# Experimental investigations of diacetylene ice photochemistry in Titan's atmospheric conditions

Benjamin Fleury, Murthy Gudipati, Isabelle Couturier-Tamburelli

► To cite this version:

Benjamin Fleury, Murthy Gudipati, Isabelle Couturier-Tamburelli. Experimental investigations of diacetylene ice photochemistry in Titan's atmospheric conditions. Astronomy and Astrophysics - A&A, 2024, 684, pp.A1. 10.1051/0004-6361/202348658. hal-04529416

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https://hal.science/hal-04529416

Submitted on 3 Apr 2024

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Distributed under a Creative Commons Attribution 4.0 International License
# Experimental investigations of diacetylene ice photochemistry in Titan's atmospheric conditions

Benjamin Fleury, Murthy Gudipati, Isabelle Couturier-Tamburelli

► To cite this version:

Benjamin Fleury, Murthy Gudipati, Isabelle Couturier-Tamburelli. Experimental investigations of diacetylene ice photochemistry in Titan's atmospheric conditions. Astronomy & Astrophysics - A&A, 2024, 684, pp.A1. 10.1051/0004-6361/202348658. [hal-04529416](https://hal.science/hal-04529416v1)

HAL Id: hal-04529416

https://hal.science/hal-04529416v1

Submitted on 3 Apr 2024

HAL is a multi-disciplinary open access
archive for the deposit and dissemination of sci-
entific research documents, whether they are pub-
lished or not. The documents may come from
teaching and research institutions in France or
abroad, or from public or private research centers.

L'archive ouverte pluridisciplinaire HAL, est
destinée au dépôt et à la diffusion de documents
scientifiques de niveau recherche, publiés ou non,
émanant des établissements d'enseignement et de
recherche français ou étrangers, des laboratoires
publics ou privés.

<figure><img src="image_1.png" /></figure>

Distributed under a Creative Commons Attribution 4.0 International License
# Experimental investigations of diacetylene ice photochemistry in Titan's atmospheric conditions

Benjamin Fleury<sup>1,2</sup>✉, Murthy S. Gudipati<sup>2</sup>✉, and Isabelle Couturier-Tamburelli<sup>3</sup>

Received 17 November 2023 / Accepted 31 January 2024

## ABSTRACT

**Context.** A large fraction of the organic species produced photochemically in the atmosphere of Titan can condense to form ice particles in the stratosphere and in the troposphere. According to various studies, diacetylene ($C_4H_2$) condenses below 100 km where it can be exposed to ultraviolet radiation.

**Aims.** We studied experimentally the photochemistry of diacetylene ice ($C_4H_2$) to evaluate its potential role in the lower altitude photochemistry of Titan's atmospheric ices.

**Methods.** $C_4H_2$ ice films were irradiated with near-ultraviolet (near-UV) photons ($\lambda > 300$ nm) with different UV sources to assess the impact of the wavelengths of photons on the photochemistry of $C_4H_2$. The evolution of the ice's composition was monitored using spectroscopic techniques.

**Results.** Our results reveal that diacetylene ice is reactive through singlet-triplet absorption, similar to the photochemistry of other organic ices of Titan (such as dicyanoacetylene $C_4N_2$ ice) that we investigated previously. Several chemical processes occurred during the photolysis: the hydrogenation of $C_4H_2$ to form other $C_4$ hydrocarbons (vinylacetylene $C_4H_4$ to butane $C_4H_{10}$); the formation of larger and highly polymerizable hydrocarbons, such as triacetylene ($C_6H_2$); and the formation of an organic polymer that is stable at room temperature.

**Conclusions.** The nondetection of diacetylene ice in Titan's atmosphere or surface could be rationalized based on our experimental results that $C_4H_2$ is photochemically highly reactive in the solid phase when exposed to near-UV radiation that reaches Titan's lower altitudes and surface. $C_4H_2$ may be one of the key molecules promoting the chemistry in the ices and aerosols of Titan's haze layers, especially in the case of co-condensation with other organic volatiles, with which it could initiate more complex solid-phase chemistry.

**Key words.** astrochemistry – methods: laboratory: molecular – techniques: spectroscopic – planets and satellites: atmospheres – ultraviolet: planetary systems

## 1. Introduction

The complex organic chemistry initiated in Titan's thermosphere and ionosphere by solar photons and energetic particles of Saturn's magnetosphere leads to the production of many volatile organics as well as organic aerosols (Lavvas et al. 2013; Liang et al. 2007; Waite et al. 2007). The decrease in temperature from the stratosphere to the tropopause (Fulchignoni et al. 2005) allows the direct condensation of many volatiles (hydrocarbons and nitriles), thus forming ice particles or ice accreted on organic aerosols (Anderson et al. 2016; Barth 2003, 2017; de Kok et al. 2008; Frère et al. 1990; Lavvas et al. 2011; Mayo & Samuelson 2005; Raulin & Owen 2002; Sagan & Reid Thompson 1984; Samuelson & Mayo 1991; Samuelson et al. 1997).

Gas molecules and organic hazes in Titan's atmosphere significantly attenuate high-energy photons. As a result, only longer-wavelength photons make it through the stratosphere and the troposphere and eventually to the surface of Titan. Vuitton et al. (2019) model the flux of photons from 1.5 to 300 nm as a function of the altitude in the atmosphere of Titan. According to their work, photons with wavelengths shorter than 150 nm do not penetrate below ~200 km, while photons in the 150 to 200 nm range are progressively absorbed from ~200 km to

~100 km. Finally, only photons in the 200–300 nm range penetrate below 100 km, down to ~50 km. Our recent experimental studies have demonstrated that these longer-wavelength (200 nm and above) ultraviolet (UV) photons could efficiently drive the photochemistry of ices, resulting in the production of organic polymers (Couturier-Tamburelli et al. 2014, 2015; Gudipati et al. 2013; Mouzay et al. 2021a,b) and to the photochemically driven incorporation of these molecules into existing haze particles (Couturier-Tamburelli et al. 2018; Fleury et al. 2019).

Our previous studies of pure-ice photochemistry in Titan's atmosphere were focused on acetylene ($C_2H_2$), benzene ($C_6H_6$), and some nitriles (hydrogen cyanide HCN, cyanoacetylene $HC_3N$, dicyanoacetylene $C_4N_2$, and cyanodiacetylene $HC_5N$), as these species represent the composition of most identified ice clouds (Anderson & Samuelson 2011; Anderson et al. 2010, 2018b; de Kok et al. 2014; Khanna et al. 1987; Samuelson et al. 1997). However, higher hydrocarbons may also condense in Titan's stratosphere, as highlighted by the recent identification of ice clouds that contain benzene at Titan's south pole (Vinatier et al. 2018) and by the discovery by the Cassini Composite InfraRed Spectrometer (CIRS) of the High Altitude South Polar (HASP) cloud (Anderson et al. 2018b) whose spectral signature is consistent with co-condensed HCN-$C_6H_6$ ices

<footnote n="1">¹ Université Paris Cité and Univ Paris Est Creteil, CNRS, LISA, 75013 Paris, France
e-mail: benjamin.fleury@lisa.ipsl.fr</footnote>

<footnote n="2">² Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA</footnote>

<footnote n="3">³ Aix-Marseille Université, CNRS, PIIM, UMR 7345, 13013 Marseille, France
e-mail: isabelle.couturier@univ-amu.fr</footnote>
# Experimental investigations of diacetylene ice photochemistry in Titan's atmospheric conditions

Benjamin Fleury<sup>1,2</sup>✉, Murthy S. Gudipati<sup>2</sup>✉, and Isabelle Couturier-Tamburelli<sup>3</sup>

Received 17 November 2023 / Accepted 31 January 2024

## ABSTRACT

**Context.** A large fraction of the organic species produced photochemically in the atmosphere of Titan can condense to form ice particles in the stratosphere and in the troposphere. According to various studies, diacetylene ($C_4H_2$) condenses below 100 km where it can be exposed to ultraviolet radiation.

**Aims.** We studied experimentally the photochemistry of diacetylene ice ($C_4H_2$) to evaluate its potential role in the lower altitude photochemistry of Titan's atmospheric ices.

**Methods.** $C_4H_2$ ice films were irradiated with near-ultraviolet (near-UV) photons ($\lambda > 300$ nm) with different UV sources to assess the impact of the wavelengths of photons on the photochemistry of $C_4H_2$. The evolution of the ice's composition was monitored using spectroscopic techniques.

**Results.** Our results reveal that diacetylene ice is reactive through singlet-triplet absorption, similar to the photochemistry of other organic ices of Titan (such as dicyanoacetylene $C_4N_2$ ice) that we investigated previously. Several chemical processes occurred during the photolysis: the hydrogenation of $C_4H_2$ to form other $C_4$ hydrocarbons (vinylacetylene $C_4H_4$ to butane $C_4H_{10}$); the formation of larger and highly polymerizable hydrocarbons, such as triacetylene ($C_6H_2$); and the formation of an organic polymer that is stable at room temperature.

**Conclusions.** The nondetection of diacetylene ice in Titan's atmosphere or surface could be rationalized based on our experimental results that $C_4H_2$ is photochemically highly reactive in the solid phase when exposed to near-UV radiation that reaches Titan's lower altitudes and surface. $C_4H_2$ may be one of the key molecules promoting the chemistry in the ices and aerosols of Titan's haze layers, especially in the case of co-condensation with other organic volatiles, with which it could initiate more complex solid-phase chemistry.

**Key words.** astrochemistry – methods: laboratory: molecular – techniques: spectroscopic – planets and satellites: atmospheres – ultraviolet: planetary systems

## 1. Introduction

The complex organic chemistry initiated in Titan's thermosphere and ionosphere by solar photons and energetic particles of Saturn's magnetosphere leads to the production of many volatile organics as well as organic aerosols (Lavvas et al. 2013; Liang et al. 2007; Waite et al. 2007). The decrease in temperature from the stratosphere to the tropopause (Fulchignoni et al. 2005) allows the direct condensation of many volatiles (hydrocarbons and nitriles), thus forming ice particles or ice accreted on organic aerosols (Anderson et al. 2016; Barth 2003, 2017; de Kok et al. 2008; Frère et al. 1990; Lavvas et al. 2011; Mayo & Samuelson 2005; Raulin & Owen 2002; Sagan & Reid Thompson 1984; Samuelson & Mayo 1991; Samuelson et al. 1997).

Gas molecules and organic hazes in Titan's atmosphere significantly attenuate high-energy photons. As a result, only longer-wavelength photons make it through the stratosphere and the troposphere and eventually to the surface of Titan. Vuitton et al. (2019) model the flux of photons from 1.5 to 300 nm as a function of the altitude in the atmosphere of Titan. According to their work, photons with wavelengths shorter than 150 nm do not penetrate below ~200 km, while photons in the 150 to 200 nm range are progressively absorbed from ~200 km to

~100 km. Finally, only photons in the 200–300 nm range penetrate below 100 km, down to ~50 km. Our recent experimental studies have demonstrated that these longer-wavelength (200 nm and above) ultraviolet (UV) photons could efficiently drive the photochemistry of ices, resulting in the production of organic polymers (Couturier-Tamburelli et al. 2014, 2015; Gudipati et al. 2013; Mouzay et al. 2021a,b) and to the photochemically driven incorporation of these molecules into existing haze particles (Couturier-Tamburelli et al. 2018; Fleury et al. 2019).

Our previous studies of pure-ice photochemistry in Titan's atmosphere were focused on acetylene ($C_2H_2$), benzene ($C_6H_6$), and some nitriles (hydrogen cyanide HCN, cyanoacetylene $HC_3N$, dicyanoacetylene $C_4N_2$, and cyanodiacetylene $HC_5N$), as these species represent the composition of most identified ice clouds (Anderson & Samuelson 2011; Anderson et al. 2010, 2018b; de Kok et al. 2014; Khanna et al. 1987; Samuelson et al. 1997). However, higher hydrocarbons may also condense in Titan's stratosphere, as highlighted by the recent identification of ice clouds that contain benzene at Titan's south pole (Vinatier et al. 2018) and by the discovery by the Cassini Composite InfraRed Spectrometer (CIRS) of the High Altitude South Polar (HASP) cloud (Anderson et al. 2018b) whose spectral signature is consistent with co-condensed HCN-$C_6H_6$ ices

<footnote n="1">¹ Université Paris Cité and Univ Paris Est Creteil, CNRS, LISA, 75013 Paris, France
e-mail: benjamin.fleury@lisa.ipsl.fr</footnote>

<footnote n="2">² Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA</footnote>

<footnote n="3">³ Aix-Marseille Université, CNRS, PIIM, UMR 7345, 13013 Marseille, France
e-mail: isabelle.couturier@univ-amu.fr</footnote>
(Anderson et al. 2018b). After C<sub>6</sub>H<sub>6</sub>, which we studied previ-
ously (Mouzay et al. 2021a,b), diacetylene (C<sub>4</sub>H<sub>2</sub>) is the next
hydrocarbon to condense in the stratosphere of Titan at altitudes
ranging from 70 to 130 km as a function of the latitude and
the season according to different studies (Anderson et al. 2018b,
2016; Barth 2017). Intrigued by the lack of detection of con-
densed C<sub>4</sub>H<sub>2</sub> either in the atmosphere or at the surface of Titan,
we decided to focus our study on the photochemistry of C<sub>4</sub>H<sub>2</sub> ice
as a potential sink for condensed C<sub>4</sub>H<sub>2</sub> in these environments.

In Titan's atmosphere, C₄H₂ is formed in the gas phase below 1200 km by the reaction of acetylene with C₂H radicals (Chastaing et al. 1998; Kaiser et al. 2002), while another mechanism involving the reaction of C₄H₃ with CH₃ radicals exists at higher altitude (Vuitton et al. 2019). Its mixing ratio varies significantly with altitude, decreasing from ~7 × 10⁻⁶ at 981 km in the ionosphere (Cui et al. 2009) to 1 × 10⁻⁹ in the stratosphere (Coustenis et al. 2007, 2010; Vinatier et al. 2007, 2010). In addition, the atmospheric mixing ratio of diacetylene is subject to seasonal variations, leading to a strong polar enrichment in the winter hemisphere (Coustenis et al. 2016; Sylvestre et al. 2018). Further, among the major unsaturated hydrocarbons, C₄H₂ has one of the most extended UV absorptions toward long wavelengths involving the S₀→S₁ (286 nm) and S₀→T₁ (387 nm) excitations (Fischer & Ross 2003; Vila et al. 2000) in addition to its strong photoabsorption cross section between 120 and 220 nm (Ferradaz et al. 2009). Our previous works have shown that direct photoexcitation from the singlet ground state to a triplet excited state is possible in the condensed phase (Couturier-Tamburelli et al. 2014; Gudipati et al. 2013). Therefore, diacetylene is an excellent candidate for solid-state photochemistry and a possible source for the formation of larger volatile molecules or organic polymers in the atmosphere of Titan. In addition, such a reactive photochemical sink could also potentially explain the lack of C₄H₂-ice detection, whereas other ices such as HC₃N have been detected in Titan's atmosphere (Anderson et al. 2010, 2016). C₄H₂ is known to be photochemically reactive in the gas phase (Bandy et al. 1992, 1993; Delpech et al. 1994; Frost et al. 1995; Glicker & Okabe 1987), producing long carbon-chain species such as tri-acetylene (C₆H₂) and tetra-acetylene (C₈H₂). Therefore, C₄H₂ is suspected to be an important intermediate in the reaction pathways for the formation of large organic molecules that make up Titan's atmospheric haze (Abplanalp et al. 2019; Kaiser & Mebel 2012; Wilson & Atreya 2004). Another possibility is that the nondetection of C₄H₂ ice in Titan's atmosphere could be due to the existence of C₄H₂ co-condensate with another species such as HCN, that results in a modification of its spectral signature, as has been observed for the HC₃N-HCN or C₄N₂-HCN co-condensate (Anderson et al. 2018a).

The work reported here presents the first experimental study of the photochemistry of diacetylene ice irradiated with near-UV (λ > 300 nm) photons. We studied the role of longer-wavelength UV-irradiation in the chemical evolution of C₄H₂ ices, the formation of volatile species, and organic polymers in the lower atmosphere of Titan. Finally, we assess the influence of the UV source (monochromatic vs. broadband) on the simulated photochemistry.

**2. Experimental methods and analysis protocols**

**2.1. *The TOAST and RING experimental setups***

For this study we used the Titan Organic Aerosol SpecTroscopy (TOAST) experimental setup at the Jet Propulsion Laboratory, USA (Fleury et al. 2019; Gudipati et al. 2013), and the RING

<figure><img src="image_2.png" /><figcaption>**Fig. 1.** Schemes of the TOAST experimental setup at JPL (left) and the RING experimental setup at PIIM (right).</figcaption></figure>

experimental setup at the PIIM Laboratory at Aix-Marseille
University, France (Theule et al. 2011). Figure 1 presents the
schemes of the TOAST and RING setups. We decided to use
these two experimental setups to obtain complementary datasets.
As described in greater detail below, the two setups used infrared
(IR) spectroscopy in transmission and reflection modes as well
as complementary wavelength ranges. In addition, the experi-
mental setup used at JPL used a monochromatic wavelength for
the ice irradiation, while the setup at PIIM used a polychromatic
UV source, which allowed us to study the possible differences
in the chemistry between monochromatic and polychromatic
irradiation.

Diacetylene is not available commercially and needs to be
synthesized. For this study diacetylene was synthesized accord-
ing to the method described in the literature (Khlifi et al. 1995),
by the dropwise addition of 1,4-dichlroro-2-butyne (C₄H₄Cl₂)
to a mixture of potassium hydroxide (KOH), dimethyl sulfoxide
(DMSO), and water maintained at a temperature of 72 °C under
nitrogen flow atmosphere. DMSO serves to increase the solu-
bility of C₄H₂ in the aqueous phase. At the end of the addition
the temperature was increased to 95 °C and held at this tem-
perature for 15 min. C₄H₂ gas was then driven off by bubbling
N₂ gas through the liquid, passed through a calcium chloride
(CaCl₂) trap to remove traces of water, and condensed in a trap
cooled with liquid nitrogen (LN₂). Finally, C₄H₂ was purified
by vacuum distillation and its purity was checked using mass
spectrometry.

At JPL, ice films were formed by vapor deposition on a
sapphire window fixed on the sample holder of a closed-cycle
helium cryostat, located within a high vacuum chamber with a
background pressure ~8 × 10⁻⁹ mbar. The cryostat has a resis-
tive heater and a temperature controller to precisely control the
temperature of the sample from 10 to 300 K. The temperature
of the sample holder was measured using a silicon diode. In this
study, C₄H₂ vapor was deposited from a gas line at a pressure
of 1 × 10⁻⁶ mbar for 15 min on a sapphire window cooled to
70 K. This is lower than the temperature at which C₄H₂ could
condense in Titan's atmosphere which is ~110 K for an alti-
tude of ~70 km (Barth 2017; Lavvas et al. 2011). However, we
made this choice based on different experimental constraints.
First, a previous experimental study determined that diacetylene
starts to sublimate at ~100 K (Zhou et al. 2009) under a back-
ground pressure of ~5 × 10⁻⁹ mbar, similar to the pressures
reached in our experimental chamber (i.e., ~8 × 10⁻⁹ mbar). It
was therefore necessary to use a temperature lower than 100 K.
We decided to use 70 K, a temperature much lower than 100 K,
to avoid a possible slow sublimation of C₄H₂ during the irradia-
tion experiments, which typically took several hours to complete.
Sublimation could happen at any temperature in a high vacuum
chamber because an ice is in equilibrium with its vapor phase.
As the experimental chambers have turbopumps, vapor can be
(Anderson et al. 2018b). After C<sub>6</sub>H<sub>6</sub>, which we studied previ-
ously (Mouzay et al. 2021a,b), diacetylene (C<sub>4</sub>H<sub>2</sub>) is the next
hydrocarbon to condense in the stratosphere of Titan at altitudes
ranging from 70 to 130 km as a function of the latitude and
the season according to different studies (Anderson et al. 2018b,
2016; Barth 2017). Intrigued by the lack of detection of con-
densed C<sub>4</sub>H<sub>2</sub> either in the atmosphere or at the surface of Titan,
we decided to focus our study on the photochemistry of C<sub>4</sub>H<sub>2</sub> ice
as a potential sink for condensed C<sub>4</sub>H<sub>2</sub> in these environments.

In Titan's atmosphere, C₄H₂ is formed in the gas phase below 1200 km by the reaction of acetylene with C₂H radicals (Chastaing et al. 1998; Kaiser et al. 2002), while another mechanism involving the reaction of C₄H₃ with CH₃ radicals exists at higher altitude (Vuitton et al. 2019). Its mixing ratio varies significantly with altitude, decreasing from ~7 × 10⁻⁶ at 981 km in the ionosphere (Cui et al. 2009) to 1 × 10⁻⁹ in the stratosphere (Coustenis et al. 2007, 2010; Vinatier et al. 2007, 2010). In addition, the atmospheric mixing ratio of diacetylene is subject to seasonal variations, leading to a strong polar enrichment in the winter hemisphere (Coustenis et al. 2016; Sylvestre et al. 2018). Further, among the major unsaturated hydrocarbons, C₄H₂ has one of the most extended UV absorptions toward long wavelengths involving the S₀→S₁ (286 nm) and S₀→T₁ (387 nm) excitations (Fischer & Ross 2003; Vila et al. 2000) in addition to its strong photoabsorption cross section between 120 and 220 nm (Ferradaz et al. 2009). Our previous works have shown that direct photoexcitation from the singlet ground state to a triplet excited state is possible in the condensed phase (Couturier-Tamburelli et al. 2014; Gudipati et al. 2013). Therefore, diacetylene is an excellent candidate for solid-state photochemistry and a possible source for the formation of larger volatile molecules or organic polymers in the atmosphere of Titan. In addition, such a reactive photochemical sink could also potentially explain the lack of C₄H₂-ice detection, whereas other ices such as HC₃N have been detected in Titan's atmosphere (Anderson et al. 2010, 2016). C₄H₂ is known to be photochemically reactive in the gas phase (Bandy et al. 1992, 1993; Delpech et al. 1994; Frost et al. 1995; Glicker & Okabe 1987), producing long carbon-chain species such as tri-acetylene (C₆H₂) and tetra-acetylene (C₈H₂). Therefore, C₄H₂ is suspected to be an important intermediate in the reaction pathways for the formation of large organic molecules that make up Titan's atmospheric haze (Abplanalp et al. 2019; Kaiser & Mebel 2012; Wilson & Atreya 2004). Another possibility is that the nondetection of C₄H₂ ice in Titan's atmosphere could be due to the existence of C₄H₂ co-condensate with another species such as HCN, that results in a modification of its spectral signature, as has been observed for the HC₃N-HCN or C₄N₂-HCN co-condensate (Anderson et al. 2018a).

The work reported here presents the first experimental study of the photochemistry of diacetylene ice irradiated with near-UV (λ > 300 nm) photons. We studied the role of longer-wavelength UV-irradiation in the chemical evolution of C₄H₂ ices, the formation of volatile species, and organic polymers in the lower atmosphere of Titan. Finally, we assess the influence of the UV source (monochromatic vs. broadband) on the simulated photochemistry.

**2. Experimental methods and analysis protocols**

## 2.1. *The TOAST and RING experimental setups*

For this study we used the Titan Organic Aerosol SpecTroscopy
(TOAST) experimental setup at the Jet Propulsion Laboratory,
USA (Fleury et al. 2019; Gudipati et al. 2013), and the RING

<figure><img src="image_2.png" /><figcaption>**Fig. 1.** Schemes of the TOAST experimental setup at JPL (left) and the RING experimental setup at PIIM (right).</figcaption></figure>

experimental setup at the PIIM Laboratory at Aix-Marseille
University, France (Theule et al. 2011). Figure 1 presents the
schemes of the TOAST and RING setups. We decided to use
these two experimental setups to obtain complementary datasets.
As described in greater detail below, the two setups used infrared
(IR) spectroscopy in transmission and reflection modes as well
as complementary wavelength ranges. In addition, the experi-
mental setup used at JPL used a monochromatic wavelength for
the ice irradiation, while the setup at PIIM used a polychromatic
UV source, which allowed us to study the possible differences
in the chemistry between monochromatic and polychromatic
irradiation.

Diacetylene is not available commercially and needs to be
synthesized. For this study diacetylene was synthesized accord-
ing to the method described in the literature (Khlifi et al. 1995),
by the dropwise addition of 1,4-dichloro-2-butyne (C₄H₄Cl₂)
to a mixture of potassium hydroxide (KOH), dimethyl sulfoxide
(DMSO), and water maintained at a temperature of 72 °C under
nitrogen flow atmosphere. DMSO serves to increase the solu-
bility of C₄H₂ in the aqueous phase. At the end of the addition
the temperature was increased to 95 °C and held at this tem-
perature for 15 min. C₄H₂ gas was then driven off by bubbling
N₂ gas through the liquid, passed through a calcium chloride
(CaCl₂) trap to remove traces of water, and condensed in a trap
cooled with liquid nitrogen (LN₂). Finally, C₄H₂ was purified
by vacuum distillation and its purity was checked using mass
spectrometry.

At JPL, ice films were formed by vapor deposition on a
sapphire window fixed on the sample holder of a closed-cycle
helium cryostat, located within a high vacuum chamber with a
background pressure ~8 × 10⁻⁹ mbar. The cryostat has a resis-
tive heater and a temperature controller to precisely control the
temperature of the sample from 10 to 300 K. The temperature
of the sample holder was measured using a silicon diode. In this
study, C₄H₂ vapor was deposited from a gas line at a pressure
of 1 × 10⁻⁶ mbar for 15 min on a sapphire window cooled to
70 K. This is lower than the temperature at which C₄H₂ could
condense in Titan's atmosphere which is ~110 K for an alti-
tude of ~70 km (Barth 2017; Lavvas et al. 2011). However, we
made this choice based on different experimental constraints.
First, a previous experimental study determined that diacetylene
starts to sublimate at ~100 K (Zhou et al. 2009) under a back-
ground pressure of ~5 × 10⁻⁹ mbar, similar to the pressures
reached in our experimental chamber (i.e., ~8 × 10⁻⁹ mbar). It
was therefore necessary to use a temperature lower than 100 K.
We decided to use 70 K, a temperature much lower than 100 K,
to avoid a possible slow sublimation of C₄H₂ during the irradia-
tion experiments, which typically took several hours to complete.
Sublimation could happen at any temperature in a high vacuum
chamber because an ice is in equilibrium with its vapor phase.
As the experimental chambers have turbopumps, vapor can be
pumped, inducing more and more sublimation of the ice over time. Nevertheless, the lower the temperature away from the sublimation temperature (~100 K), the weaker the ice's sublimation, and it was negligible at 70 K for the duration of the trial (which we experimentally determined).

The prepared ice film, about a micrometer thick (see Sect. 3.1), was subsequently irradiated for 6 h at 1 h doses, with photons at 355 nm obtained by a third harmonic generation from a nanosecond pulsed Nd:YAG laser (Quantel) with a repetition rate of 20 Hz. After each hour of irradiation, the spectra were measured before continuing the photolysis. The diameter of the initial circular laser beam was expanded from 3 to 20 mm using a plano-convex lens (75 mm focal length) that reduced the laser photons flux by a factor of 44 to uniformly illuminate the entire surface of the ice film and to avoid multi-photon processes. In a previous publication we showed that photons at 355 nm produced by a defocused nanosecond pulsed laser drove solid-phase photochemistry via a single-photon process (Gudipati et al. 2013), and one-photon absorption was shown to dominate even at 8 mJ pulse⁻¹ or 9.1 × 10¹⁶ photons cm⁻² s⁻¹ at 355 nm and 20 Hz repetition rate. The present work was carried out under similar conditions: at the same wavelength at 20 Hz repetition rate with an energy of 10.5 mJ pulse⁻¹ or 1.3 × 10¹⁷ photons cm⁻² s⁻¹. Pulse energies were measured at the laser outlet, while photons fluxes were calculated at the sample's surface after expansion of the laser. The evolution of the diacetylene ice film was monitored after each irradiation using transmission-absorption IR and ultraviolet-visible (UV-Vis) spectroscopy. After irradiation, the sample was warmed to 180 K under vacuum using temperature-programmed desorption (TPD) at 1 K min⁻¹ in order to sublimate the photo-produced volatiles. During the experiment, the composition of the sublimated gas-phase molecules was also monitored using in situ mass spectrometry.

At PIIM, ice films were formed by vapor deposition on a copper substrate fixed on the sample holder of a closed-cycle helium cryostat, located within a high vacuum chamber with a background pressure of ~8 × 10⁻⁹ mbar. The cryostat has a resistive heater and a temperature controller to precisely control the temperature of the sample from 10 K to 300 K. The temperature of the sample holder was measured using a silicon diode. We deposited 0.6 mbar of gas phase C₄H₂ for around 20 min on the copper surface kept at 70 K at a pressure of 1 × 10⁻⁶ mbar. In contrast to the JPL experiments where the ice was irradiated with a single wavelength laser, during the RING experiments, a diacetylene ice film (a few hundred nanometers thick; see Sect. 3.1) was irradiated with broadband UV photons (λ > 300 nm) generated by an Osram 200 W high-pressure mercury lamp equipped with a cutoff filter at 300 nm. The total photon flux of the lamp at wavelengths above 300 nm has been estimated to be about 2.75 × 10¹⁶ photons cm⁻² s⁻¹ (Couturier-Tamburelli et al. 2014). After about 5 h of irradiation, the ice samples were slowly warmed up to room temperature to evaporate the volatile species. Changes in the ice samples were monitored by reflection IR spectroscopy.

## 2.2. IR spectroscopy

At JPL, IR spectra were recorded in transmission with a Thermo Scientific Nicolet 6700 Fourier Transform InfraRed (FTIR) spectrometer. After passing through the sample, the IR beam was focused on a mercury cadmium telluride (MCT) detector cooled to 77 K with LN₂. Each spectrum consists of an average of 200 scans with a resolution of 1 cm⁻¹ and covers the 1600 cm⁻¹

(sapphire cut on) to 4500 cm⁻¹ range. Reflection absorption IR spectra were measured at PIIM from 4000 to 600 cm⁻¹ using a Vertex 70 FTIR spectrometer. Each spectrum was averaged over 100 scans with a resolution of 1 cm⁻¹. At the copper surface the IR beam was reflected with a 36° angle and focused on a MCT detector cooled to 77 K. The two experiments at PIIM and JPL are therefore complementary in terms of spectral ranges, and provide a large spectral covering from 4500 to 600 cm⁻¹. The IR spectra recorded at JPL and PIIM were used to calculate the thickness of the deposited ice films and the diacetylene column density (see Sect. 3). To do this, we used the Beer-Lambert law. In the case of the reflection absorption spectra recorded at PIIM, this is an approximation that could bias the calculated values. Even so, this approach has been used in experimental studies using reflection absorption spectroscopy (Bennett & Kaiser 2005; Couturier-Tamburelli et al. 2018; Mouzay et al. 2021b; Noble et al. 2012). To take this problem into account and limit the error on the calculated values in the case of the PIIM experiments, we decided to divide the integrated absorbance in the equations used in Sect. 3 by a factor of 2 to correct for the incoming and outgoing infrared beam through the ice film.

## 2.3. UV-Vis spectroscopy

At JPL, the UV-Vis spectra were measured from 210 to 1100 nm with an incidence angle of 45° (Fig. 1), using an Ocean Optics DH-2000 deuterium-halogen lamp and a USB4000 spectrograph connected to the chamber via optical fiber feedthrough. Each spectrum was averaged over 500 scans with 20 ms of integration per scan.

## 2.4. Mass spectrometry

At JPL, the analysis by mass spectrometry of the molecules desorbed during the TPD was achieved with a quadrupole mass spectrometer (RGA 300, SRS instrument), with a mass range of 1–300 amu and equipped with a continuous dynode electron multiplier (CDEM) detector, enabling measurement of trace molecules at partial pressures as low as 1 × 10⁻¹² mbar. The molecules were ionized by electron impact with an energy of 70 eV. The mass resolution (m/Δm) is 100 at m/z 100.

# 3. Results

## 3.1. Spectroscopy of C₄H₂ ice deposited at 70 K

Figure 2 presents the IR spectra of the diacetylene ice films deposited at 70 K at JPL and PIIM in the 3400–1800 cm⁻¹ region and in the 4000–600 cm⁻¹ region, respectively. Three fundamental absorption bands of C₄H₂ are observed in the JPL spectrum, in agreement with previous studies (Khanna et al. 1988; Zhou et al. 2009). The most intense peak at 3272 cm⁻¹ is assigned to the ν₄ asymmetric stretching mode of the C-H bond. This band is saturated on the JPL spectrum because of the thick ice film used for the experiment (see discussion below). Weaker absorption bands at 2013 and 2177 cm⁻¹ are assigned to the ν₅ asymmetric stretching mode and the ν₂ symmetric stretching mode of the C≡C bond, respectively. Two other fundamental absorption bands of C₄H₂ are observed in the PIIM’s spectrum located at 674 and 847 cm⁻¹ and assigned to the ν₈ CH bending mode and to the ν₃ stretching mode of the C–C bond respectively. The position and shape of the absorption bands suggest that C₄H₂ is in a crystalline form when deposited at 70 K. This agrees with the previous experimental study of Zhou et al. (2009), which found
pumped, inducing more and more sublimation of the ice over time. Nevertheless, the lower the temperature away from the sublimation temperature (~100 K), the weaker the ice's sublimation, and it was negligible at 70 K for the duration of the trial (which we experimentally determined).

The prepared ice film, about a micrometer thick (see Sect. 3.1), was subsequently irradiated for 6 h at 1 h doses, with photons at 355 nm obtained by a third harmonic generation from a nanosecond pulsed Nd:YAG laser (Quantel) with a repetition rate of 20 Hz. After each hour of irradiation, the spectra were measured before continuing the photolysis. The diameter of the initial circular laser beam was expanded from 3 to 20 mm using a plano-convex lens (75 mm focal length) that reduced the laser photons flux by a factor of 44 to uniformly illuminate the entire surface of the ice film and to avoid multi-photon processes. In a previous publication we showed that photons at 355 nm produced by a defocused nanosecond pulsed laser drove solid-phase photochemistry via a single-photon process (Gudipati et al. 2013), and one-photon absorption was shown to dominate even at 8 mJ pulse⁻¹ or 9.1 × 10¹⁶ photons cm⁻² s⁻¹ at 355 nm and 20 Hz repetition rate. The present work was carried out under similar conditions: at the same wavelength at 20 Hz repetition rate with an energy of 10.5 mJ pulse⁻¹ or 1.3 × 10¹⁷ photons cm⁻² s⁻¹. Pulse energies were measured at the laser outlet, while photons fluxes were calculated at the sample's surface after expansion of the laser. The evolution of the diacetylene ice film was monitored after each irradiation using transmission-absorption IR and ultraviolet-visible (UV-Vis) spectroscopy. After irradiation, the sample was warmed to 180 K under vacuum using temperature-programmed desorption (TPD) at 1 K min⁻¹ in order to sublimate the photo-produced volatiles. During the experiment, the composition of the sublimated gas-phase molecules was also monitored using in situ mass spectrometry.

At PIIM, ice films were formed by vapor deposition on a copper substrate fixed on the sample holder of a closed-cycle helium cryostat, located within a high vacuum chamber with a background pressure of ~8 × 10⁻⁹ mbar. The cryostat has a resistive heater and a temperature controller to precisely control the temperature of the sample from 10 K to 300 K. The temperature of the sample holder was measured using a silicon diode. We deposited 0.6 mbar of gas phase C₄H₂ for around 20 min on the copper surface kept at 70 K at a pressure of 1 × 10⁻⁶ mbar. In contrast to the JPL experiments where the ice was irradiated with a single wavelength laser, during the RING experiments, a diacetylene ice film (a few hundred nanometers thick; see Sect. 3.1) was irradiated with broadband UV photons (λ > 300 nm) generated by an Osram 200 W high-pressure mercury lamp equipped with a cutoff filter at 300 nm. The total photon flux of the lamp at wavelengths above 300 nm has been estimated to be about 2.75 × 10¹⁶ photons cm⁻² s⁻¹ (Couturier-Tamburelli et al. 2014). After about 5 h of irradiation, the ice samples were slowly warmed up to room temperature to evaporate the volatile species. Changes in the ice samples were monitored by reflection IR spectroscopy.

## 2.2. IR spectroscopy

At JPL, IR spectra were recorded in transmission with a Thermo Scientific Nicolet 6700 Fourier Transform InfraRed (FTIR) spectrometer. After passing through the sample, the IR beam was focused on a mercury cadmium telluride (MCT) detector cooled to 77 K with LN₂. Each spectrum consists of an average of 200 scans with a resolution of 1 cm⁻¹ and covers the 1600 cm⁻¹

(sapphire cut on) to 4500 cm⁻¹ range. Reflection absorption IR spectra were measured at PIIM from 4000 to 600 cm⁻¹ using a Vertex 70 FTIR spectrometer. Each spectrum was averaged over 100 scans with a resolution of 1 cm⁻¹. At the copper surface the IR beam was reflected with a 36° angle and focused on a MCT detector cooled to 77 K. The two experiments at PIIM and JPL are therefore complementary in terms of spectral ranges, and provide a large spectral covering from 4500 to 600 cm⁻¹. The IR spectra recorded at JPL and PIIM were used to calculate the thickness of the deposited ice films and the diacetylene column density (see Sect. 3). To do this, we used the Beer-Lambert law. In the case of the reflection absorption spectra recorded at PIIM, this is an approximation that could bias the calculated values. Even so, this approach has been used in experimental studies using reflection absorption spectroscopy (Bennett & Kaiser 2005; Couturier-Tamburelli et al. 2018; Mouzay et al. 2021b; Noble et al. 2012). To take this problem into account and limit the error on the calculated values in the case of the PIIM experiments, we decided to divide the integrated absorbance in the equations used in Sect. 3 by a factor of 2 to correct for the incoming and outgoing infrared beam through the ice film.

## 2.3. UV-Vis spectroscopy

At JPL, the UV-Vis spectra were measured from 210 to 1100 nm with an incidence angle of 45° (Fig. 1), using an Ocean Optics DH-2000 deuterium-halogen lamp and a USB4000 spectrograph connected to the chamber via optical fiber feedthrough. Each spectrum was averaged over 500 scans with 20 ms of integration per scan.

## 2.4. Mass spectrometry

At JPL, the analysis by mass spectrometry of the molecules desorbed during the TPD was achieved with a quadrupole mass spectrometer (RGA 300, SRS instrument), with a mass range of 1–300 amu and equipped with a continuous dynode electron multiplier (CDEM) detector, enabling measurement of trace molecules at partial pressures as low as 1 × 10⁻¹² mbar. The molecules were ionized by electron impact with an energy of 70 eV. The mass resolution (m/Δm) is 100 at m/z 100.

# 3. Results

## 3.1. Spectroscopy of C₄H₂ ice deposited at 70 K

Figure 2 presents the IR spectra of the diacetylene ice films deposited at 70 K at JPL and PIIM in the 3400–1800 cm⁻¹ region and in the 4000–600 cm⁻¹ region, respectively. Three fundamental absorption bands of C₄H₂ are observed in the JPL spectrum, in agreement with previous studies (Khanna et al. 1988; Zhou et al. 2009). The most intense peak at 3272 cm⁻¹ is assigned to the ν₄ asymmetric stretching mode of the C-H bond. This band is saturated on the JPL spectrum because of the thick ice film used for the experiment (see discussion below). Weaker absorption bands at 2013 and 2177 cm⁻¹ are assigned to the ν₅ asymmetric stretching mode and the ν₂ symmetric stretching mode of the C≡C bond, respectively. Two other fundamental absorption bands of C₄H₂ are observed in the PIIM’s spectrum located at 674 and 847 cm⁻¹ and assigned to the ν₈ CH bending mode and to the ν₃ stretching mode of the C–C bond respectively. The position and shape of the absorption bands suggest that C₄H₂ is in a crystalline form when deposited at 70 K. This agrees with the previous experimental study of Zhou et al. (2009), which found
<figure><img src="image_3.png" /><figcaption>**Fig. 2.** Infrared spectra of C₄H₂ films obtained at JPL and PIIM independently. (a) IR spectrum of C₄H₂ ice deposited at 70 K at JPL on a sapphire window. The splitting of the v₅ band is due to the crystalline nature of the ice film. The spectrum is cropped at 2340 cm⁻¹ to remove the absorption band due to gas-phase CO₂ in the path of the IR beam outside the vacuum chamber. (b) IR spectrum of C₄H₂ ice deposited at 70 K at PIIM on a copper substrate.</figcaption></figure>

<figure><img src="image_4.png" /><figcaption>**Fig. 3.** UV spectrum of C₄H₂ ice deposited at 70 K at JPL on a sapphire window. The positions of the center of some electronic transitions of C₄H₂ are indicated (see discussion in Sect. 4.1).</figcaption></figure>

that for C₄H₂ ice the amorphous to crystalline transition occurs around 70 K.

The diacetylene ice thickness h can be calculated as

$$h = \frac{\int \tau_v d\nu}{\int \alpha d\nu}, \qquad (1)$$

where $\int \tau_v d\nu$ is the integrated optical depth of the band, which was determined from the absorbance of the band, and $\int \alpha d\nu$ is the integrated extinction coefficient of the band (cm⁻¹). For our calculation, we used an integrated extinction coefficient value of 3.9 × 10³ cm⁻¹ for the 2013 cm⁻¹ band, determined for crystalline diacetylene at 70 K by Khanna et al. (1988). We calculated a diacetylene ice thickness of ~374 nm for the PIIM experiment and ~1.1 µm for the JPL experiment, reflecting the difference in the deposition conditions between experiments carried out at JPL and PIIM. Although the thicker deposit used at JPL leads to a saturation of the C–H absorption band of C₄H₂ (see Fig. 2), we decided to proceed with this ice thickness to enhance the formation of volatile species and increase their detectability by IR and UV spectroscopy and mass spectrometry.

As presented in Fig. 3, C₄H₂ ice at 70 K has strong absorption in the UV, with structured absorption bands at 226, 237, and 249 nm. These bands are separated by 2040 cm⁻¹ wavenumbers, corresponding to v₅ vibronic coupling in the singlet exited state ¹Δₐ. These absorption bands are close to those measured in the gas phase for C₄H₂, but as expected they are shifted by ~5 nm toward longer wavelengths compared to the gas-phase bands (Jolly & Benilan 2008; Smith et al. 1998). However, in contrast to the gas phase, we observed in the solid phase the presence of a weaker absorption continuum from 250 to 400 nm.

## 3.2. Photochemistry of pure C₄H₂ ice at $\lambda > 300$ nm

At JPL the C₄H₂ ice film was irradiated for 6 hr with a 355 nm defocused laser. We monitored the gas-phase volatiles in the chamber using mass spectrometry during the irradiation and did not observe any photodesorption of diacetylene. In addition, IR and UV-Vis spectra were recorded after each irradiation period. We used the evolution of the diacetylene absorption bands at 3272 and 2013 cm⁻¹ after each irradiation period to monitor its consumption due to photochemical reactions. Figure 4 (panels a and c) presents the evolution of the differential absorbance of these two absorption bands of C₄H₂ after each irradiation period. The differential absorbance is the difference between the absorbance after a time “t” of irradiation A_t and the initial absorbance A_t=0. After 1 h of irradiation we observed a small change in the C–H absorption band at 3272 cm⁻¹. However, this change is not conclusive (increase and decrease of the band) because of the saturation of the C–H absorption band at the beginning of the experiment (absorbance value >>2.5, Fig. 2). In addition, we observed a very small depletion of the v₅ band at 2013 cm⁻¹. However, when we pursued the irradiation further, the absorbance of both diacetylene bands decreased, indicating a significant depletion of the ice sample. We also observed an increase in the absorbance at higher wavenumber, with broad peaks at 3284 and 3291 cm⁻¹ as well as a larger continuum at higher wavenumber. This indicates the formation of new products from the C₄H₂ ice photochemistry. The peak at 3284 cm⁻¹ may be attributed to vinylacetylene, C₄H₄ (Kim & Kaiser 2009). The same peak was observed in previous laboratory experiments involving acetylene ice photochemistry (Cuylle et al. 2014).

The C₄H₂ ice film irradiation was performed at PIIM with a lamp generating photons at $\lambda > 300$ nm in order to see
<figure><img src="image_3.png" /></figure>

<figure><img src="image_4.png" /><figcaption>Fig. 2. Infrared spectra of C₄H₂ films obtained at JPL and PIIM independently. (a) IR spectrum of C₄H₂ ice deposited at 70 K at JPL on a sapphire window. The splitting of the v₅ band is due to the crystalline nature of the ice film. The spectrum is cropped at 2340 cm⁻¹ to remove the absorption band due to gas-phase CO₂ in the path of the IR beam outside the vacuum chamber. (b) IR spectrum of C₄H₂ ice deposited at 70 K at PIIM on a copper substrate.</figcaption></figure>

that for C₄H₂ ice the amorphous to crystalline transition occurs around 70 K.

The diacetylene ice thickness h can be calculated as

$$h = \frac{\int \tau_v d\nu}{\int \alpha d\nu}, \qquad (1)$$

where $\int \tau_v d\nu$ is the integrated optical depth of the band, which was determined from the absorbance of the band, and $\int \alpha d\nu$ is the integrated extinction coefficient of the band (cm⁻¹). For our calculation, we used an integrated extinction coefficient value of 3.9 × 10³ cm⁻¹ for the 2013 cm⁻¹ band, determined for crystalline diacetylene at 70 K by Khanna et al. (1988). We calculated a diacetylene ice thickness of ~374 nm for the PIIM experiment and ~1.1 µm for the JPL experiment, reflecting the difference in the deposition conditions between experiments carried out at JPL and PIIM. Although the thicker deposit used at JPL leads to a saturation of the C–H absorption band of C₄H₂ (see Fig. 2), we decided to proceed with this ice thickness to enhance the formation of volatile species and increase their detectability by IR and UV spectroscopy and mass spectrometry.

<figure><img src="image_5.png" /><figcaption>Fig. 3. UV spectrum of C₄H₂ ice deposited at 70 K at JPL on a sapphire window. The positions of the center of some electronic transitions of C₄H₂ are indicated (see discussion in Sect. 4.1).</figcaption></figure>

As presented in Fig. 3, C₄H₂ ice at 70 K has strong absorption in the UV, with structured absorption bands at 226, 237, and 249 nm. These bands are separated by 2040 cm⁻¹ wavenumbers, corresponding to v₅ vibronic coupling in the singlet exited state ¹Δₐ. These absorption bands are close to those measured in the gas phase for C₄H₂, but as expected they are shifted by ~5 nm toward longer wavelengths compared to the gas-phase bands (Jolly & Benilan 2008; Smith et al. 1998). However, in contrast to the gas phase, we observed in the solid phase the presence of a weaker absorption continuum from 250 to 400 nm.

## 3.2. Photochemistry of pure C₄H₂ ice at $\lambda > 300$ nm

At JPL the C₄H₂ ice film was irradiated for 6 hr with a 355 nm defocused laser. We monitored the gas-phase volatiles in the chamber using mass spectrometry during the irradiation and did not observe any photodesorption of diacetylene. In addition, IR and UV-Vis spectra were recorded after each irradiation period. We used the evolution of the diacetylene absorption bands at 3272 and 2013 cm⁻¹ after each irradiation period to monitor its consumption due to photochemical reactions. Figure 4 (panels a and c) presents the evolution of the differential absorbance of these two absorption bands of C₄H₂ after each irradiation period. The differential absorbance is the difference between the absorbance after a time “t” of irradiation A_t and the initial absorbance A_t=0. After 1 h of irradiation we observed a small change in the C–H absorption band at 3272 cm⁻¹. However, this change is not conclusive (increase and decrease of the band) because of the saturation of the C–H absorption band at the beginning of the experiment (absorbance value >>2.5, Fig. 2). In addition, we observed a very small depletion of the v₅ band at 2013 cm⁻¹. However, when we pursued the irradiation further, the absorbance of both diacetylene bands decreased, indicating a significant depletion of the ice sample. We also observed an increase in the absorbance at higher wavenumber, with broad peaks at 3284 and 3291 cm⁻¹ as well as a larger continuum at higher wavenumber. This indicates the formation of new products from the C₄H₂ ice photochemistry. The peak at 3284 cm⁻¹ may be attributed to vinylacetylene, C₄H₄ (Kim & Kaiser 2009). The same peak was observed in previous laboratory experiments involving acetylene ice photochemistry (Cuylle et al. 2014).

The C₄H₂ ice film irradiation was performed at PIIM with a lamp generating photons at $\lambda > 300$ nm in order to see
<figure><img src="image_5.png" /><figcaption>Fig. 4. Changes to IR spectra observed during near-UV irradiation of C₄H₂ ice films. (a) Evolution of the differential absorbance (Aᵢ - Aᵢ=0) of the v₄ band of C₄H₂ as function of the time of irradiation at 355 nm at JPL. (b) Evolution of the differential absorbance of the v₄ band of C₄H₂ as function of the time of irradiation at λ > 300 nm at PIIM. (c) Evolution of the differential absorbance of the v₅ band of C₄H₂ as function of the time of irradiation at 355 nm at JPL. (d) Evolution of the differential absorbance of the v₅ band of C₄H₂ as function of the time of irradiation at λ > 300 nm at PIIM.</figcaption></figure>

if broadband irradiation leads to different results. Neverthe-
less, the results of these experiments are similar to those per-
formed at JPL, as illustrated by the IR spectra shown in Fig. 4
(Panels b and d). The subtraction spectra reveal the appearance
of new infrared bands, listed in Table 1, in addition to those
observed at 3284 and 3291 cm⁻¹ in the laser experiment. They
are attributed without ambiguity to C₄H₄ when compared to the
data of Kim & Kaiser (2009). From these results obtained at JPL
and PIIM, we confirm that C₄H₄ is one of the photoproducts
of C₄H₂ ice photochemistry. We note that the sapphire window
used for transmission-absorption spectroscopy in the JPL exper-
iments cuts off below 1600 cm⁻¹. For this reason, and based on
the relative intensities of infrared bands obtained at PIIM, we
observed only the v₁ band of C₄H₄ in the JPL experiments. On
the other hand, the PIIM experimental setup records the entire
mid-infrared region thanks to the use of a reflection-absorption
configuration. As a result, several absorption bands assigned to
C₄H₄ are also observed in the experiments conducted at PIIM,
increasing the confidence of our assignment. We also note that in
the transmission-absorption mode employed at JPL, the sample
is ~1100 nm thick, which is also the IR beam pathlength. Under
reflection-absorption conditions, the IR beam penetrates through
longer than twice the ice thickness of 374 nm. For this reason, we
could be sampling twice the amount of the ice.

We derived the evolution of the C₄H₂ column density con-
sumed as a function of the photon fluences for both experiments
from the IR data shown in Fig. 4. We decided to calculate the
column density using the integrated v₅ band area of C₄H₂ at
2013 cm⁻¹ because the other band at 3272 cm⁻¹ was saturated.
The consumed column density can be calculated with Eq. (2),

$$
N_c = N_0 - N_f, \tag{2}
$$

where N_c is the consumed column density (molecules cm⁻²)
after a fluence f, N₀ is the initial column density
(molecules cm⁻²) of C₄H₂, and N_f is the column density
(molecules cm⁻²) of C₄H₂ molecules remaining after a fluence
f. The column density is determined using Eq. (3),

$$
N = \frac{\int \tau_{\nu} d\nu}{A}, \qquad (3)
$$

where N is the column density (molecules cm⁻²), A is the band
strength (cm molecule⁻¹), and ∫τνdν is the integrated band in
optical depth derived from the absorbance. The band strength A
can be calculated from the integrated extinction coefficient using
Eq. (4),

$$
A = \frac{\int \alpha d\nu}{\rho_N}, \qquad (4)
$$
<figure><img src="image_6.png" /><figcaption>Fig. 4. Changes to IR spectra observed during near-UV irradiation of C₄H₂ ice films. (a) Evolution of the differential absorbance (Aᵢ - Aᵢ=0) of the v₄ band of C₄H₂ as function of the time of irradiation at 355 nm at JPL. (b) Evolution of the differential absorbance of the v₄ band of C₄H₂ as function of the time of irradiation at λ > 300 nm at PIIM. (c) Evolution of the differential absorbance of the v₅ band of C₄H₂ as function of the time of irradiation at 355 nm at JPL. (d) Evolution of the differential absorbance of the v₅ band of C₄H₂ as function of the time of irradiation at λ > 300 nm at PIIM.</figcaption></figure>

if broadband irradiation leads to different results. Neverthe-
less, the results of these experiments are similar to those per-
formed at JPL, as illustrated by the IR spectra shown in Fig. 4
(Panels b and d). The subtraction spectra reveal the appearance
of new infrared bands, listed in Table 1, in addition to those
observed at 3284 and 3291 cm⁻¹ in the laser experiment. They
are attributed without ambiguity to C₄H₄ when compared to the
data of Kim & Kaiser (2009). From these results obtained at JPL
and PIIM, we confirm that C₄H₄ is one of the photoproducts
of C₄H₂ ice photochemistry. We note that the sapphire window
used for transmission-absorption spectroscopy in the JPL exper-
iments cuts off below 1600 cm⁻¹. For this reason, and based on
the relative intensities of infrared bands obtained at PIIM, we
observed only the v₁ band of C₄H₄ in the JPL experiments. On
the other hand, the PIIM experimental setup records the entire
mid-infrared region thanks to the use of a reflection-absorption
configuration. As a result, several absorption bands assigned to
C₄H₄ are also observed in the experiments conducted at PIIM,
increasing the confidence of our assignment. We also note that in
the transmission-absorption mode employed at JPL, the sample
is ~1100 nm thick, which is also the IR beam pathlength. Under
reflection-absorption conditions, the IR beam penetrates through
longer than twice the ice thickness of 374 nm. For this reason, we
could be sampling twice the amount of the ice.

We derived the evolution of the C₄H₂ column density con-
sumed as a function of the photon fluences for both experiments
from the IR data shown in Fig. 4. We decided to calculate the
column density using the integrated v₅ band area of C₄H₂ at
2013 cm⁻¹ because the other band at 3272 cm⁻¹ was saturated.
The consumed column density can be calculated with Eq. (2),

$$
N_c = N_0 - N_f, \tag{2}
$$

where N_c is the consumed column density (molecules cm⁻²)
after a fluence f, N₀ is the initial column density
(molecules cm⁻²) of C₄H₂, and N_f is the column density
(molecules cm⁻²) of C₄H₂ molecules remaining after a fluence
f. The column density is determined using Eq. (3),

$$
N = \frac{\int \tau_{\nu} d\nu}{A}, \qquad (3)
$$

where N is the column density (molecules cm⁻²), A is the band
strength (cm molecule⁻¹), and ∫τνdν is the integrated band in
optical depth derived from the absorbance. The band strength A
can be calculated from the integrated extinction coefficient using
Eq. (4),

$$
A = \frac{\int \alpha d\nu}{\rho_N}, \qquad (4)
$$
<table><caption>**Table 1.** Infrared absorption bands of C₄H₄ ice observed in our experimental conditions.</caption><thead><tr><th rowspan="2">Assignment</th><th>Kim & Kaiser (2009)</th><th>JPL 70 K</th><th>PIIM 70 K</th><th>PIIM 70 K</th></tr><tr><th>100 K<br>Position (cm<sup>-1</sup>)</th><th>Position (cm<sup>-1</sup>)</th><th>Position (cm<sup>-1</sup>)</th><th>Relative intensity</th></tr></thead><tbody><tr><td>ν<sub>1</sub></td><td>3288</td><td>3291/3284</td><td>3290/3281</td><td>100</td></tr><tr><td>ν<sub>3</sub></td><td>3049</td><td></td><td>3037</td><td>1.5</td></tr><tr><td>ν<sub>4</sub></td><td>3014</td><td></td><td>3017</td><td>2.1</td></tr><tr><td>ν<sub>6</sub> + ν<sub>7</sub></td><td></td><td></td><td>2965</td><td>0.5</td></tr><tr><td>ν<sub>5</sub></td><td>2103</td><td></td><td>2104</td><td>2.0</td></tr><tr><td>ν<sub>6</sub></td><td>1599</td><td></td><td>1592</td><td>0.9</td></tr><tr><td>ν<sub>10</sub> + ν<sub>12</sub></td><td>1374</td><td></td><td>1384</td><td>10.3</td></tr><tr><td>2ν<sub>11</sub>/2ν<sub>17</sub>/ν<sub>11</sub> + ν<sub>17</sub></td><td>1259</td><td></td><td>1262</td><td>15.9</td></tr></tbody></table>

**Notes.** The position of the absorption bands observed after irradiation in the JPL and PIIM experiments at 70 K is shown. The position of the IR absorption bands of crystalline C₄H₄ ice at 100 K determined experimentally by Kim & Kaiser (2009) is also shown for reference. Relative intensities of the IR bands observed in the PIIM experiment were calculated from the integrated areas of the IR bands.

<figure><img src="image_6.png" /><figcaption>**Fig. 5.** Quantity of C₄H₂ consumed as a function of the photon-fluence (JPL, 355 nm, black square; PIIM, λ > 300 nm, red circle). The quantity is expressed in column density and was calculated from the IR spectra.</figcaption></figure>

<figure><img src="image_7.png" /><figcaption>**Fig. 6.** Differential absorbance ($A_t - A_{t=0}$) in the UV-Vis domain for the different time of irradiation at 355 nm. Assignments of some of the absorption bands are shown.</figcaption></figure>

where $\int \alpha d\nu$ is the integrated extinction coefficient (cm⁻¹) and $\rho_N$ is the number density (molecules cm⁻³). Finally, by combining Eqs. (3) and (4), we obtained Eq. (5):

$$N = \frac{\int \tau_{\nu} d\nu \times \rho_{N}}{\int \alpha d\nu} \qquad (5)$$

For our calculation we used an integrated extinction coefficient value of $3.9 \times 10^3$ cm⁻² for the 2013 cm⁻¹ band calculated for the crystalline diacetylene at 70 K by Khanna et al. (1988) and a $\rho_N$ of $9.2 \times 10^{21}$ molecules cm⁻³. The value of the number density is the more important source of uncertainties for this calculation and this value is derived from the mass density using Avogadro's number, and the molar mass of diacetylene (50.06 g mol⁻¹). However, the mass density of crystalline diacetylene is not available in the literature. Thus, we assumed a mass density of 0.76 g cm⁻³ measured for crystalline acetylene at 131 K (Hudson et al. 2014; McMullan et al. 1992). Figure 5 presents the evolution of the consumed C₄H₂ in column density as a function of the photon-fluence for both experiments performed at JPL and PIIM. As explained in Sect. 2.2, a doubled pathlength of absorption due to the reflection-absorption technique used at PIIM was factored in when calculating the column density for the PIIM experiments. We obtained that $2.6 \times 10^{17}$ molecule cm⁻² of C₄H₂ were

consumed for a photon-fluence of $3.9 \times 10^{21}$ photons cm⁻² at 355 nm, while $3.4 \times 10^{17}$ molecule cm⁻² of C₄H₂ were consumed for a fluence of $4.5 \times 10^{20}$ photons cm⁻² at λ > 300 nm. These results indicate that a polychromatic photon flux covering a broader wavelength range longward of 300 nm substantially increases the kinetics of the diacetylene photolysis, leading to a slightly higher number of diacetylene molecules consumed with a photon fluence that is ten times lower compared to irradiation performed at 355 nm. We can make the hypothesis that this difference is due to a significant increase in the absorbance of diacetylene between 350 and 300 nm (Fig. 3).

The UV-Vis spectra obtained during the experiments at JPL are presented in Fig. 6; they provide complementary information on the photochemistry of C₄H₂ upon irradiation at 355 nm. We observed the diminution of the diacetylene absorption bands after 60 min of irradiation and then after each successive step of irradiation, in agreement with the IR measurements. In addition, new absorption bands were observed at longer wavelengths: 270, 287, 306, 414, 513, and 575 nm. In addition to these individual bands, we observed an increase in continuum from 260 to 700 nm after each irradiation. A similar absorption continuum was also observed during previous experiments on C₄N₂ ice (Gudipati et al. 2013) and can be attributed to the growth of a polymeric organic material in the ice. The new bands can
<table><caption>**Table 1.** Infrared absorption bands of C₄H₄ ice observed in our experimental conditions.</caption><thead><tr><th rowspan="2">Assignment</th><th>Kim & Kaiser (2009)</th><th>JPL 70 K</th><th>PIIM 70 K</th><th>PIIM 70 K</th></tr><tr><th>100 K<br>Position (cm<sup>-1</sup>)</th><th>Position (cm<sup>-1</sup>)</th><th>Position (cm<sup>-1</sup>)</th><th>Relative intensity</th></tr></thead><tbody><tr><td>ν<sub>1</sub></td><td>3288</td><td>3291/3284</td><td>3290/3281</td><td>100</td></tr><tr><td>ν<sub>3</sub></td><td>3049</td><td></td><td>3037</td><td>1.5</td></tr><tr><td>ν<sub>4</sub></td><td>3014</td><td></td><td>3017</td><td>2.1</td></tr><tr><td>ν<sub>6</sub> + ν<sub>7</sub></td><td></td><td></td><td>2965</td><td>0.5</td></tr><tr><td>ν<sub>5</sub></td><td>2103</td><td></td><td>2104</td><td>2.0</td></tr><tr><td>ν<sub>6</sub></td><td>1599</td><td></td><td>1592</td><td>0.9</td></tr><tr><td>ν<sub>10</sub> + ν<sub>12</sub></td><td>1374</td><td></td><td>1384</td><td>10.3</td></tr><tr><td>2ν<sub>11</sub>/2ν<sub>17</sub>/ν<sub>11</sub> + ν<sub>17</sub></td><td>1259</td><td></td><td>1262</td><td>15.9</td></tr></tbody></table>

**Notes.** The position of the absorption bands observed after irradiation in the JPL and PIIM experiments at 70 K is shown. The position of the IR absorption bands of crystalline C₄H₄ ice at 100 K determined experimentally by Kim & Kaiser (2009) is also shown for reference. Relative intensities of the IR bands observed in the PIIM experiment were calculated from the integrated areas of the IR bands.

<figure><img src="image_7.png" /><figcaption>**Fig. 5.** Quantity of C₄H₂ consumed as a function of the photon-fluence (JPL, 355 nm, black square; PIIM, λ > 300 nm, red circle). The quantity is expressed in column density and was calculated from the IR spectra.</figcaption></figure>

<figure><img src="image_8.png" /><figcaption>**Fig. 6.** Differential absorbance (A<sub>t</sub> - A<sub>t=0</sub>) in the UV-Vis domain for the different time of irradiation at 355 nm. Assignments of some of the absorption bands are shown.</figcaption></figure>

where $\int \alpha d\nu$ is the integrated extinction coefficient (cm⁻¹) and $\rho_N$ is the number density (molecules cm⁻³). Finally, by combining Eqs. (3) and (4), we obtained Eq. (5):

$$N = \frac{\int \tau_{\nu} d\nu \times \rho_{N}}{\int \alpha d\nu} \qquad (5)$$

For our calculation we used an integrated extinction coefficient value of 3.9 × 10³ cm⁻² for the 2013 cm⁻¹ band calculated for the crystalline diacetylene at 70 K by Khanna et al. (1988) and a $\rho_N$ of 9.2 × 10²¹ molecules cm⁻³. The value of the number density is the more important source of uncertainties for this calculation and this value is derived from the mass density using Avogadro's number, and the molar mass of diacetylene (50.06 g mol⁻¹). However, the mass density of crystalline diacetylene is not available in the literature. Thus, we assumed a mass density of 0.76 g cm⁻³ measured for crystalline acetylene at 131 K (Hudson et al. 2014; McMullan et al. 1992). Figure 5 presents the evolution of the consumed C₄H₂ in column density as a function of the photon-fluence for both experiments performed at JPL and PIIM. As explained in Sect. 2.2, a doubled pathlength of absorption due to the reflection-absorption technique used at PIIM was factored in when calculating the column density for the PIIM experiments. We obtained that 2.6 × 10¹⁷ molecule cm⁻² of C₄H₂ were

consumed for a photon-fluence of 3.9 × 10²¹ photons cm⁻² at 355 nm, while 3.4 × 10¹⁷ molecule cm⁻² of C₄H₂ were consumed for a fluence of 4.5 × 10²⁰ photons cm⁻² at λ > 300 nm. These results indicate that a polychromatic photon flux covering a broader wavelength range longward of 300 nm substantially increases the kinetics of the diacetylene photolysis, leading to a slightly higher number of diacetylene molecules consumed with a photon fluence that is ten times lower compared to irradiation performed at 355 nm. We can make the hypothesis that this difference is due to a significant increase in the absorbance of diacetylene between 350 and 300 nm (Fig. 3).

The UV-Vis spectra obtained during the experiments at JPL are presented in Fig. 6; they provide complementary information on the photochemistry of C₄H₂ upon irradiation at 355 nm. We observed the diminution of the diacetylene absorption bands after 60 min of irradiation and then after each successive step of irradiation, in agreement with the IR measurements. In addition, new absorption bands were observed at longer wavelengths: 270, 287, 306, 414, 513, and 575 nm. In addition to these individual bands, we observed an increase in continuum from 260 to 700 nm after each irradiation. A similar absorption continuum was also observed during previous experiments on C₄H₂ ice (Gudipati et al. 2013) and can be attributed to the growth of a polymeric organic material in the ice. The new bands can
be attributed to the production of new species. The bands at 270, 287, and 306 nm can be tentatively assigned to C₆H₂. In the gas phase C₆H₂ has strong absorption bands located at 260, 275, and 293 nm (Jolly & Benilan 2008; Shindo et al. 2003). In the solid phase we observed a shift of the absorption bands of C₆H₂ toward longer wavelengths by about 10 nm compared to the gas phase, as also observed for C₄H₂. We did not observe absorption bands of C₆H₂ in the infrared, but the C₆H₂ absorption bands are most likely buried under the C₄H₂ bands (particularly in the C-H stretch region), which prevents its identification by IR spectroscopy. Other absorption bands at longer wavelengths could not be attributed to a specific compound. Nevertheless, polycyclic aromatic compounds (PAHs) are good candidates to explain these absorption bands because the formation of PAHs has been observed in another experimental study after the irradiation of acetylene ice (C₂H₂) with low-energy electrons (Abplanalp et al. 2019). Further, several PAHs, such as phenanthrene (C₁₄H₁₀), perylene (C₂₀H₁₂; Salama et al. 2011), or larger PAHs (Ruiterkamp et al. 2002), have a strong absorption in the UV at wavelengths shorter than 300 nm and additional weaker absorption bands at longer wavelengths, similar to those observed in Fig. 6. However, the fundamental transition of these PAHs overlaps with the absorption bands of other volatiles, such as C₆H₂, and with the absorption continuum of the polymer. The UV-Vis spectra alone are not specific enough to identify, if formed during the experiments, a single PAH among many other photoproducts. Future work employing other analytical techniques such as chromatography mass spectrometry could provide a better identification of these molecules.

### 3.3. Temperature-programmed desorption (TPD) of the ice after irradiation

After the irradiation of the diacetylene ice at JPL, the sample was warmed under vacuum from 70 to 180 K with a ramp of 1 K min⁻¹ to sublimate all the volatile species formed during irradiation (180 K is the lowest temperature to observe the sublimation of all volatiles). Desorption of several species was tracked as a function of the sample temperature using in situ mass spectrometry. After preliminary experiments in which we recorded mass spectra from m/z 1 to 200 during TPD experiments, we decided to track the thermal desorption of C₄H₂ (C₄H₂⁺, m/z 50) and its hydrogenation products detected by IR spectroscopy, C₄H₄ (C₄H₄⁺, m/z 52). We also monitored the thermal desorption of other, more saturated C₄ species: butyne C₄H₆ (C₄H₆⁺, m/z 54), butene C₄H₈ (C₄H₈⁺, m/z 56), and butane (C₄H₁₀) using its major fragmentation peak (C₃H₇⁺, m/z 43) as the proxy. Finally, we tracked the thermal desorption of C₆H₂ (C₆H₂⁺, m/z 74), which was identified using UV-Vis spectroscopy. We did not observe an increase in the intensity at other masses, except for those corresponding to fragments of these molecules. Figure 7 presents the temperature-dependent desorption profile for m/z 43, 50, 52, 54, 56, and 74.

The C₄H₂ ice remaining after the irradiation is the most abundant species detected during the TPD. Its desorption started at ~80 K with a first peak at 90 K, while the maximum of desorption occurred at ~120 K; a last peak is visible at ~150 K. In a previous study crystalline C₄H₂ was found to start desorbing at ~100 K with maxima at 120 and ~150 K (Zhou et al. 2009). Therefore, our results agree with this previous study. The ion signal at m/z 52 starts to increase at 100 K with a maximum at 120 K, and can be attributed to the desorption of C₄H₄, which was also detected using IR spectroscopy. Finally, ion signals at m/z 43, 54, 56, and 74 started to increase at 110 K with maxima

<figure><img src="image_8.png" /><figcaption>Fig. 7. Temperature desorption profile of m/z 43 (C₃H₇⁺, main fragment of C₄H₁₀), 50 (C₄H₂⁺), 52 (C₄H₄⁺), 54 (C₄H₆⁺), 56 (C₄H₈⁺), and 74 (C₆H₂⁺) after irradiation of C₄H₂ with a laser at 355 nm. The sample was heated (1 K min⁻¹) from 70 to 180 K.</figcaption></figure>

<figure><img src="image_9.png" /><figcaption>Fig. 8. Infrared spectra obtained from non-volatile residue subsequent to C₄H₂ photolysis. Top: IR absorption spectrum of the organic polymer produced during the JPL experiment. Bottom: IR absorption spectrum of the organic polymer produced during the PIIM experiment. The spectra were recorded at ambient temperature at the end of the experiments.</figcaption></figure>

at 120 K, coinciding with maximum desorption of C₄H₂. C₄H₄ is the main volatile product of the C₄H₂ photochemistry detected during the TPD followed by C₆H₂ and C₄H₁₀ (based on C₃H₇⁺, the C₄H₁₀ main fragment). Ion signal variations at m/z 54 and 56 were very low, showing that these two species were produced in a negligible amount compared to the three other hydrocarbons produced. It is likely that C₄H₆ and C₄H₈ are highly reactive compared to the other products.

### 3.4. Organic residues spectra

At the end of the TPD run, each sample was further warmed to room temperature. Figure 8 presents the IR spectra of the organic residues remaining, on the sapphire window (top) in the JPL studies and on the copper surface (bottom) in the PIIM studies, after the sublimation of the ices at room temperature under vacuum. These residues are lightly colored (brownish).
be attributed to the production of new species. The bands at 270, 287, and 306 nm can be tentatively assigned to C₆H₂. In the gas phase C₆H₂ has strong absorption bands located at 260, 275, and 293 nm (Jolly & Benilan 2008; Shindo et al. 2003). In the solid phase we observed a shift of the absorption bands of C₆H₂ toward longer wavelengths by about 10 nm compared to the gas phase, as also observed for C₄H₂. We did not observe absorption bands of C₆H₂ in the infrared, but the C₆H₂ absorption bands are most likely buried under the C₄H₂ bands (particularly in the C-H stretch region), which prevents its identification by IR spectroscopy. Other absorption bands at longer wavelengths could not be attributed to a specific compound. Nevertheless, polycyclic aromatic compounds (PAHs) are good candidates to explain these absorption bands because the formation of PAHs has been observed in another experimental study after the irradiation of acetylene ice (C₂H₂) with low-energy electrons (Abplanalp et al. 2019). Further, several PAHs, such as phenanthrene (C₁₄H₁₀), perylene (C₂₀H₁₂; Salama et al. 2011), or larger PAHs (Ruiterkamp et al. 2002), have a strong absorption in the UV at wavelengths shorter than 300 nm and additional weaker absorption bands at longer wavelengths, similar to those observed in Fig. 6. However, the fundamental transition of these PAHs overlaps with the absorption bands of other volatiles, such as C₆H₂, and with the absorption continuum of the polymer. The UV-Vis spectra alone are not specific enough to identify, if formed during the experiments, a single PAH among many other photoproducts. Future work employing other analytical techniques such as chromatography mass spectrometry could provide a better identification of these molecules.

### 3.3. Temperature-programmed desorption (TPD) of the ice after irradiation

After the irradiation of the diacetylene ice at JPL, the sample was warmed under vacuum from 70 to 180 K with a ramp of 1 K min⁻¹ to sublimate all the volatile species formed during irradiation (180 K is the lowest temperature to observe the sublimation of all volatiles). Desorption of several species was tracked as a function of the sample temperature using in situ mass spectrometry. After preliminary experiments in which we recorded mass spectra from *m/z* 1 to 200 during TPD experiments, we decided to track the thermal desorption of C₄H₂ (C₄H₂⁺, *m/z* 50) and its hydrogenation products detected by IR spectroscopy, C₄H₄ (C₄H₄⁺, *m/z* 52). We also monitored the thermal desorption of other, more saturated C₄ species: butyne C₄H₆ (C₄H₆⁺, *m/z* 54), butene C₄H₈ (C₄H₈⁺, *m/z* 56), and butane (C₄H₁₀) using its major fragmentation peak (C₃H₇⁺, *m/z* 43) as the proxy. Finally, we tracked the thermal desorption of C₆H₂ (C₆H₂⁺, *m/z* 74), which was identified using UV-Vis spectroscopy. We did not observe an increase in the intensity at other masses, except for those corresponding to fragments of these molecules. Figure 7 presents the temperature-dependent desorption profile for *m/z* 43, 50, 52, 54, 56, and 74.

The C₄H₂ ice remaining after the irradiation is the most abundant species detected during the TPD. Its desorption started at ~80 K with a first peak at 90 K, while the maximum of desorption occurred at ~120 K; a last peak is visible at ~150 K. In a previous study crystalline C₄H₂ was found to start desorbing at ~100 K with maxima at 120 and ~150 K (Zhou et al. 2009). Therefore, our results agree with this previous study. The ion signal at *m/z* 52 starts to increase at 100 K with a maximum at 120 K, and can be attributed to the desorption of C₄H₄, which was also detected using IR spectroscopy. Finally, ion signals at *m/z* 43, 54, 56, and 74 started to increase at 110 K with maxima

<figure><img src="image_9.png" /><figcaption>**Fig. 7.** Temperature desorption profile of *m/z* 43 (C₃H₇⁺, main fragment of C₄H₁₀), 50 (C₄H₂⁺), 52 (C₄H₄⁺), 54 (C₄H₆⁺), 56 (C₄H₈⁺), and 74 (C₆H₂⁺) after irradiation of C₄H₂ with a laser at 355 nm. The sample was heated (1 K min⁻¹) from 70 to 180 K.</figcaption></figure>

<figure><img src="image_10.png" /><figcaption>**Fig. 8.** Infrared spectra obtained from non-volatile residue subsequent to C₄H₂ photolysis. Top: IR absorption spectrum of the organic polymer produced during the JPL experiment. Bottom: IR absorption spectrum of the organic polymer produced during the PIIM experiment. The spectra were recorded at ambient temperature at the end of the experiments.</figcaption></figure>

at 120 K, coinciding with maximum desorption of C₄H₂. C₄H₄ is the main volatile product of the C₄H₂ photochemistry detected during the TPD followed by C₆H₂ and C₄H₁₀ (based on C₃H₇⁺, the C₄H₁₀ main fragment). Ion signal variations at *m/z* 54 and 56 were very low, showing that these two species were produced in a negligible amount compared to the three other hydrocarbons produced. It is likely that C₄H₆ and C₄H₈ are highly reactive compared to the other products.

### 3.4. Organic residues spectra

At the end of the TPD run, each sample was further warmed to room temperature. Figure 8 presents the IR spectra of the organic residues remaining, on the sapphire window (top) in the JPL studies and on the copper surface (bottom) in the PIIM studies, after the sublimation of the ices at room temperature under vacuum. These residues are lightly colored (brownish).
<figure><img src="image_10.png" /><figcaption>Fig. 9. UV-Vis absorption spectrum of the organic polymer produced during the JPL experiment. The spectrum was recorded at ambient temperature at the end of the experiment.</figcaption></figure>

Both IR spectra (JPL and PIIM) show an intense absorption band ~3300 cm⁻¹, as illustrated in Fig. 8, attributed to stretching ≡CH. The position and shape of this absorption band of the polymer are similar for the two different C₄H₂ ice photochemistry studies (355 nm laser irradiation at JPL and λ > 300 nm Hg lamp irradiation at PIIM). However, the spectra of the organic films generated at JPL and at PIIM (Fig. 8) also show significant differences between 3100 and 2800 cm⁻¹. The lower-frequency absorptions between 3100 and 3000 cm⁻¹ (due to alkene and aromatic C–H stretch) seen in the PIIM studies are consistently absent in the JPL studies, indicating that the broad range of wavelengths used in the PIIM irradiation (unlike the single laser wavelength used during the JPL experiments) resulted in more unsaturated and aromatic hydrocarbons.

In addition to the IR spectroscopy, the absorption spectrum of the polymer was recorded in the UV-Vis for the sample produced at JPL. The spectrum is presented in Fig. 9. At room temperature, the organic residue presents an intense absorption continuum in the UV, which decreases exponentially in the visible and extends up to 600 nm. Observations of interference fringes between 500 and 900 nm indicate that the polymer residue forms a nonscattering and homogeneous film on the sapphire window. The continuum absorption of the residue does not differ significantly from that observed at 70 K (Fig. 6), indicating that a large part of the polymer is formed during the irradiation of the ice. We observed at room temperature that all the absorption bands attributed previously to C₄H₂, C₆H₂, and tentatively to PAHs have disappeared, leaving only a large continuum. This indicates that most of these species are volatile at room temperature under vacuum, as illustrated by the detection of desorbed C₄ hydrocarbons and C₆H₂ by mass spectrometry during the TPD (Fig. 7). It is also likely that thermal reactions could occur between volatile compounds or between volatile compounds and the polymer during the warming up of the sample, modifying the composition of the polymer, which would be reflected in its UV-Vis absorption spectrum.

# 4. Discussions

## 4.1. Chemical pathways for hydrocarbon formations

Our experiments point out that C₄H₂ is photochemically highly active in the solid phase, leading to the formation of C₆H₂ and

hydrogenated products (C₄H₄, C₄H₆, C₄H₈, and C₄H₁₀). However, we did not find clear evidence of the formation of C₈H₂), which was observed previously in the gas phase irradiation of C₄H₂ (Bandy et al. 1992, 1993). Although it is difficult to identify the reaction mechanism in our experimental conditions, based on literature data (Bandy et al. 1992, 1993), we can try to propose chemical pathways for the formation of the different species observed.

During the JPL experiments, irradiation of C₄H₂ with the laser at λ = 355 nm (3.49 eV or ~28 169 cm⁻¹) can provide enough energy to excite C₄H₂ into the second lowest exited state ³Δₐ, extended between 3.2 and 4.7 eV (~263 nm or ~38 023 cm⁻¹ and ~400 nm or ~25000 cm⁻¹) in the gas phase, as predicted by Allan (1984) and Bandy et al. (1993). This also suggests that the JPL experiments could access the first triplet excited state ³Σ⁺ₐ centered at 3.2 eV (~387 nm or ~25 800 cm⁻¹), which should be involved in the photochemistry observed. Hence, the observed photochemistry must be mediated by the two lowest triplet states (³Σ⁺ₐ or ³Δₐ) reached through direct excitation from the ground singlet state, similar to the mechanism proposed for the C₄N₂ ice photochemistry (Gudipati et al. 2013).

Likewise, for the experiments conducted at PIIM with λ > 300 nm (E < 4.13 eV or ~33 333 cm⁻¹), we can access the UV absorption bands below 4.13 eV. As seen from Fig. 3, and as in the case of the JPL experiments, C₄H₂ can be also excited into the two first excited states ³Σ⁺ₐ or ³Δₐ (Allan 1984) with the lamp and filter combination used at PIIM. However, these two kinds of irradiation (λ = 355 nm and λ > 300 nm) are not sufficient to excite the ¹Σ⁻ₐ (4.8 eV or ~38 800 cm⁻¹) or ¹Δₐ (5.1 eV or ~40 800 cm⁻¹), which are known to induce the C₄H + H and C₂H formation (Bandy et al. 1993). According to the work of Bandy et al. (1993) and more recently Vuitton et al. (2019), at the wavelengths of our work at PIIM or JPL, photochemical reactions are supposed to be initiated from the metastable higher triplet excited state of C₄H₂, instead of the direct photolysis. These reaction channels are illustrated below. They can explain the formation of three compounds observed during our irradiation experiments namely C₄H₄, C₄H₆, and C₆H₂:

$$C_4H_2^*(^3\Delta_u) + C_4H_2 \rightarrow C_8H_3 + H \\ \rightarrow C_6H_2 + C_2H_2, \\ \rightarrow C_8H_2 + H_2 \qquad (6)$$

$$C_4H_2^*(^3\Delta_u) + 2H \rightarrow C_4H_4, \qquad (7)$$

$$C_4H_4^* + 2H \rightarrow C_4H_6. \qquad (8)$$

Bandy et al. (1993) proposed additional routes for the formation of secondary species via the reaction of C₄H₂ with primary products, as illustrated by reaction (9):

$$C_8H_2 + C_4H_2 \rightarrow 2C_6H_2. \qquad (9)$$

This secondary reaction could explain the nondetection of C₈H₂ at the end of our experiment. Bandy et al. (1993) explained that the C₆H₂ formation induces the production of C₂H₂, as previously illustrated in reaction (6). In addition, work from Glicker & Okabe (1987) suggests that C₄H₂ photopolymerization occurred via molecular mechanisms, free radicals being detected only at λ < 180 nm, so it seems highly probable that in both our experiments at JPL and PIIM (irradiations performed at λ > 300 nm and λ = 355 nm) the photochemistry occurred through the metastable triplet excited state pathway and not through the
<figure><img src="image_11.png" /><figcaption>Fig. 9. UV-Vis absorption spectrum of the organic polymer produced during the JPL experiment. The spectrum was recorded at ambient temperature at the end of the experiment.</figcaption></figure>

Both IR spectra (JPL and PIIM) show an intense absorption band ~3300 cm⁻¹, as illustrated in Fig. 8, attributed to stretching ≡CH. The position and shape of this absorption band of the polymer are similar for the two different C₄H₂ ice photochemistry studies (355 nm laser irradiation at JPL and λ > 300 nm Hg lamp irradiation at PIIM). However, the spectra of the organic films generated at JPL and at PIIM (Fig. 8) also show significant differences between 3100 and 2800 cm⁻¹. The lower-frequency absorptions between 3100 and 3000 cm⁻¹ (due to alkene and aromatic C–H stretch) seen in the PIIM studies are consistently absent in the JPL studies, indicating that the broad range of wavelengths used in the PIIM irradiation (unlike the single laser wavelength used during the JPL experiments) resulted in more unsaturated and aromatic hydrocarbons.

In addition to the IR spectroscopy, the absorption spectrum of the polymer was recorded in the UV-Vis for the sample produced at JPL. The spectrum is presented in Fig. 9. At room temperature, the organic residue presents an intense absorption continuum in the UV, which decreases exponentially in the visible and extends up to 600 nm. Observations of interference fringes between 500 and 900 nm indicate that the polymer residue forms a nonscattering and homogeneous film on the sapphire window. The continuum absorption of the residue does not differ significantly from that observed at 70 K (Fig. 6), indicating that a large part of the polymer is formed during the irradiation of the ice. We observed at room temperature that all the absorption bands attributed previously to C₄H₂, C₆H₂, and tentatively to PAHs have disappeared, leaving only a large continuum. This indicates that most of these species are volatile at room temperature under vacuum, as illustrated by the detection of desorbed C₄ hydrocarbons and C₆H₂ by mass spectrometry during the TPD (Fig. 7). It is also likely that thermal reactions could occur between volatile compounds or between volatile compounds and the polymer during the warming up of the sample, modifying the composition of the polymer, which would be reflected in its UV-Vis absorption spectrum.

# 4. Discussions

## 4.1. Chemical pathways for hydrocarbon formations

Our experiments point out that C₄H₂ is photochemically highly active in the solid phase, leading to the formation of C₆H₂ and

hydrogenated products (C₄H₄, C₄H₆, C₄H₈, and C₄H₁₀). However, we did not find clear evidence of the formation of C₈H₂), which was observed previously in the gas phase irradiation of C₄H₂ (Bandy et al. 1992, 1993). Although it is difficult to identify the reaction mechanism in our experimental conditions, based on literature data (Bandy et al. 1992, 1993), we can try to propose chemical pathways for the formation of the different species observed.

During the JPL experiments, irradiation of C₄H₂ with the laser at λ = 355 nm (3.49 eV or ~28 169 cm⁻¹) can provide enough energy to excite C₄H₂ into the second lowest excited state ³Δₐ, extended between 3.2 and 4.7 eV (~263 nm or ~38 023 cm⁻¹ and ~400 nm or ~25000 cm⁻¹) in the gas phase, as predicted by Allan (1984) and Bandy et al. (1993). This also suggests that the JPL experiments could access the first triplet excited state ³Σ⁺ₐ centered at 3.2 eV (~387 nm or ~25 800 cm⁻¹), which should be involved in the photochemistry observed. Hence, the observed photochemistry must be mediated by the two lowest triplet states (³Σ⁺ₐ or ³Δₐ) reached through direct excitation from the ground singlet state, similar to the mechanism proposed for the C₄N₂ ice photochemistry (Gudipati et al. 2013).

Likewise, for the experiments conducted at PIIM with λ > 300 nm (E < 4.13 eV or ~33 333 cm⁻¹), we can access the UV absorption bands below 4.13 eV. As seen from Fig. 3, and as in the case of the JPL experiments, C₄H₂ can be also excited into the two first excited states ³Σ⁺ₐ or ³Δₐ (Allan 1984) with the lamp and filter combination used at PIIM. However, these two kinds of irradiation (λ = 355 nm and λ > 300 nm) are not sufficient to excite the ¹Σ⁻ₐ (4.8 eV or ~38 800 cm⁻¹) or ¹Δₐ (5.1 eV or ~40 800 cm⁻¹), which are known to induce the C₄H + H and C₂H formation (Bandy et al. 1993). According to the work of Bandy et al. (1993) and more recently Vuitton et al. (2019), at the wavelengths of our work at PIIM or JPL, photochemical reactions are supposed to be initiated from the metastable higher triplet excited state of C₄H₂, instead of the direct photolysis. These reaction channels are illustrated below. They can explain the formation of three compounds observed during our irradiation experiments namely C₄H₄, C₄H₆, and C₆H₂:

$$C_4H_2^*(^3\Delta_u) + C_4H_2 \rightarrow C_8H_3 + H \\ \rightarrow C_6H_2 + C_2H_2, \\ \rightarrow C_8H_2 + H_2 \quad (6)$$

$$C_4H_2^*(^3\Delta_u) + 2H \rightarrow C_4H_4, \quad (7)$$

$$C_4H_4^* + 2H \rightarrow C_4H_6. \quad (8)$$

Bandy et al. (1993) proposed additional routes for the formation of secondary species via the reaction of C₄H₂ with primary products, as illustrated by reaction (9):

$$C_8H_2 + C_4H_2 \rightarrow 2C_6H_2. \quad (9)$$

This secondary reaction could explain the nondetection of C₈H₂ at the end of our experiment. Bandy et al. (1993) explained that the C₆H₂ formation induces the production of C₂H₂, as previously illustrated in reaction (6). In addition, work from Glicker & Okabe (1987) suggests that C₄H₂ photopolymerization occurred via molecular mechanisms, free radicals being detected only at λ < 180 nm, so it seems highly probable that in both our experiments at JPL and PIIM (irradiations performed at λ > 300 nm and λ = 355 nm) the photochemistry occurred through the metastable triplet excited state pathway and not through the
involvement of singlet excited states. Similarly, the formation of C₄H₄ seems to be driven by the reaction of C₄H₂\* and H in solid phase (Arrington et al. 1998), as depicted by (reaction (7)). Based on the above analysis, we conclude that C₄H₂ ice photochemistry is driven by the direct photoexcitation into the triplet excited states, as previously observed with C₄N₂ ice (Gudipati et al. 2013). At least, C₄H₈ and C₄H₁₀ could be formed by successive addition of 2H on C₄H₆ and C₄H₈. Such photochemistry is accessible only in the condensed phase, where the spin-selection rules are relaxed for the absorption of a photon by a molecule with other molecules, making ground-state singlet to excited state triplet transitions weakly allowed. As a result, longer-wavelength photons can be absorbed through these transitions and can initiate photochemical reactions.

## 4.2. Implications for Titan's atmospheric and surface chemistry

Our experimental results reveal that the exposure of diacetylene ice particles to near-UV photons ($\lambda > 300$ nm) could drive a complex organic chemistry in Titan's lower atmosphere. However, our results point out that the kinetics of the diacetylene photochemistry vary significantly as a function of the wavelength of the photons used for the irradiation. Our experiments at JPL show that a significant amount of photon fluence ($3.9 \times 10^{21}$ photons cm$^{-2}$) is necessary with a monochromatic laser irradiation at 355 nm to obtain a moderate depletion of diacetylene ice. However, with a polychromatic photon flux (which is expected on Titan) covering wavelengths down to 300 nm, the kinetic of the diacetylene photolysis drastically increases leading to similar diacetylene molecules consumption with a fluence ($4.5 \times 10^{20}$ photons cm$^{-2}$) ten times lower compared to the monochromatic experiments. We can qualitatively understand this difference as being due to a significant increase in the absorbance of diacetylene between 350 and 300 nm (Fig. 3) as well as broadband polychromatic lamp versus monochromatic laser as the photolysis source. Nevertheless, the flux of photons used in our experiments is orders of magnitude larger than that reaching the stratosphere and the troposphere of Titan. To enable a more rigorous quantification of our laboratory data in regard to Titan's conditions, it is necessary to have better modeling studies that estimate photon fluxes at different wavelengths below 350 nm and at different altitudes in Titan's atmosphere. This estimation would allow us to quantify the fraction of the diacetylene ice that could be photolyzed in the atmosphere of Titan during the ice particles sedimentation before reaching the surface.

Moreover, this would allow us to quantify the impact of the solid-phase photochemistry for the composition of Titan's lower atmosphere. This solid-phase chemistry could act as a sink for volatile species such as C₄H₂ in Titan's lower atmosphere and provide a source for other volatile hydrocarbons such as C₆H₂, although these products may be trapped in the ice phase depending on the pressure and temperature. We also expect other atmospheric molecules to precipitate and accrete onto the ice at lower altitudes all the way to the surface. Other major atmospheric molecules of Titan such as HCN and other nitriles, which are known constituents of Titan's ice clouds (Anderson & Samuelson 2011; Anderson et al. 2010; de Kok et al. 2014; Samuelson et al. 1997), could undergo similar reactivity in the solid phase. An analysis of the spectral signatures of ice clouds suggests that those ice particles could be made of co-condensed molecular species (Anderson et al. 2018a). In the case of the co-condensation of a hydrocarbon such as C₄H₂ and a

nitrogen-bearing species such as HCN or HC₃N, solid-phase reactivity likely leads to a coupling of the nitrogen and hydrocarbon chemistry and may initiate the formation of nitrogen containing complex organics, including N-PAHs and possibly biologically important molecules such as adenine (C₅H₅N₅). Overall, this solid-phase reactivity plays an important role in determining the composition of the organic material formed in the atmosphere and that will ultimately contribute to the complex organic molecular, ice, and aerosol diversity on Titan's surface, whose composition will be studied by the future Dragonfly mission.

## 5. Conclusions

Titan's atmosphere is enriched with simple hydrocarbons and nitriles. Some of the most abundant molecules are detected both in the gas phase and in the condensed phase in the atmosphere. Diacetylene is one exception, which is detected in the gas phase but not in the condensed phase. Non-detection of C₄H₂ in the atmospheric ice clouds as well as on the surface of Titan has been a puzzle, for which the results of our laboratory experiments provide a potential rationale:

1. We studied experimentally the photochemistry of solid diacetylene at 70 K under irradiation with photons at wavelengths longer than 300 nm, closely simulating the radiations received by ice particles in Titan's atmosphere. Our experimental results have shown that diacetylene ice is very reactive under these conditions. A total of $2.6 \times 10^{17}$ molecules cm$^{-2}$ of C₄H₂ were consumed after a photon-fluence of $3.9 \times 10^{21}$ photons cm$^{-2}$ at 355 nm while $3.4 \times 10^{17}$ molecules cm$^{-2}$ of C₄H₂ were consumed after a photon-fluence of $4.5 \times 10^{20}$ photons cm$^{-2}$ at $\lambda > 300$ nm, indicating increasing photochemistry yields with decreasing photon wavelengths between 355 nm and 300 nm;

2. We analyzed the evolution of the composition of the solid phase after irradiation using IR and UV-Vis spectroscopy. In addition, we used TPD to analyze the composition of the desorbed species using in situ mass spectrometry. Our results show that the diacetylene photochemistry follows different pathways leading to the formation of different volatile species as well as an organic residue. First, we observed hydrogenation of C₄H₂ to form other C₄H₂n ($n = 2–5$) hydrocarbons. The main photoproduct was C₄H₄ and then C₄H₁₀, while C₄H₆ and C₄H₈ were produced in a negligible amount. Second, the photochemistry of C₄H₂ ice also resulted in the production of larger and highly polymerizable hydrocarbons such as C₆H₂, and presumably aromatics compounds such as PAHs;

3. Finally, we observed the very efficient formation of a tholin-like organic polymer that is stable at room temperature, which has a strong absorption continuum at UV-Vis wavelengths, monotonically decreasing from 200 to 600 nm. Beyond 600 nm no absorption was detected, indicating that the photopolymer could be photochemically activated with photons at wavelengths between 250 and 600 nm either in Titan's troposphere and stratosphere or on the surface. These results agree with our earlier work on other tholins, indicating that this is the general behavior of Titan's organic aerosol analogs;

4. Although diacetylene ice has not been observed yet on Titan, our experimental results highlight the importance that this compound could have for the ice photochemistry in Titan's troposphere and stratosphere. A significant amount of C₄H₂
involvement of singlet excited states. Similarly, the formation of C₄H₄ seems to be driven by the reaction of C₄H₂ and H in solid phase (Arrington et al. 1998), as depicted by (reaction (7)). Based on the above analysis, we conclude that C₄H₂ ice photochemistry is driven by the direct photoexcitation into the triplet excited states, as previously observed with C₄N₂ ice (Gudipati et al. 2013). At least, C₄H₈ and C₄H₁₀ could be formed by successive addition of 2H on C₄H₆ and C₄H₈. Such photochemistry is accessible only in the condensed phase, where the spin-selection rules are relaxed for the absorption of a photon by a molecule with other molecules, making ground-state singlet to excited state triplet transitions weakly allowed. As a result, longer-wavelength photons can be absorbed through these transitions and can initiate photochemical reactions.

## 4.2. Implications for Titan's atmospheric and surface chemistry

Our experimental results reveal that the exposure of diacetylene ice particles to near-UV photons ($\lambda > 300$ nm) could drive a complex organic chemistry in Titan's lower atmosphere. However, our results point out that the kinetics of the diacetylene photochemistry vary significantly as a function of the wavelength of the photons used for the irradiation. Our experiments at JPL show that a significant amount of photon fluence ($3.9 \times 10^{21}$ photons cm$^{-2}$) is necessary with a monochromatic laser irradiation at 355 nm to obtain a moderate depletion of diacetylene ice. However, with a polychromatic photon flux (which is expected on Titan) covering wavelengths down to 300 nm, the kinetic of the diacetylene photolysis drastically increases leading to similar diacetylene molecules consumption with a fluence ($4.5 \times 10^{20}$ photons cm$^{-2}$) ten times lower compared to the monochromatic experiments. We can qualitatively understand this difference as being due to a significant increase in the absorbance of diacetylene between 350 and 300 nm (Fig. 3) as well as broadband polychromatic lamp versus monochromatic laser as the photolysis source. Nevertheless, the flux of photons used in our experiments is orders of magnitude larger than that reaching the stratosphere and the troposphere of Titan. To enable a more rigorous quantification of our laboratory data in regard to Titan's conditions, it is necessary to have better modeling studies that estimate photon fluxes at different wavelengths below 350 nm and at different altitudes in Titan's atmosphere. This estimation would allow us to quantify the fraction of the diacetylene ice that could be photolyzed in the atmosphere of Titan during the ice particles sedimentation before reaching the surface.

Moreover, this would allow us to quantify the impact of the solid-phase photochemistry for the composition of Titan's lower atmosphere. This solid-phase chemistry could act as a sink for volatile species such as C₄H₂ in Titan's lower atmosphere and provide a source for other volatile hydrocarbons such as C₆H₂, although these products may be trapped in the ice phase depending on the pressure and temperature. We also expect other atmospheric molecules to precipitate and accrete onto the ice at lower altitudes all the way to the surface. Other major atmospheric molecules of Titan such as HCN and other nitriles, which are known constituents of Titan's ice clouds (Anderson & Samuelson 2011; Anderson et al. 2010; de Kok et al. 2014; Samuelson et al. 1997), could undergo similar reactivity in the solid phase. An analysis of the spectral signatures of ice clouds suggests that those ice particles could be made of co-condensed molecular species (Anderson et al. 2018a). In the case of the co-condensation of a hydrocarbon such as C₄H₂ and a

nitrogen-bearing species such as HCN or HC₃N, solid-phase reactivity likely leads to a coupling of the nitrogen and hydrocarbon chemistry and may initiate the formation of nitrogen containing complex organics, including N-PAHs and possibly biologically important molecules such as adenine (C₅H₅N₅). Overall, this solid-phase reactivity plays an important role in determining the composition of the organic material formed in the atmosphere and that will ultimately contribute to the complex organic molecular, ice, and aerosol diversity on Titan's surface, whose composition will be studied by the future Dragonfly mission.

# 5. Conclusions

Titan's atmosphere is enriched with simple hydrocarbons and nitriles. Some of the most abundant molecules are detected both in the gas phase and in the condensed phase in the atmosphere. Diacetylene is one exception, which is detected in the gas phase but not in the condensed phase. Non-detection of C₄H₂ in the atmospheric ice clouds as well as on the surface of Titan has been a puzzle, for which the results of our laboratory experiments provide a potential rationale:

1. We studied experimentally the photochemistry of solid diacetylene at 70 K under irradiation with photons at wavelengths longer than 300 nm, closely simulating the radiations received by ice particles in Titan's atmosphere. Our experimental results have shown that diacetylene ice is very reactive under these conditions. A total of $2.6 \times 10^{17}$ molecules cm$^{-2}$ of C₄H₂ were consumed after a photon-fluence of $3.9 \times 10^{21}$ photons cm$^{-2}$ at 355 nm while $3.4 \times 10^{17}$ molecules cm$^{-2}$ of C₄H₂ were consumed after a photon-fluence of $4.5 \times 10^{20}$ photons cm$^{-2}$ at $\lambda > 300$ nm, indicating increasing photochemistry yields with decreasing photon wavelengths between 355 nm and 300 nm;

2. We analyzed the evolution of the composition of the solid phase after irradiation using IR and UV-Vis spectroscopy. In addition, we used TPD to analyze the composition of the desorbed species using in situ mass spectrometry. Our results show that the diacetylene photochemistry follows different pathways leading to the formation of different volatile species as well as an organic residue. First, we observed hydrogenation of C₄H₂ to form other C₄H₂n ($n = 2-5$) hydrocarbons. The main photoproduct was C₄H₄ and then C₄H₁₀, while C₄H₆ and C₄H₈ were produced in a negligible amount. Second, the photochemistry of C₄H₂ ice also resulted in the production of larger and highly polymerizable hydrocarbons such as C₆H₂, and presumably aromatics compounds such as PAHs;

3. Finally, we observed the very efficient formation of a tholin-like organic polymer that is stable at room temperature, which has a strong absorption continuum at UV-Vis wavelengths, monotonically decreasing from 200 to 600 nm. Beyond 600 nm no absorption was detected, indicating that the photopolymer could be photochemically activated with photons at wavelengths between 250 and 600 nm either in Titan's troposphere and stratosphere or on the surface. These results agree with our earlier work on other tholins, indicating that this is the general behavior of Titan's organic aerosol analogs;

4. Although diacetylene ice has not been observed yet on Titan, our experimental results highlight the importance that this compound could have for the ice photochemistry in Titan's troposphere and stratosphere. A significant amount of C₄H₂
ice could be transformed into other volatile molecules, and into organic polymers, and so provide a significant loss process for diacetylene. It is likely that in the case of co-condensation of two or more volatiles, C₄H₂ could trigger the photochemistry through reaction with other hydrocarbons or nitriles, initiating a more complex chemistry in the solid phase.

*Acknowledgements*. Some of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology under a contract with the National Aeronautics and Space Administration. The JPL part of the work was supported by the NASA Solar System Workings and New Frontiers Data Analysis programs. The work carried out at the Physique des Interactions Ioniques et Moléculaires (PIIM) laboratory, Aix-Marseille Université, was supported by the Programme National de Planétologie (PNP).

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