased column abundance of C2H6 and C2H2 and relatively larger column abundance of C2H4 at close-in Exo-Titans with warm, H2-dominant atmospheres than Titan, at a more distant orbit with a cool, N2-dominant atmosphere. Meanwhile, close-in orbits around stars with greater shortwave photon emission result in faster N2 photolysis and a greater availability of HCN, HC3N, and C2H3CN. We find these abundances may be detectable at close-in, H2 dominated atmospheres (e.g., GJ 1132b) should these worlds have clear skies, but we caution the reader of large haze production rates which may mute these spectral features.
Data availability statement
The original contributions presented in the study are included in the article/supplementary material, further inquiries can be directed to the corresponding author.
Author contributions
DA and YL developed the research concept and contributed to drafting and editing the manuscript. DA performed the model simulations.
Funding
DA was supported by NASA’s FINESST program under Proposal Number 80NSSC19K1548. YL was supported in party by funding from NASA’s Astrobiology Institute’s proposal “Habitability of Hydrocarbon Worlds: Titan and Beyond” (PI: R.M. Lopes of JPL).
Acknowledgments
We thank Karen Willacy, Mark Swain, and Randy Gladstone for providing helpful discussions which greatly helped this work.
Conflict of interest
The authors declare that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.
Publisher’s note
All claims expressed in this article are solely those of the authors and do not necessarily represent those of their affiliated organizations, or those of the publisher, the editors and the reviewers. Any product that may be evaluated in this article, or claim that may be made by its manufacturer, is not guaranteed or endorsed by the publisher.
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Keywords: hydrocarbon, exoplanet atmosphere, titan, photochemistry, exoplanet astronomy
Citation: Adams D, Luo Y and Yung YL (2022) Hydrocarbon chemistry in the atmosphere of a Warmer Exo-Titan. Front. Astron. Space Sci. 9:823227. doi: 10.3389/fspas.2022.823227
Received: 26 November 2021; Accepted: 31 August 2022;
Published: 19 September 2022.
Edited by:
Jun Yang, Peking University, ChinaReviewed by:
Xinting Yu, University of California, Santa Cruz, United StatesNigel John Mason, University of Kent, United Kingdom
Copyright © 2022 Adams, Luo and Yung. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.
*Correspondence: Danica Adams, ZGphZGFtc0BjYWx0ZWNoLmVkdQ==