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Photochemical activity of Titan’s low-altitude condensed haze


Titan, the largest moon of Saturn and similar to Earth in many aspects, has unique orange-yellow colour that comes from its atmospheric haze, whose formation and dynamics are far from well understood. Present models assume that Titan’s tholin-like haze formation occurs high in atmosphere through gas-phase chemical reactions initiated by high-energy solar radiation. Here we address an important question: Is the lower atmosphere of Titan photochemically active or inert? We demonstrate that indeed tholin-like haze formation could occur on condensed aerosols throughout the atmospheric column of Titan. Detected in Titan’s atmosphere, dicyanoacetylene (C4N2) is used in our laboratory simulations as a model system for other larger unsaturated condensing compounds. We show that C4N2 ices undergo condensed-phase photopolymerization (tholin formation) at wavelengths as long as 355 nm pertinent to solar radiation reaching a large portion of Titan’s atmosphere, almost close to the surface.


Titan, an orange-yellow coloured moon of Saturn, is unique in many ways. It is the second largest moon in our solar system and the only moon with a significant atmosphere—enriched with organics, in the atmosphere and on the surface. Unlike Earth, Titan’s atmosphere is oxygen-deficient, but instead dominated by nitrogen (>90%) and methane (~5%). Organics on Titan originate from photochemistry of N2 and CH4 in Titan’s upper atmosphere, initiated by solar wind particles and solar ultraviolet radiation. The earlier Voyager1 and the current Cassini-Huygens2,3,4 missions have provided tremendous insight into the atmosphere, aerosols and the surface—lakes, flows and dunes.

The processes that control the observed Titan’s haze are still not well understood; in particular, at what altitudes the haze formation occurs. Pioneering laboratory studies showed that polymeric organic material, called tholins5,6, formed in discharge-driven reactions involving nitrogen, methane and other atmospheric compounds have optical properties similar to what had been deduced from observations of the Titan’s haze. Please note that ‘tholins’ are laboratory analogues of Titan’s haze particles, not the haze itself. Larger organics are currently thought to form high in Titan’s atmosphere at altitudes above 800 km (7), grow through coagulation in the lower atmosphere down to 500 km (refs 8, 9, 10), and finally rain down onto the surface. It has been suggested that ultraviolet-induced chemical processing (aging and hardening) of these aerosols can occur via solid-state polymerization11,12. Other observations and modelling studies infer that about 60% of the total column mass production of tholin-like aerosols may occur below 300 km (ref. 13) and that the production of large macromolecular particles peaks at ~100 km (ref. 14). This production includes condensation of simpler unsaturated organic compounds onto the larger haze particles at these cold low altitudes15.

Below ~600 km, the gas composition and organic haze of Titan’s atmosphere significantly attenuate the greater part of high-energy electron, ion and photon radiation16. However, at longer wavelengths the solar spectrum is not significantly attenuated in Titan’s atmosphere until the 100 km altitude level is reached17. For example, ~99% of photons at wavelengths >220 nm make it through to lower altitudes14,18. The solar flux at 220 nm is estimated to be ~1 × 1010 photons cm−2 nm−1 s−1 at 200 km, and at the same altitude the estimated solar flux at 350 nm is ~3 × 1011 photons cm−2 nm−1 s−1. The solar flux at 350 nm and at 200 km altitude is comparable to the upper atmosphere radiation field at shorter wavelengths that is important for inducing gas-phase upper atmospheric photochemistry. Even at lower altitudes (for example, at 70 km) the photon flux is not insignificant at both these wavelengths (~8 × 107 photons cm−2 nm−1 s−1). Thus, photochemical reactions that may occur in lower atmosphere (<600 km) involving longer wavelength solar photons (>200 nm) will have a significant role to play in Titan’s atmosphere and its photochemical evolution.

Titan’s unusual dense and oxygen-depleted atmosphere has a wide variety of linear unsaturated polyynes—nitrogen-containing polycyanoacetylenes19, such as C4N2 as well as polyacetylenes20 and aromatic molecules21—that undergo photopolymerization forming complex tholin-like molecules, whose structure is still under intense investigation22. Recent laboratory studies showed that when these tholins come into contact with oxygen-bearing molecules such as water (surface/subsurface ice on Titan), result in the formation of complex prebiotic molecules such as amino acids5 and nucleobases23,24. Thus, atmospheric aerosol photochemistry has a key role in the processes leading to the potential prebiotic chemistry on Titan’s surface25.

As photoabsorption of condensed molecules can occur at longer wavelengths due to polarizability of condensed phase26 exciton interactions27,28 and spin-orbit coupling29, compared with their isolated molecular counterparts, the absorption of longer wavelength photons may trigger solid-state chemical processes with a sufficient yield to significantly affect low-altitude particle composition. Solid-state organic photochemistry could continue to altitudes as low as 50 km or below, leading to progressive conversion of Titan’s aerosols to complex polymeric organic material during the rain-down process.

The three possible phases of organics in Titan’s atmosphere are schematically shown in Fig. 1. Our laboratory studies presented here model the condensed small linear organic molecules that form a class of polyynes observed on Titan. While preparing a mixture of various possible polyynes and cyanopolyynes, as shown in Fig. 1, would be a challenging task, the photochemical principles that govern these mixed monomers can be illustrated in the chemistry of one of these components alone, hence our choice to study single monomer condensates. Voyager 1 provided the first detection of crystalline organic ice in the Titan’s atmosphere—dicyanoacetylene (C4N2)—that confirmed the model expectation for gas condensation30,31, which prompted a series of laboratory work on C4N2 in late 1990s (refs 32,33). Solid-state photopolymerization of these atmospheric ice condensates could be an important low-altitude source of macromolecular organic tholin-like material. The lower the altitude, the longer would be the wavelength of photons that could be causing photochemical activity in Titan’s atmosphere—all the way to the surface. Our laboratory simulations presented here show that photopolymerization of condensed unsaturated Titan’s volatiles indeed occurs at wavelengths at least as long as 355 nm. We conclude that contrary to the present understanding that Titan’s lower atmosphere is inert, our studies presented here show that Titan’s atmosphere is photochemically active even at lower altitudes and leads to the formation of complex tholin-like potential prebiotic molecules due to the penetrating longer wavelength photons. This is consistent with observations of Titan’s haze stretching between ~500 km and ~50 km above the surface9, containing several regions of haze (0, A, B and C) as recently characterized by the Cassini CIRS instrument34,35.

Figure 1: Three phases of molecules in Titan’s atmosphere.

Small molecules in Titan’s atmosphere could exist as isolated entities in the gas phase (left), condensed small molecules (middle) or accreted onto a larger aerosol particle (right). Gas-phase photochemistry is controlled by the molecular spectroscopic properties of the isolated molecules. In both condensed phases, additional photochemical pathways are triggered as detailed in the text.


Long-wavelength Titan aerosol analogue photochemistry

We developed a laboratory study to investigate whether solid-state polymerization of large unsaturated organic molecules condensed on Titan’s aerosols could be induced by the photons (>220 nm) that still could penetrate through its atmosphere to low altitudes. For this simulation we chose C4N2 given its known presence in Titan’s lower atmosphere30. Therefore, it also could serve as a model for other large condensed unsaturated organic compounds, particularly long linear chains of alternating single and multiple bonds, which are formed in this atmosphere. In the condensed phase, their interactions will be similar—whether between molecules with same molecular formula such as C4N2 or a statistical distribution of a wide variety of molecules with varying chain lengths. As illustrated in Fig. 2 (top), the ultraviolet absorption spectrum of C4N2 ice at 100 K has structure at <300 nm in agreement with the gas-phase spectrum36,37,38,39, but also a featureless long-wavelength absorption stretching to >360 nm, beyond where the gas-phase absorption ends. The broad continuum absorption at longer wavelengths than ~350 nm could be due to the weak singlet-triplet absorption amplified in the condensed phase, in agreement with detection of phosphorescence from the first triplet (T1) state of C4N2 at ~390 nm (ref. 40).

Figure 2: Ultraviolet-visible spectra of dicyanoacetylene ice and its photoproduct tholin.

Top: ultraviolet-visible absorption spectra of dicyanoacetylene (C4N2) solid films condensed at 100 K on a sapphire window. The gas-phase ultraviolet absorption spectrum of C4N2 (39) is shown as black curve for comparison. Bottom: ultraviolet–visible absorption difference spectra obtained by subtracting the spectrum taken before laser photolysis from the spectra measured, first during photolysis at 355 nm, then followed by photolysis at 266 nm. Sample temperature was kept at 100 K during irradiation and then, subsequent to irradiation, warmed up to 300 K under vacuum (shifted curve on the top). The ultraviolet spectrum of the residual polymer (top curve) does not change significantly between 180 and 300 K, and it is similar to that of the conventional tholin (shown as dashed line) reported by Sagan and Khare6. Spikes and wiggles in the red curve at ~500 nm are artefacts from the ultraviolet lamp profile.

Details of the laboratory simulation apparatus are summarized in Methods and further details are available in the Supplementary Material for this article. Laser photolysis experiments at the Jet Propulsion Laboratory were conducted at three wavelengths: 532, 355 and 266 nm, which were obtained by second, third and fourth harmonic generation of a 5-ns pulsed Nd-YAG. Photon fluxes used in these experiments were typically ~1 × 1017, ~3 × 1016 and ~5 × 1016 photons cm−2 s−1 at 532, 355 and 266 nm, respectively. To avoid multiphoton processes, the initial laser beam of ~3 mm diameter was expanded to ~20 mm using a 10-cm focal-length quartz lens. The experiments were designed to conserve the C4N2 that was difficult to synthesize. The C4N2 ice sample was first irradiated with the 532 nm laser for several hours at ~0.15 W cm−2 flux. No detectable change in the infrared spectra (2,244 cm−1) was observed from the photolysis at this wavelength. The same C4N2 ice was then subjected to 355 nm irradiation, which resulted in depletion of ~7% of the infrared absorption over 8 h of irradiation. As the degree of processing due to 355 nm irradiation was small, the same sample was then exposed to the 266 nm laser beam, which resulted in significantly more (a total of ~50%) depletion of the infrared absorption. In subsequent experiments, the 532 nm irradiation was omitted. We are confident that, although laser-desorption as a competing process could not be completely ruled out, it is not the dominant process. If it were, one should observe only a decrease in the monomer band and not an increase in the broad absorption that persists even after sublimation of the monomer C4N2. We also conducted several control experiments where the C4N2 ices were (a) not irradiated, (b) only irradiated with 355 nm laser, and (c) only irradiated with 266 nm laser. Unirradiated C4N2 films did not yield a residue on warm-up. Irradiation only with 266 nm laser resulted in similar photopolymerization process as with 355 nm irradiation before the 266 nm irradiation.

In both 266 nm laser and mercury (Hg) lamp photolysis experiments, the latter carried out at the University of Provence, France, the photopolymer remaining at room temperature under vacuum was similar—an orange-brown non-volatile film. A photograph of the experimental photopolymerized aerosol analogue made at the Jet Propulsion Laboratory is shown in Fig. 3. The structured vibronic absorption of condensed C4N2 ice in the ultraviolet (200–300 nm) decreases during 355 nm irradiation due to photopolymerization, whereas the broad and structure-less absorption increases, indicating photoproduct absorption/scattering to be stronger than the monomer C4N2 absorption in the ultraviolet. This trend continues with 266 nm laser photolysis (Fig. 2, bottom). Differencing spectra taken before and after the initiation of irradiation at each wavelength reveals the extent of sample processing. As shown in Fig. 4 (top), photolysis at 355 nm results in depletion of the 2,244 cm−1 band and an increase of a broader absorption around the depleted peak, also due to CN stretching of the polymer (Fig. 4, top inset). Irradiation at 266 nm resulted in a significant decrease of monomer absorption at 2,244 cm−1, but the increase in the broad absorption was not relatively as significant as in the 355 nm photolysis (Fig. 4, middle).

Figure 3: Photochemically produced tholin under simulated Titan’s lower atmospheric conditions.

Photograph of the non-volatile polymeric residue film remaining on the sapphire substrate window after warmup to 300 K under vacuum. This residue was formed during the laser photolysis of condensed C4N2 molecules at 266 nm at the Jet Propulsion Laboratory (JPL). Similar orange-brown tholin-like non-volatile polymeric residues were observed during several similar experiments at JPL and the University of Provence, France.

Figure 4: Infrared spectra of dicyanoacetylene ice and their changes during laser photolysis.

Results of the laser irradiation experiments conducted at the Jet Propulsion Laboratory (top and middle) and Hg-lamp irradiation experiments conducted at the University of Provence, France (bottom). The polymer residual spectra (middle and bottom boxes) were referenced to background spectra taken before C4N2 was deposited, whereas all the other spectra show differences between the spectra after irradiation at the specified wavelength and duration and the spectra before irradiation. Negative absorbance means depletion of the spectral feature. Positive absorbance is due to the appearance of a new spectral feature. Top: laser photolysis at 355 nm. Depletion of the absorption at 2,244 cm−1 and increase in polymer/intermediate photoproducts absorption (broad 2,235–2,250 cm−1) can clearly be seen. Middle: laser photolysis at 266 nm resulting in more significant depletion. Broad 2,215 cm−1 CN stretching band, measured at 300 K after warm-up, is the infrared spectrum for the orange-brown coloured non-volatile polymer (Fig. 3). Bottom: high-pressure Hg-lamp photolysis (photons <300 nm filtered out) showing spectra similar to 355 nm laser photolysis (top panel).

Nature of the photopolymer

During warm-up under vacuum, spectral features of non-volatile photopolymer emerge in the ultraviolet and infrared spectra at temperatures beyond the sublimation temperature of C4N2 (~160 K) to room temperature. The polymer should be forming even at 100 K during photolysis or between 100 and 160 K during the warm-up, but its spectral signatures, as they are broad, are obscured by monomer spectra before the monomer sublimes at ~160 K (Supplementary Fig. S1). For purposes of confirmation, we performed a similar C4N2 ice irradiation at the University of Provence (Marseille, France), using a conventional high-pressure Hg-lamp equipped with a <300 nm cutoff filter. The results obtained were very similar to the 355 nm laser irradiation experiments, as can be seen from the infrared spectra shown in Fig. 4 (bottom). The differences in the polymer absorption maximum when irradiated with the 266 nm laser (2,215 cm−1) or with the Hg lamp at >300 nm (2,230 cm−1), shown in Fig. 4, could be due to the difference in reaction pathways accessible for photons below 280 nm versus above 300 nm. The structure-less ultraviolet spectrum resembles more closely the tholin ultraviolet-visible spectra reported by Sagan and Khare6, shown as dashed curve in Fig. 2, than the spectra of Imanaka et al.41 On the other hand, Fourier transform infrared (FTIR) spectra in the 4,000–1,600 cm−1 region are similar (Fig. 5) to the infrared spectra of discharge-generated polymer reported by Imanaka et al.41,42 In spite of the difference in preparation methods (gas-phase discharge at various pressures versus condensed-phase photochemistry) and the initial conditions (N2+CH4 versus C4N2), these qualitative similarities in the optical properties of the non-volatile polymer (tholin) reveal that these materials have very similar chemical structures. The actual structural properties of tholins are not known and are expected to be diverse, both at the molecular structure (chemical bonding) level and at the supramolecular structure (three-dimensional polymer structures) level. We prefer not to over interpret these data, but to show that tholins—though could have similar spectral properties may have diverse molecular and supramolecular aerosol structures.

Figure 5: A comparison of the infrared spectra of tholins synthesized in the gas and condensed phases.

Infrared spectra of tholin-like photopolymers at room temperature compared with tholins made from conventional discharge experiments by Imanaka41,42. Method of preparation of tholin, bottom to top (ad): JPL 266 nm laser photolysis (a); Marseille Hg lamp (>300 nm) pholysis (b); 10% methane in nitrogen discharge41 at 26 Pa (c) and at 160 Pa (d). An excellent comparison between longer wavelength photochemical polymer spectra (JPL: 266 nm; Marseille >300 nm) and with the discharge-made tholins spectra can be seen. In our spectra the ratio of CN to CH and NH, band strengths is different (more CN) compared to Imanaka’s data, because in our experiments far-less hydrogen is available (either as traces of H2O impurity, or intentionally added H2O or other hydrocarbons such as CH4 or C2H2). *Gas-phase CO2 residual absorption.

In the condensed phase, in addition to normal spin-allowed ultraviolet absorption, photochemical reactions can also occur through absorption of light at longer wavelengths directly into the triplet-excited states, which have strong radical character. In the case of C4N2, the spin-allowed ultraviolet absorption occurs at <300 nm and spin-forbidden absorption occurs at >300 nm—hence very efficient photodepletion of monomer at 266 nm compared to irradiation at 355 nm (Fig. 2). Larger unsaturated organics condensed onto aerosols likely have both spin-allowed strong and spin-forbidden (condensed-phase enhanced) weak photoabsorptions and similar solid-state photoprocessing potential. It is known that gas-phase C4N2 could dissociate with 248 nm light43,44 resulting in the formation of CN and the CCCN radicals. Hence, the 266 nm photochemistry is likely to be controlled by dissociation products.


Results discussed above indicate that singlet-triplet absorption-driven (355 nm irradiation) photochemical processes involves triplet C4N2 molecules reacting with other C4N2 molecules in its surrounding, resulting in the formation of the photopolymer (Fig. 6), whose CN stretching vibrational absorption remains around 2,244 cm−1, but is much broader. Upon warm-up this band shifts to 2,225 cm−1, once the monomer is sublimed above 160 K. On the other hand, singlet-excitation-driven (<280 nm) photochemical processes result in molecular dissociation of C4N2 into C3N and CN radicals as well as photopolymerization (Fig. 6). The dissociation products recombine and react with other molecules during the warm-up until the monomer C4N2 sublimes, at which time the polymer absorption ~2,215 cm−1 can clearly be seen. These mechanisms, qualitatively highlighted in Fig. 6, would be applicable to mixed cyanopolyynes and polyynes, known to be present in Titan’s atmosphere. Both ultraviolet and infrared spectra of the polymer do not change significantly between 180 and 300 K, once the volatile monomer has evaporated above 160 K. Slight shifts in the broad absorption maxima of the polymer in 266 nm laser, 355 nm laser and >300 nm Hg-lamp studies, 2,215 cm−1, 2,225 cm−1, 2,230 cm−1, respectively, could be due to different local environments around the –CN functional group of the photopolymer. It is known that the CN stretching frequency shifts based on the structural environment around it—less or more polar and less or more hydrogen bonding45.

Figure 6: Possible reaction pathways for longer wavelength production of tholins in condensed phase.

Proposed mechanisms for the longer wavelength (ultraviolet-visible photons) triplet excitation-driven and shorter wavelength (ultraviolet photons) singlet-excitation-driven photopolymerization of C4N2 in the condensed aerosol phase. Broken lines are not bonds, but represent new bond formation in progress. Radical centers are not specifically shown to avoid congestion in structures. While longer wavelengths result in more uniform polymerization, shorter wavelengths result in dissociation of parent C4N2 to C3N and CN radicals that react to form a wide distribution of polymers. In both cases, monomer molecules accreted on an existing aerosol particle (Fig. 1) could chemically bind to this haze particle, increasing its size and modifying it chemically on its surface—a process that could be critical to Titan’s atmospheric chemistry, but not considered previously.

In our studies presented here, during the photolysis and warm-up, additional reactions with traces of H2O impurity, or intentionally added H2O, or other hydrocarbons such as CH4 or C2H2, result in the formation of CH and NH functional groups into the polymer, whose spectra at room temperature are very similar to the tholin infrared spectra made from conventional discharge experiments41 (Fig. 5). Based on this observation, we conclude that the intermediate photoproducts are very reactive towards hydrogen-containing molecules. Though water is sparse, hydrocarbons are abundant on Titan and similar photochemical processes are expected to occur in the Titan’s atmosphere.

In addition, we investigated the efficiency of photoprocessing by monitoring the time evolution of the C4N2 infrared absorption on irradiation at 355 and 266 nm. Figure 7 shows the change in C4N2 infrared absorption with exposure time. The change during 355 nm irradiation is linear with photon flux (dose), indicating that the photochemistry is due to weak electronic transitions (singlet-triplet), falling in a small linear segment of a first-order reaction (only ~13% depletion in ~1,300 min) that would have developed into a nonlinear exponential behaviour on prolonged photolysis. Continuing with the photolysis at 266 nm resulted in more rapid depletion of C4N2, following a single exponential behaviour, in accordance with first-order exponential process46 (a total of ~48% depletion after 860 min irradiation at 266 nm).

Figure 7: Photodepletion kinetics of dicyanoacetylene ice.

Time variation of change in absorption at 2,244 cm−1 when C4N2 film at 100 K is photolysed at 355 nm (inset) and 266 nm. As expected for a forbidden and weak singlet-triplet absorption-induced photochemistry, the depletion of C4N2 is linearly proportion to the irradiation time when exposed at 355 nm, representing initial stages of an exponential process. Only 14% of C4N2 was depleted after ~1,400 min irradiation at ~50 mW cm−2. The last three points on the lower curve (filled squares) were obtained using higher laser power (160 mW cm−2 or 8 mJ per pulse), whereas the rest of the data were derived using a 50 mW cm−2 (2.5 mJ per pulse) laser power. Linearity of this curve when fluence is converted to time clearly indicates that the 355 nm photochemistry is a one-photon process. We also plotted these three points with 160 mW cm−2 laser power separately (filled circles). As discussed in the text, the slopes of these two curves scale linearly with the laser fluencies—confirming that the 355 nm photochemistry is indeed a one-photon process. The 266 nm photolysis through singlet-singlet excitation follows a monoexponential curve with over 35% depletion within the first 800 min of irradiation at 120 mW cm−2. Extrapolation towards the longer durations of the 266 nm photolysis may not be accurate due to simultaneous increase in extinction of the film at this wavelength from the formation of new products.

We also conducted experiments to rule out the possibility whether multiphoton processes could have resulted in the observed photochemistry. The experiments conducted in France were conducted using a 150 W high-pressure Mercury lamp that was flooded (without focusing) on the sample after cutting out the shorter wavelengths below 300 nm using a glass filter. These results are very similar to the results from defocused laser irradiation. Further, we changed the pulse energy (EL) of 355 nm laser by a factor of 3 (from 50 to 160 mW cm−2 before defocusing the laser), keeping the repetition rate at 20 Hz. The photolysis yields (φ) plotted in the insert of Fig. 7 (after converting normalizing photon flux to time) fall linearly on the curve at the last three-irradiation points. Also plotted in Fig. 7 are the photolysis yields for 160 mW cm−2 irradiation (the last four points on the main curve). The slopes of these two curves give the photolysis yields per minute at these two laser fluencies. While a single-photon process follows the equation (φ)=k × EL; a two-photon process obeys a quadratic dependence (φ)=k′ × (EL)2. Ratios of photolysis yields at two laser fluencies EL1 and EL2 should follow (φ12)=(EL1/EL2) for single-photon process and (EL1/EL2)2 for a two-photon process. The laser fluence ratio (160 mW/50 mW) is 3.2 for single-photon and 10.24 for two-photon processes. The observed photolysis yield ratio (φ12) of 3.15 (Fig. 7) clearly demonstrates that the photoabsorption and the photochemistry with 355 nm laser irradiation presented here are linear one-photon processes, not involving nonlinear multiphoton processes. Laser irradiation at 266 nm is done under similar conditions (~0.12 W cm−2 before defocusing) and we infer a single-photon-induced photochemical process at this wavelength as well.

Under our experimental conditions (~10−9 mbar vacuum) C4N2 starts to sublime around 160 K. No sign of sublimation is detected at 100 K. Based on these observations, for similar monomer molecules, we expect the sticking coefficient in Titan’s atmosphere at much higher pressures and similar temperatures to be close to unity. Experimental data presented here demonstrate that solar radiation at wavelengths that penetrate deep into Titan’s atmosphere, down to 200 km and below, can initiate a new source of tholin-like haze production from the condensates in this altitude range. As the sedimentation velocity in this region is very slow, of order ~0.03 cm s−1 at ~100 km altitude22, aerosol particles stay within the haze layer for ~10 Earth years or ~3 × 108 s. Solar photon flux at 10 AU is ~14 W m−2 and photons between 200 and 350 nm constitute ~5% of the total energy flux, resulting in ~0.7 or 7 × 10−5 W cm−2 or ~1014 photons cm−2 s−1 (over 200–350 nm) or ~6 × 1011 photons cm−2 s−1 nm−1. The laboratory dose was typically 0.15 W cm−2, which amounts to ~2,000 times more flux than received by Titan’s atmosphere at these wavelengths. As seen in Fig. 7, photochemical polymerization at 355 nm of a condensed C4N2 film (~200 nm thick) is ~13% over 1,340 min (84,000 s) and 0.05 W cm−2 flux, which corresponds to ~6 × 107 s on Titan, which is a factor of 5 less time that an aerosol particle spends in Titan’s atmosphere. So significant photopolymerization processing in Titan’s atmosphere is possible from weakly allowed spin-forbidden photoexcitations, resulting in solid-state radical reactions. On the other hand, photopolymerization due to 266 nm photons, caused by strongly allowed photoexcitation, occurs much faster, ~35% yield over 860 min (21,600 s) at 0.12 W cm−2, which corresponds to ~4 × 107 s on Titan, an order of magnitude less than the residence time of aerosols in Titan’s condensed haze layer. Based on these data we infer that significant photochemical polymerization is expected to occur involving spin-allowed strong ultraviolet absorption by Titan’s aerosol molecules.

Chemical models predict the formation of unsaturated organic molecules even larger than C4N2 in Titan’s atmosphere47. As with C4N2, the larger molecules will condense into ices in the lower atmosphere. The gas-phase spectra of such molecules will have absorption longward of the C4N2 gas-phase absorption, and in condensed phase these absorption spectra would be shifted to even longer wavelengths. Therefore, solar radiation out to visible wavelengths penetrating to Titan’s lower atmosphere may initiate production of photopolymerization of condensed organic aerosols not previously accounted for and can provide a mechanism for the majority of tholin formation predicted to occur at low altitudes. We conclude that Titan’s lower atmosphere is more photochemically active than so far assumed. In addition, experimental results presented here can be extrapolated to shorter wavelength solar radiation at higher altitudes, exposure to which should lead to condensed-phase processing of accumulations of unsaturated organic molecules as previously suggested11,12. Thus, tholin-like haze formation occurs by a variety of different photo-initiated processes throughout the whole atmospheric column of Titan.


Titan organic aerosol synthesis and photochemistry experiment

Dicyanoacetylene (C4N2) was synthesized according to a well-established procedure reported in the literature48,49. These molecules are highly unstable and hazardous. Hence we developed a synthesis laboratory adjacent to the spectroscopy and photochemistry lab. C4N2 was prepared and used immediately to make ice films at 100 K. During the vapour deposition of C4N2 on the cryogenic window (Sapphire or KBr, both transmit ultraviolet and infrared for the CN stretch around 2,244 cm−1, sapphire cutoff is ~1,600 cm−1, whereas KBr is transparent down to 450 cm−1), the sample window was kept at 100 K. Bulk C4N2 was kept at around −30 °C during the sublimation into the ice chamber and subsequently after the preparation of ice films, the C4N2 container was removed from the vacuum line and was stored in an −80 °C ice chest or in a dry-ice container.

Details of the experimental system are shown in Supplementary Figs S2 and S3. The experimental system in which thin films of C4N2 ices were generated consisted of a closed-cycle helium cryostat (Advanced Research Systems) that cooled the substrate window (Sapphire or KBr). C4N2 was deposited from gas phase onto the window cooled to 100 K, a temperature relevant to Titan’s lower atmosphere. All the irradiation experiments were done at 100 K, and at the end of the experiments temperature was raised at 5 K min−1 to room temperature. Infrared spectra were collected during the entire warm-up. Optical configuration of the substrate, FTIR, fibre optics ultraviolet-visible spectrometers and irradiation lasers were such that sample was not moved during simulataneous ultraviolet and infrared spectral measurements or during laser irradiation (Supplementary Fig. S3). Growth of C4N2 films were controlled such that the 2,244 cm−1 infrared absorption band reached an absorbance of ~0.1. This process ensured that enough material was deposited to allow measurable photoprocessing, but not too much material that would result in nonlinear absorption properties (>1.0 Abs) or scattering. Both the laser beam and the infrared beam from the FTIR spectrometer illuminated the whole ~20 mm sapphire window and the C4N2 film, while ultraviolet-visible spectra were collected from a ~5 mm diameter area in the centre of the window. To avoid inducing additional photoprocessing due to ultraviolet light that may interfere with the kinetic analysis, we did not monitor the sample evolution using ultraviolet spectra, but instead used the mid-infrared band at 2,244 cm−1. We used the sapphire window for its excellent optical quality in the ultraviolet-visible spectral region (>180 nm) all the way into the mid-infrared (>1,600 cm−1), enabling simultaneous ultraviolet and infrared spectroscopy. In few experiments we used KBr substrate, gaining access to the infrared (>500 cm−1) at the cost of ultraviolet spectra. In these studies, other strong infrared bands of C4N2 (738 and 1,160 cm−1) with relative peak heights of ~10% compared with the 2,244 cm−1 band, as well as a number of very weak combination bands between 2,250 and 3,400 cm−1 were observed (Supplementary Fig. S4), in accordance with earlier studies of C4N2 in Ar matrices50. For this reason, we used the strongest 2,244 cm−1 CN asymmetric stretch band for quantitative data analysis. Ultraviolet and FTIR spectra were measured on C4N2 ice at 100 K simultaneously on the same sample around the same time, enabling a good comparison between the ultraviolet and infrared spectra. While increasing scattering was observed with increasing ice thickness in the FTIR spectra, ultraviolet spectra were a convolution of electronic absorption and interference due to reflections caused by the C4N2 ice film on the sapphire window. These interference modulations were used to derive film thickness assuming a refractive index of 1.45, typical of many refractory organics such as polycyclic aromatic hydrocarbons (PAHs).

Laser and lamp photochemistry

A Nd-YAG laser (Quantel Brio) with second, third and fourth harmonic generation at 532, 355 and 266 nm was used for photochemistry. Laser light was defocused as explained below to avoid multiphoton processes such as resonance-enhanced multiphoton ionization or two-photon excitation into electronically excited states. Under solar radiation conditions such multiphoton absorption processes are negligible and in the laboratory these processes must be avoided to have a valid Titan simulation. The diameter of laser light was initially ~5 mm. A 10 cm focal length quartz biconvex lens was placed at ~50 cm from the cryostat to result in a beam diameter of ~20 mm on the optical window containing C4N2 sample. Photon fluxes used in these experiments were typically ~1 × 1017, ~3 × 1016 and ~5 × 1016 photons cm−2 s−1 at 532, 355 and 266 nm, respectively, before defocusing. A ultraviolet-visible absorption spectrograph (Ocean Optics USB4000) was used to detect optical changes between 200 and 1,000 nm, a FTIR spectrometer (Thermo Nicolet 6700) covering 1 micron to 20 microns (10,000 to 500 cm−1), sapphire substrate cutoff ~1,600 cm−1. Though the substrate window could be rotated around 360° in the vacuum chamber, to enhance the accuracy of spectral changes, the organic film substrate window was kept in the same position during the entire experiment (after initial deposition) enabling simultaneous laser irradiation, ultraviolet and infrared spectral measurements.

Additional information

How to cite this article: Gudipati, M. S. et al. Photochemical activity of Titan’s low-altitude condensed haze. Nat. Commun. 4:1648 doi: 10.1038/ncomms2649 (2013).


  1. 1

    Lane, A. L. et al. Photopolarimetry from Voyager-2—preliminary-results on Saturn, Titan, and the rings. Science 215, 537–543 (1982).

    CAS  ADS  Article  Google Scholar 

  2. 2

    Rannou, P. et al. Titan haze distribution and optical properties retrieved from recent observations. Icarus 208, 850–867 (2010).

    CAS  ADS  Article  Google Scholar 

  3. 3

    Stephan, K. et al. Specular reflection on Titan: liquids in Kraken Mare. Geophys. Res. Lett. 37, 5 (2010).

    Article  Google Scholar 

  4. 4

    Lorenz, R. D. et al. The sand seas of Titan: Cassini RADAR observations of longitudinal dunes. Science 312, 724–727 (2006).

    CAS  ADS  Article  Google Scholar 

  5. 5

    Khare, B. N. et al. Amino-acids derived from Titan tholins. Icarus 68, 176–184 (1986).

    CAS  ADS  Article  Google Scholar 

  6. 6

    Sagan, C. & Khare, B. N. Tholins—organic-chemistry of inter-stellar grains and gas. Nature 277, 102–107 (1979).

    CAS  ADS  Article  Google Scholar 

  7. 7

    Vuitton, V., Yelle, R. V., Lavvas, P. & Klippenstein, S. J. Rapid association reactions at low pressure: impact on the formation of hydrocarbons on Titan. Astrophys. J. 744, Article No. 11 (2012).

    ADS  Article  Google Scholar 

  8. 8

    Lavvas, P., Sander, M., Kraft, M. & Imanaka, H. Surface chemistry and particle shape: processes for the evolution of aerosols in Titan’s atmosphere. Astrophys. J. 728, Article No. 80 (2011).

    ADS  Article  Google Scholar 

  9. 9

    West, R. A. et al. The evolution of Titan's detached haze layer near equinox in 2009. Geophys. Res. Lett. 38, Article No. L06204 (2011).

    ADS  Article  Google Scholar 

  10. 10

    Tomasko, M. G. et al. A model of Titan’s aerosols based on measurements made inside the atmosphere. Planet Space Sci. 56, 669–707 (2008).

    ADS  Article  Google Scholar 

  11. 11

    Dimitrov, V. & Bar-Nun, A. Aging of Titan’s aerosols. Icarus 156, 530–538 (2002).

    CAS  ADS  Article  Google Scholar 

  12. 12

    Dimitrov, V. & Bar-Nun, A. Hardening of Titan’s aerosols by their charging. Icarus 166, 440–443 (2003).

    CAS  ADS  Article  Google Scholar 

  13. 13

    Liang, M.-C., Yung, Y. L. & Shemansky, D. E. Photolytically generated aerosols in the mesosphere and thermosphere of Titan. Astrophys. J. 661, L199–L202 (2007).

    CAS  ADS  Article  Google Scholar 

  14. 14

    Lavvas, P. P., Coustenis, A. & Vardavas, I. M. Coupling photochemistry with haze formation in Titan’s atmosphere, Part II: results and validation with Cassini/Huygens data. Planet Space Sci. 56, 67–99 (2008).

    CAS  ADS  Article  Google Scholar 

  15. 15

    Lavvas, P., Griffith, C. A. & Yelle, R. V. Condensation in Titan’s atmosphere at the Huygens landing site. Icarus 215, 732–750 (2011).

    CAS  ADS  Article  Google Scholar 

  16. 16

    Lavvas, P. et al. Energy deposition and primary chemical products in Titan’s upper atmosphere. Icarus 213, 233–251 (2011).

    CAS  ADS  Article  Google Scholar 

  17. 17

    Toublanc, D. et al. Photochemical modeling of titans atmosphere. Icarus 113, 2–26 (1995).

    CAS  ADS  Article  Google Scholar 

  18. 18

    Wilson, E. H. & Atreya, S. K. Current state of modeling the photochemistry of Titan’s mutually dependent atmosphere and ionosphere. J. Geophys. Res.-Planets 109, Article No. E06002 (2004).

    ADS  Article  Google Scholar 

  19. 19

    Anderson, C. M. & Samuelson, R. E. Titan's aerosol and stratospheric ice opacities between 18 and 500 μm: vertical and spectral characteristics from Cassini CIRS. Icarus 212, 762–778 (2011).

    CAS  ADS  Article  Google Scholar 

  20. 20

    Teanby, N. A. et al. Titan’s stratospheric C2N2, C3H4, and C4H2 abundances from Cassini/CIRS far-infrared spectra. Icarus 202, 620–631 (2009).

    CAS  ADS  Article  Google Scholar 

  21. 21

    Vuitton, V., Yelle, R. V. & Cui, J. Formation and distribution of benzene on Titan. J. Geophys. Res.-Planets 113, Article No. E05007 (2008).

    ADS  Article  Google Scholar 

  22. 22

    Lavvas, P., Yelle, R. V. & Griffith, C. A. Titan’s vertical aerosol structure at the Huygens landing site: constraints on particle size, density, charge, and refractive index. Icarus 210, 832–842 (2010).

    CAS  ADS  Article  Google Scholar 

  23. 23

    Pilling, S., Andrade, D. P. P., Neto, A. C., Rittner, R. & de Brito, A. N. DNA nucleobase synthesis at Titan atmosphere analog by soft X-rays. J. Phys. Chem. A 113, 11161–11166 (2009).

    CAS  Article  Google Scholar 

  24. 24

    Cable, M. L. et al. Titan tholins: simulating Titan organic chemistry in the Cassini-Huygens era. Chem. Rev. 112, 1882–1909 (2011).

    Article  Google Scholar 

  25. 25

    Raulin, F., Brasse, C., Poch, O. & Coll, P. Prebiotic-like chemistry on Titan. Chem. Soc. Rev. 41, 5380–5393 (2012).

    CAS  Article  Google Scholar 

  26. 26

    Marcus, R. A. On theory of shifts and broadening of electronic spectra of polar solutes in polar media. J. Chem. Phys. 43, 1261–126 (1965).

    CAS  ADS  Article  Google Scholar 

  27. 27

    Gudipati, M. S. Exciton, exchange, and through-bond interactions in multichromophoric molecules: an analysis of the electronic excited states. J. Phys. Chem. 98, 9750–9763 (1994).

    CAS  Article  Google Scholar 

  28. 28

    Kasha, M. Characterization of electronic transitions in complex molecules. Discuss Faraday Soc. 9, 14–19 (1950).

    Article  Google Scholar 

  29. 29

    Klessinger, M. & Michl, J. Excited States and Photochemistry of Organic Molecules VCH (1995).

  30. 30

    Samuelson, R. E., Mayo, L. A., Knuckles, M. A. & Khanna, R. J. C4N2 ice in Titan’s north polar stratosphere. Planet Space Sci. 45, 941–948 (1997).

    CAS  ADS  Article  Google Scholar 

  31. 31

    Coustenis, A., Schmitt, B., Khanna, R. K. & Trotta, F. Plausible condensates in Titan’s stratosphere from Voyager infrared spectra. Planet Space Sci. 47, 1305–1329 (1999).

    CAS  ADS  Article  Google Scholar 

  32. 32

    Coll, P., Guillemin, J. C., Gazeau, M. C. & Raulin, F. Report and implications of the first observation of C4N2 in laboratory simulations of Titan’s atmosphere. Planet Space Sci. 47, 1433–1440 (1999).

    CAS  ADS  Article  Google Scholar 

  33. 33

    Khlifi, M. et al. Gas infrared spectra, assignments, and absolute IR band intensities of C4N2 in the 250–3500, cm(−1) region: implications for Titan’s stratosphere. Spectrochim. Acta A—Mol. Biomol. Spectrosc. 53, 707–712 (1997).

    ADS  Article  Google Scholar 

  34. 34

    de Kok, R., Irwin, P. G. J. & Teanby, N. A. Far-infrared opacity sources in Titan’s troposphere reconsidered. Icarus 209, 854–857 (2010).

    CAS  ADS  Article  Google Scholar 

  35. 35

    de Kok, R. et al. Characteristics of Titan’s stratospheric aerosols and condensate clouds from Cassini CIRS far-infrared spectra. Icarus 191, 223–235 (2007).

    ADS  Article  Google Scholar 

  36. 36

    Fischer, G., Johnson, G. D., Ramsay, D. A. & Ross, I. G. Electronic spectrum of dicyanoacetylene. 2. Interpretation of the 2800 A transition. J. Phys. Chem. A 107, 10637–10641 (2003).

    CAS  Article  Google Scholar 

  37. 37

    Fischer, G. & Ross, I. G. Electronic spectrum of dicyanoacetylene. 1. Calculations of the geometrics and vibrations of ground and excited states of diacetylene, cyanoacetylene, cyanogen, triacetylene, cyanodiacetylene, and dicyanoacetylene. J. Phys. Chem. A 107, 10631–10636 (2003).

    CAS  Article  Google Scholar 

  38. 38

    Miller, F. A. & Hannan, R. B. The ultraviolet absorption spectrum of dicyanoacetylene. Spectrochim. Acta 12, 321–331 (1958).

    CAS  ADS  Article  Google Scholar 

  39. 39

    Benilan, Y. et al. Temperature dependence of HC3N, C6H2, and C4N2 mid-UV absorption coefficients. Application to the interpretation of Titan's atmospheric spectra. Astrophys. Space Sci. 236, 85–95 (1996).

    CAS  ADS  Article  Google Scholar 

  40. 40

    Smith, A. M., Schallmoser, G., Thoma, A. & Bondybey, V. E. Infrared spectral evidence of Nc-Cc-Nc—photoisomerization of Nc-Cc-Cn in an Argon matrix. J. Chem. Phys. 98, 1776–1785 (1993).

    CAS  ADS  Article  Google Scholar 

  41. 41

    Imanaka, H. et al. Laboratory experiments of Titan tholin formed in cold plasma at various pressures: implications for nitrogen-containing polycyclic aromatic compounds in Titan haze. Icarus 168, 344–366 (2004).

    CAS  ADS  Article  Google Scholar 

  42. 42

    Imanaka, H., Cruikshank, D. P., Khare, B. N. & McKay, C. P. Optical constants of Titan tholins at mid-infrared wavelengths (2.5–25 μm) and the possible chemical nature of Titan’s haze particles. Icarus 218, 247–261 (2012).

    CAS  ADS  Article  Google Scholar 

  43. 43

    Kolos, R., Zielinski, Z., Grabowski, Z. R. & Mizerski, T. Dicyanoacetylene photodissociation at 193-nm and at 248-nm studied by transient absorption-spectroscopy—production of CN, C2 and C3N. Chem. Phys. Lett. 180, 73–80 (1991).

    CAS  ADS  Article  Google Scholar 

  44. 44

    Crepin, C. et al. UV-induced growth of cyanopolyyne chains in cryogenic solids. Phys. Chem. Chem. Phys. 13, 16780–16785 (2011).

    CAS  Article  Google Scholar 

  45. 45

    Lindquist, B. A. & Corcelli, S. A. Nitrile groups as vibrational probes: calculations of the CN infrared absorption line shape of acetonitrile in water and tetrahydrofuran. J. Phys. Chem. B 112, 6301–6303 (2008).

    CAS  Article  Google Scholar 

  46. 46

    Atkins, P. & de Paula, J. Atkins’ Physical Chemistry 9th edn Oxford University Press (2009).

  47. 47

    Lavvas, P. P., Coustenis, A. & Vardavas, I. M. Coupling photochemistry with haze formation in Titan’s atmosphere, part I: Model description. Planet Space Sci. 56, 27–66 (2008).

    CAS  ADS  Article  Google Scholar 

  48. 48

    Coupeaud, A., Pietri, N., Couturier-Tamburelli, I. & Aycard, J. P. NC4NC2: a new isomer of dicyanodiacetylene isolated in a cryogenic matrix. Chem. Phys. Lett. 416, 349–353 (2005).

    CAS  ADS  Article  Google Scholar 

  49. 49

    Ciganek, E. & Krespan, C. G. Syntheses of dicyanoacetylene. J. Organic Chem. 33, 541–554 (1968).

    CAS  Article  Google Scholar 

  50. 50

    Guennoun, Z., Couturier-Tamburelli, I., Pietri, N. & Aycard, J. P. UV photoisomerisation of cyano and dicyanoacetylene: the first identification of CCNCH and CCCNCN isomers—matrix isolation, infrared and ab initio study. Chem. Phys. Lett. 368, 574–583 (2003).

    CAS  ADS  Article  Google Scholar 

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The Jet Propulsion Laboratory (JPL) part of the work is partly supported by several of the following funding sources: NASA Astrobiology Institute team ‘Titan as a Prebiotic Chemical System’, the Jet Propulsion Laboratory Director’s Research and Development Fund and the JPL Research and Technology Development funding for the infrastructure of the Ice Spectroscopy Laboratory (ISL) and Titan organic aerosol spectroscopy and chemistry (TOAST) laboratory at JPL. The University of Provence part of the work was funded by the French national program Environnements Planétaires et Origines de la Vie (EPOV). This research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.

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M.S.G. and M.A. conceived the research ideas and wrote a significant part of the publication. M.S.G. coordinated the research activity, put the team together, involved in conducting the experiments, data analysis and data interpretation. R.J. and A.L. contributed to build infrastructure of the laboratory needed to synthesize the materials, conducted synthesis under the guidance of I.C. and majority of experiments described in this publication under the guidance of M.G. I.C. conducted the research in Marseille, France, as well as guided the synthesis and a part of photochemical investigations at JPL. R.J. performed the work as a NASA Post Doctoral Fellow at the Jet Propulsion Laboratory. A.L. performed a part of this work at the Jet Propulsion Laboratory during Academy of Finland fellowship.

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Correspondence to Murthy S. Gudipati.

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Gudipati, M., Jacovi, R., Couturier-Tamburelli, I. et al. Photochemical activity of Titan’s low-altitude condensed haze. Nat Commun 4, 1648 (2013).

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