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Home All issues Volume 575 (March 2015) A&A, 575 (2015) A76 Full HTML
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Issue
A&A
Volume 575, March 2015
Article Number A76
Number of page(s) 11
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201425154
Published online 26 February 2015

© ESO, 2015

1. Introduction

The importance of studying the composition of icy mantles that form on dust grains in certain regions of the interstellar medium (ISM), including star-forming molecular cloud cores, is already known, which helps to unveil how such mantles affect the chemistry of the ISM, as well as the abundances of gaseous species that may freeze out onto grains (Teixeira et al. 1998; Whittet 1993; Whittet et al. 1998; Palumbo & Strazzulla 1993; Satorre et al. 2000).

Astronomical data and studies of meteorites show that dust grains are mainly composed of silicate and carbonaceous material. They are mainly formed via gas-phase condensation in the winds of asymptotic giant branch (AGB) stars (Zhukovska & Gail 2007; Gail et al. 2009; Groenewegen et al. 2011; Zhukovska & Henning 2013). Carbon dust is formed in the envelopes of carbon-rich late-type stars as nanosized particles. The observational facts indicate that the chemical processing of the condensed carbon particles has to occur during the transfer from the circumstellar shells into the diffuse interstellar medium or during their stay in this medium (Jaeger et al. 1998). The evolution of carbon dust in the ISM is driven by UV photons, interaction with gas, heating processes, and ion-induced processing due to cosmic rays and to shock waves that accelerate grains, atoms, and ions. Carbonaceous components are discussed as the carrier for the 2175 Å bump in the interstellar extinction curves. Small graphitic grains, hydrogenated amorphous carbon, fullerene-like carbon particles, and even polycyclic aromatic hydrocarbons are some of the possible candidates (Mennella et al. 1996; Draine 2003; Henning et al. 2004). In addition, the far-IR emission of the circumstellar environment of carbon-rich stars and dense molecular cloud cores is believed to be dominated by the emissivity of carbon dust that is assumed to be caused by graphite structures in many dust models (Draine & Lee 1984; Li & Greenberg 1997).

Dust grains are bare in diffuse, low-density clouds, but in dark and dense clouds, the grains are covered with ice mantles such as solid water doped with CO and CO2. Since oxygen is an abundant element, solid O2 is considered as an important constituent of icy grain mantles in dense molecular clouds (Ehrenfreund et al. 1992). However, it is difficult to detect because of its very weak absorption in the IR (Vandenbussche et al. 1999). The gaseous O2 was only detected in low abundances in dense regions of the ISM. Hincelin et al. (2011) argue that the low abundance of O2 in dark clouds can be explained by gas-grain chemical models taking the elemental oxygen depletion into account (Jenkins 2009; Whittet 2010). However, in ices, molecular oxygen is accompanied by ozone in the presence of energetic radiation (Ennis et al. 2011; Gerakines et al. 1996; Raut et al. 2011) and can be traced by O3 in ice layers on interstellar grains.

Much laboratory work has been carried out to characterize the infrared spectra of CO- and CO2-bearing ices of astrophysical interest and their modifications under thermal processing and irradiation (Sandford et al. 1988; Sandford & Allamandola 1990; Palumbo & Strazzulla 1993; Gerakines et al. 1996; Ehrenfreund et al. 1997; Palumbo & Baratta 2000). The interaction of gas with dust grains has an important effect on the chemical evolution of the ISM. Many molecules observed in the ISM can be formed as a consequence of reactions in the ice (Herbst 2005). However, the formation of important species (e.g. H2, H2O and CO2) requires the presence of dust grain surfaces that act as catalysts. The ubiquitous presence of abundant carbon dioxide (CO2) frozen on interstellar ice mantles has already been shown in several ISO and Spitzer results (de Graauw et al. 1996; Guertler et al. 1996; Whittet et al. 1998, 2007; Gerakines et al. 1999; Pontoppidan et al. 2008). Ground-based and satellite-based IR observations have clearly demonstrated the presence of frozen carbon monoxide along the line of sight to young stellar objects embedded in their parent cloud and to field stars obscured by dense molecular clouds (Tielens et al. 1991; Kerr & Adamson 1993; Chiar et al. 1994, 1995, 1998; Teixeira et al. 1998).

CO is the most abundant gas phase molecule in the ISM after H2, and it can directly freeze out on refractory cores. Since CO2 is neither predicted nor observed to have considerable abundance in the gas phase in dense clouds, its condensation on interstellar grains can be negligible (Whittet & Walker 1991). CO and CO2 may be formed as a result of energetic processing, such as UV photolysis and cosmic ray irradiation of ices containing species, such as H2O, CO, CH3OH, O2, and N2 (Gerakines et al. 1996; Moore et al. 1991; Palumbo & Strazzulla 1993; Strazzulla et al. 1997). Other laboratory studies have demonstrated that irradiation of solid CO (Loeffler et al. 2005) or mixtures of CO with water ice or solid O2 (Ehrenfreund et al. 1997; Gerakines et al. 2001; Palumbo et al. 1998; Satorre et al. 2000; Watanabe & Kouchi 2002) can produce CO2. Experiments on the formation of CO and CO2 by energetic processing of carbonaceous surfaces covered by ice mixtures using UV photons and ions were performed by Ioppolo et al. (2009, 2013), Mennella et al. (2004, 2006), Fulvio et al. (2012), and Raut et al. (2012). Furthermore, non-energetic surface formation of CO2 directly on the interface between ice layer and grain may occur because of the reaction of species on grain cores (D’Hendecourt et al. 1985; Ioppolo et al. 2011; Noble et al. 2011).

This paper studies ion-induced interactions at the interface ice/solid in laboratory conditions that simulate the conditions in the ISM experimentally. The laboratory-produced carbon dust analogs produced from 13C were covered with O2 and H2O ice layers and bombarded with 200 keV protons. The formation of CO and CO2 in the ice layer and grain erosion owing to molecule formation were observed and quantified by IR spectral analysis. In addition, sensitive analytic methods were used to investigate the strong structural and morphological modifications of the carbon grains covered by ice layers upon ion bombardment. Comparisons with structural changes of bare carbon grains upon similar ion fluences were performed.

2. Experimental procedure

The experiments were performed in several steps. Carbon layers were produced by laser ablation and deposited on silicon disks and on KBr substrates in the laboratory in Jena. In the following step, the produced carbon layers were covered with ice at the Laboratory for Experimental Astrophysics, INAF-Osservatorio Astrofisico di Catania (Italy) and processed by H+ bombardment. Finally, the irradiation-induced processing of bare carbon particles was studied using the ion implanter at the Institute of Solid State Physics in Jena.

thumbnail Fig. 1

Scheme of the laser ablation setup used for the condensation of graphite.
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2.1. Preparation of carbon grain samples

The gas-phase condensation of fullerene-like nanometer-sized carbon particles was achieved by pulsed laser ablation of a rotating graphite target and subsequent condensation of the evaporated atoms, molecules, and clusters in a quenching gas of He/H2 (2:1) atmosphere at a pressure of 3 mbar. The targets used for the laser evaporation were produced from isotopically pure 13C powder. A scheme of the experimental setup is shown in Fig. 1. A more detailed description of the experimental procedure is given in Jäger et al. (2008) and Sabri et al. (2014). The final thickness of the deposits on either KBr or silicon substrates were in the range of around 120 nm controlled by a microbalance. The measured sample thickness obtained from the microbalance corresponds rather to a compact carbon layer. However, the layer consists of nanometer-sized carbon grains that are agglomerated resulting in a very porous carbon layer of larger thickness (see Sect. 3.3).

The laser ablation is attached to a Fourier transform infrared (FTIR) spectrometer to enable in-situ spectroscopy of the deposited grains. For this purpose, the substrate can be turned for either in-situ IR spectroscopy or for the deposition process.

thumbnail Fig. 2

Schematic top view of the vacuum chamber used for the ion irradiation of the 13C grain/ice layer with 200 keV H+ at the INAF-Osservatorio Astrofisico di Catania.
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2.2. Ion bombardment of carbon grains covered by ice

The carbon particles were covered with O2 and H2O ice and finally bombarded with 200 keV protons. Experiments are carried out in a stainless steel ultra-high vacuum chamber with a base pressure of about 10-9 mbar as shown in Fig. 2. Inside the vacuum chamber, a KBr substrate covered by a particulate fullerene-like 13C film is placed in thermal contact with a closed-cycle helium cryostat, whose temperature was cooled down to 17 K. Water or oxygen was added into the chamber through a needle valve, where they froze onto the substrate. The growth of ices was monitored using an FTIR spectrometer (Bruker Vertex 70) and spectra were acquired in the 7000−400 cm-1 range at a resolution of 1 cm-1. The ice thickness was derived by the laser interference method (e.g. Fulvio et al. 2009) depositing the same amount of H2O or O2 on a clean Si substrate. It turned out that the thickness of the H2O film was about 250 nm (corresponding to 830 monolayers (ML)) and the thickness of the O2 film was about 130 nm (around 400 ML). The vacuum chamber is connected to an ion implanter (200 kV; Danfysik) from which ions of energy up to 200 keV (400 keV for double ionizations) can be obtained. The ion beam produces a spot on the target larger than the area probed by the IR beam. Current densities ranged from 100 nA cm-2 up to a few μA cm-2. In the setup, IR spectra can be obtained before and after ion irradiation without tilting the sample. Spectra were acquired after irradiation at low temperature. The optical depth was calculated from the transmission by using the OPUS 86 software. This enabled us to monitor further changes in profile of the CO2 bands upon further irradiation with 200 keV protons. The solid 13CO2 has an IR absorption band at 2275 cm-1 (4.40 μm) which is shifted from the 2345 cm-1 (4.26 μm) band of solid 12CO2. Furthermore, the absorption bands of solid 13CO2 are shifted from those of residual gaseous 12CO2 present in the external path of the infrared beam, a perturbation that is present only when the quality of the dry air purge is not optimum (Raut et al. 2012).

In this series of experiments listed in Table 1 , three different carbon samples were used for the deposition of ice layers and ion bombardment with 200 keV protons at various fluences. In experiment No. 1, a 12C sample was covered by an H2O ice layer only one time and subjected to irradiation with 200 keV H+ up to the maximum fluence of 7.8 × 1015 ions/cm2. Similarly, in experiment No. 2, a 13C sample was covered by an H2O ice layer and irradiated with 200 keV H+ with the maximum fluence of 9 × 1015 ions/cm2. The carbon grain sample in experiment No. 3 from 13C was used for multiple O2 and H2O depositions along with proton bombardment at maximum fluences of 6.57 × 1015, 1.65 × 1016, 1.65 × 1016, 1.15 × 1016, and 1.65 × 1016 ions/cm2. This corresponds to the total fluence of 6.76 × 1016 ions/cm2. After each individual bombardment experiment, the ice layer was removed by annealing to room temperature, and a new ice layer was deposited on the bare grains for the following experiment. In all our experiments, the penetration depth of impinging ions is greater than the thickness of the ice layer. According to SRIM (Stopping and Range of Ions in Matter) calculations, the penetration depth of 200 keV protons impinging at 45° is about 1 μm for both cases of 250 nm H2O ice layer and 130 nm O2 ice layer on top of an amorphous carbon layer with a density of 1.7 g/cm3 (Ziegler et al. 2010).

Table 1

Ion bombardment experiments with 200 keV H+ ions performed at INAF, Catania.

Table 2

List of molecules observed after irradiation with 200 keV H+ ions in different ices together with their band positions and strengths used to evaluate their column densities.

2.3. Ion bombardment of carbon grains without ice layer

Bare carbon grains were bombarded with 200 keV protons. The aim of these experiments were to compare and monitor the structural changes of carbon surfaces covered by ice with those having no ice layers under ion irradiation. For this reason, fullerene-like particulate carbon layers produced from both 12C and 13C were prepared by the laser ablation technique as already mentioned in Sect. 2.1. The carbon layers were deposited on silicon substrates. To compare the results of these experiments with the ones performed in Catania, we applied 200 keV H+ ions and a maximum fluence of 7 × 1016 ions/cm2. The sample was cooled down to 16 K during the experiments.

2.4. Analytical characterization

Because of the very complex structure of carbon materials, they have to be analyzed by different methods. In order to characterize as-produced and processed carbon materials, ambitious analytical methods such as high-resolution transmission electron microscopy (HRTEM) and field emission scanning electron microscopy (FESEM) were used. In addition, Fourier-transform infrared (FTIR) spectroscopy was performed in transmission in the wavelength range between 400 and 4000 cm-1. HRTEM gives us a direct view inside the grains and unveils the information on the structure, sizes, and shapes of the grains. With this method, one can distinguish between ordered and amorphous structures, or between plane and bent graphene layers. A JEOL JEM-3010 TEM microscope equipped with a LaB6 cathode operating at 300 kV and a point resolution of 0.21 nm was used. HRTEM images were recorded digitally with a CCD camera and analyzed by the Gatan Digital Micrograph 3.9.0 software. FESEM is performed with a field-emission SEM (Zeiss (LEO) 1530 Gemini). The resolution of the microscope depends on the material but it can be 2 nm in maximum. This special technique was used to provide information on the morphology of the condensed layers.

3. Results

3.1. CO and CO2 formation in ices under ion bombardment

It is already well studied that ion irradiation of simple ices produces new species both more and less volatile than those initially present in the sample. Both CO and CO2 can be obtained when mixtures containing simple molecules of astrophysical interest (e.g. Moore et al. 1991, 1996; Strazzulla et al. 1993; Palumbo et al. 1998) are irradiated.

In our experiments, the evolution of CO and CO2 in H2O and O2 ice layers bombarded with 200 keV protons was observed. In Table 2, peak positions and band strengths of these molecules are given that are considered to evaluate their column densities. Furthermore, we analyzed the morphology and spectral properties of 13C before and after processing.

thumbnail Fig. 3

IR spectra of amorphous 13C (solid line), amorphous 13C after H2O ice deposit (dotted line) and after O2 ice deposit (gray solid line) along with irradiation of 200 keV H+ (experiment No. 3 in Table 1).
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The baseline-corrected IR transmission spectra of the as-produced and processed 13C grains are presented in Fig. 3. OH-stretching bands at around 3300 cm-1 are seen in the spectra of carbon samples covered with ices. Only weak aliphatic C–H stretching bands between 2800–3000 cm-1 (3.4 μm) have been detected in the spectrum. In addition, weak features at 1430 and 1375 cm-1 are assigned to aliphatic CH-deformation vibrations. But small features between 1605 and 1610 cm-1, observed in all samples, confirm the existence of aromatic -C=C- bonds in the carbon structure. The hydrogen is mainly incorporated as saturated -CH2 or -CH3 groups probably acting as bridges between bent aromatic subunits. For more details on the fullerene-like structure and IR properties of the original condensate, we refer to the paper published by Jäger et al. (2008). In addition, narrow features of 12CO, 13CO, 12CO2, and 13CO2 molecules are distinguished in the spectrum. There is a clear shift that is about 50 cm-1 for CO and 65 cm-1 for CO2. Only the 13CO and 13CO2 molecules are formed from carbon atoms of the particulate material. The decrease in the intensity of aliphatic C–H stretching modes is related to the abstraction of hydrogen from the solid carbon structures. The decreasing intensity of the water absorption band at 3300 cm-1 in the spectra of the H2O ice-covered carbon grains is accompanied by the appearance of CO and CO2 stretching bands, which develop during irradiation. Besides this, the C≡C stretching band at 2110 cm-1 slightly increases by proton irradiation. The latter band is related to processing of carbon grains.

The column densities of CO and CO2 for common 12C and 13C at different ion fluences were calculated. To estimate the abundance of solid molecules in both laboratory samples and along the line of sight to molecular clouds, it is essential to convert the transmission spectra If into optical depth units τ(ν) = ln(I0/If), where I0 is the intensity of the incident radiation (Ioppolo et al. 2009). After the baseline correction by a linear fit, the band area is calculated and finally divided by the band strength for the given molecules, listed in Table 2, to derive the column density for each considered species. We observed that by increasing the fluence of ions, the amount of CO and CO2 increases. Only the 13CO and 13CO2 molecules are formed from carbon atoms of the particulate material.

To check the origin of 12CO2 and 12CO bands in our spectra, we carried out control experiments where only O2 ice was deposited on an inert Si substrate and irradiated at 17 K with 200 keV H+ ions up to fluences of 1.6 × 1016 ions/cm2. 13CO and 13CO2 were not spectroscopically detected. In addition, we observed that the column density of 12CO and 12CO2 is more than one order of magnitude lower than the column density measured when O2 is deposited on C grains. Consequently, a part of the 12CO and 12CO2 must have been formed in the ice layer, on top of the carbon, upon ion bombardment. From previous studies, we know that the condensed grains easily adsorb molecules on their surfaces. Therefore, we conclude that the 12CO and 12CO2 molecules exclusively result from a layer of 12C carbon-bearing molecules physisorbed on the surface of the fullerene-like grains after exposure to air.

Our results clearly indicate that the carbon particles of the layer beneath the ice are partly eroded. They have contributed to the formation of CO and CO2 molecules in the ice layer. This is proved by the formation of 13CO and 13CO2. When O2 is the only oxygen-bearing molecule, CO2 is probably formed from CO via the following reactions similar to a mechanism proposed by Fulvio et al. (2012): The efficiency of CO and CO2 formation in an H2O ice layer is about one-fifth of its efficiency in an O2 ice layer. The oxidation process that is responsible for the formation of CO and CO2 is probably different to the one observed in O2 ice. An impinging ion X can directly break a water molecule: Near the carbon-water interface, OH radicals can react with the carbon to form CO2 in steps via creation of an intermediate CO, since it is unlikely that two OH radicals are available to oxidize a single carbon atom at the same instant as explained in more detail in Raut et al. (2012):

3.2. Estimation of missing C after ion bombardment

The bombardment experiments have clearly proven that the formation of 13CO and 13CO2 was at the expense of solid carbon grains. We, therefore, estimated the amount of carbon removed from the carbon particles by the formation of CO and CO2 in the experiments No. 3a–e. Based on the column density of 13CO and 13CO2 plotted as a function of the fluence, the formation rate of 13CO and 13CO2 in this experiment was calculated. The experimental data were fitted by an exponential curve y = A(1−e− σΦ), where y is the 13CO or 13CO2 column density (molecules/cm2), A the asymptotic value (molecules/cm2), σ the total cross section (cm2/ion), and Φ the proton fluence (ions/cm2). The formation rate, R (molecules/ion), was calculated by A×σ. Figure 4 shows the column density of 13CO and 13CO2 acquired at different fluences of 200 keV protons upon irradiating an O2 ice layer deposited on a 13C grain layer and the corresponding fit curve.

thumbnail Fig. 4

Column densities of 13CO (lower graph) and 13CO2 (upper graph) versus the fluence. The formation rates of both molecules were derived from the fit of the experimental data with a standard deviation of δR = ± 0.38 (molecules/ion).
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Summing up the data of all five irradiation experiments (3a–e), we obtained a total number of 5.09 × 1017 carbon atoms/cm2 converted from the solid carbon into 13CO and 13CO2 molecules. This is calculated from the formation rate of 13CO and 13CO2 multiplied by the total fluence 6.76 × 1016 ions/cm2.

The amount of C removed from the particulate carbon layer was calculated by the formation rate, i.e. 4.7 molecules/ion for 13CO2 and 2.9 molecules/ion for 13CO, multiplied by the number of ions calculated from the total fluence 6.76 × 1016 ions/cm2 multiplied by the area of the irradiated surface, which gives 5.32 × 1016 ions. Finally, we obtained a total number of removed carbon molecules or atoms of 4 × 1017 molecules.

Based on the volume of the carbon layer that was irradiated, we determined the number of originally available carbon atoms. The fraction of atoms that was transferred into molecules from the solid corresponds to about 50%. In our study, we removed a carbon layer of about 60 nm from the original carbon film with 5.32 × 1016 ions corresponding to 1.13 × 10-15 nm/ion erosion rate. The reduction of the carbon layer thickness by about 50% is also visible in the FESEM image that shows the topography of the irradiated and nonirradiated parts of the sample (Fig. 5).

thumbnail Fig. 5

Topographic view produced from a FESEM micrograph showing the erosion of the carbon layer after ion bombardment with 6.76 × 1016 protons/cm2. The left part is the bombarded area whereas the right and bright surface represents the nonirradiated part of the sample. The scale on the right side corresponds to the layer thickness.
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3.3. Structural modifications of the carbonaceous material under ion bombardment

The HRTEM provides information on the level of ordering in the primary particles by imaging graphene subunits or lattice fringes of graphite-like structures. It is already known that the possibilities for carbon forming solid structures are extremely manifold. Tetrahedrally coordinated carbon atoms in the sp3 hybridization state can build up either diamond or diamond-like amorphous structures, whereas sp2 hybridized carbon atoms form planar structures (graphite or graphite-like). Apart from these two distinct hybridization states, mixed hybridization characterized by curved structures is possible (fullerenes or fullerene-like structures). In a carbon grain, all kinds of hybridization states (sp, sp2, sp3, and curved graphene layers) may occur together.

The gas-phase condensed grains used in this study are built of amorphous, fullerene-like structures, the same as those obtained by laser ablation of graphite in quenching gas atmospheres (Jäger et al. 2008). The comparison of 12C and 13C particulate carbon layers does not show any structural difference in the condensates. Figure 6 presents images of fullerene-like carbon before ion irradiation. The fullerene-like structure arises from the presence of bent and cross-linked graphene planes. The very fluffy agglomerates are dominated by chain-like arrangements of particles. Finally, a very porous carbon layer composed of small fullerene-like grains was observed in the micrographs. Individual grains were found to range between 1 and 3 nm. In addition, fullerenes of different sizes are observed in the condensate.

thumbnail Fig. 6

HRTEM image of fullerene-like carbon grains before ion bombardment. The inset demonstrates the cross-linking between the bent graphene layers. The arrows mark individual fullerenes between the grains.
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thumbnail Fig. 7

HRTEM images of the carbon structures after ice deposition and irradiation-induced processing (sample 3e in Table 1). The upper image shows a strongly processed area of carbon material representing graphitic structures. The lower image displays material that is less processed compared to the top layer. It still shows a similarity to the original fullerene-like material but with longer graphene layers.
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The 13C particulate sample produced by laser ablation was used for five experiments (3a–e) comprising ice deposition with O2 or H2O and subsequent ion bombardment of the grain/ice layer after each deposition. Therefore, the carbon layer (sample No. 3) should show the utmost changes in structure and morphology. Ion-irradiation of O2 or H2O ice on carbonaceous dust grain surfaces that act as a reservoir of carbon triggers reactions between the carbon and the ice at the interface. C–C and C–H bonds are dissociated by the energetic ions, and finally, CO and CO2 molecules are formed. Besides the formation of molecules, structural rearrangements in the remaining carbon can be observed. Figure 7 shows an HRTEM image of 13C grains after proton bombardment. The upper image provides insight into a strongly processed area of carbon material observed at the interface between grains and ice. Fibers showing the typical lattice fringes of graphitic structures (d002 = 0.365 nm) can be observed. The graphitic material was clearly produced from the original fullerene-like material upon the proton bombardment.

The FESEM images (Fig. 8) confirm that graphitization occurred in a surface layer after the intensive bombardment. This surface layer can be clearly distinguished from the grain-like structure underneath. In addition, the growth of the grains and densification of agglomerates are visible. The thickness of the graphitic layer was estimated to be in the range of 30 to 50 nm.

thumbnail Fig. 8

FESEM image of carbon grains before (lower image) and after 200 keV proton bombardment with 6.76 × 1016 ions/cm2 (top image).
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To interpret the results of structural modifications by proton bombardment, the interaction of protons with the target material has to be understood. The penetration depth of 200 keV protons into a very porous layer of carbon grains, covered by either 130 or 250 nm of O2 or H2O ice, respectively, is difficult to determine by SRIM calculations. Assuming a dense, non-porous carbon layer, the thickness measured by means of a quartz micro balance, was about 120 nm. SRIM simulations, which take a non-porous carbon layer with the density of 2.2 g/cm3 beneath the ice into account, calculated penetration depths between 220 and 330 nm. The protons are finally stopped in the KBr substrate. However, the chain-like, porous structure of the grain agglomerates is much less dense, resulting in a real layer thickness ranging between 900 and 1100 nm and corresponding to a density of around 0.35 g/cm3. During their trajectory, they lose energy and deposit this energy in the target mainly in the form of electronic energy. Consequently, ionization and bond breaking, as well as annealing processes, are triggered in the material. These processes are responsible for the structural modification of the fullerene-like grains. However, a gradual modification of the carbon material is observed from the surface to the bottom of the carbon layer. Beneath the strongly graphitized upper layer, we observe less processed carbonaceous material characterized by longer graphene layers than in the original material, and distinct grain structures. The different levels of carbon grain processing are shown in Fig. 9. In addition, the formation of more closed buckyonions and finally less modified grains with abundant fullerenes are observed. The energetic protons cause the abstraction of H from aliphatic -C–H bonds in the periphery of fullerene-like aromatic structures. Infrared analysis recorded during the irradiation experiments confirmed the destruction of C–H bonds under irradiation. Consequently, reactions between dangling bonds at the periphery of fullerene fragments can lead to the formation of fullerenes and bucky onions of different sizes. This scenario corresponds well to the results seen in the HRTEM analysis.

To understand the processing of carbonaceous materials upon ion bombardment, bare carbonaceous material (without ice layer) was studied. It should be noted that the fluence of protons was comparable to the total proton fluence used for the ice-covered sample 3 (a–e). Figure 10 presents the HRTEM analysis of the processed carbonaceous grains. Generally, an identical gradual processing of the carbon material as shown in Figs. 8 and 9 could be detected. On the surface, the formation of graphitic structures was observed. However, this graphitic layer was smaller compared to those observed in the ice-covered sample. A possible explanation could be that the dissociation of bonds and formation of atoms in the ice layer may contribute to the graphitization process at the interface ice/grains. They can additionally react with C–C and C=C bonds in the carbon grains and therefore increase the rate of bond dissociation in the carbon layer upon ion bombardment.

thumbnail Fig. 9

Series of images presenting material with different levels of proton-induced processing. The three types of carbon structures were observed underneath the graphitic layer after complete bombardment of sample 3 with the total fluence of 6.76 × 1016 ions/cm2. The particles are still visible, but they contain longer graphene layers compared to those observed in the original grains. In addition, one can see the formation of more closed buckyonions and fullerenes. The right micrograph finally shows grains, which are still similar to the unprocessed fullerene-like grains.
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thumbnail Fig. 10

Graphitic structures observed after bombardment of bare carbonaceous grains with 200 keV protons at total fluence of 6.76 × 1016 ions/cm2 (left). Fullerenes and bucky onions (middle), detected beneath the graphite layer, demonstrate the conversion of curved fullerene fragments into more closed structures (right).
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4. Astrophysical applications

4.1. Implication for molecular formation and erosion of solid carbon for molecular clouds and protoplanetary disks

Interactions between ice and grains are expected in the ISM, such as in dense molecular clouds, in clouds with embedded protostars, or in protoplanetary disks, where dust grains coated with ice are continually bombarded by GeV cosmic rays or stellar winds.

Solid CO and CO2 are the foremost molecules formed at low temperature after processing of C- and O-bearing ices. In the cold ISM, the formation of observed CO2 could be due to oxidation of the abundant solid CO. In this process, oxygen atoms may plate out onto grains in dense clouds or result from the dissociation of adjacent molecules in the ice, such as O2 or H2O by Lyα photons, cosmic rays, or stellar wind ions. Raut & Baragiola (2011) find that the reaction of CO and cold O atoms is relatively inefficient at making CO2, mostly because oxygen reacts primarily with O atoms to form O2 and O3. The presence of CO ice in grain mantles is generally explained in terms of direct condensation of CO molecules from the gas phase. On the other hand, it is thought that CO2 forms in the solid phase through grain surface reactions and energetic processing of ice mantles. Former laboratory results (Ioppolo et al. 2009, 2013) not only account quantitatively for the column density of observed interstellar CO2 but also provided a good spectroscopic analog of the interstellar features supporting the hypothesis that interstellar solid CO2 is formed after ion irradiation and UV photolysis of icy mantles. This, however, does not exclude the possibility that other formation routes, such as grain surface reactions, contribute to the production of the observed interstellar solid CO2.

Our experiments have shown that CO and CO2 are formed from the solid phase. That means that solid carbon is eroded not only by supernova shock waves but also by ion-induced molecule formation in ices deposited on carbon grains. Assuming that ice deposition and simultaneous ion irradiation may occur repeatedly, such processes may drastically reduce the amount of solid carbon in the ISM and in other astrophysical environments.

The erosion of carbon grains due to CO and CO2 formation at the interface between carbonaceous grains and ice layers is not well known yet. Our experiments have provided quantitative results on the level of carbon-grain erosion. A total irradiation fluence of 6.76 × 1016 H+ cm-2 applied to ice-covered carbon grains has resulted in the erosion of about 50% of the solid material here considered. The applied fluence is equivalent to the proton bombardment during the grains’ lifetime of about 108 years in dense molecular clouds. Based on the assumption of an effective monoenergetic ion irradiation between 1 and 9 MeV protons cm-2 s-1, an astrophysically relevant fluence of 3.2 × 1015 to 2.9 × 1016 protons cm-2 during the lifetime of a grain can be calculated (Mennella et al. 2004). The thickness of the ice layers used in our study is much smaller than expected for ice layers in dense molecular clouds. Based on experimental studies performed by Lamberts et al. (2014), ice layers of more than a few thousand monolayers for water ice are realistic. As a result, the erosion efficiency provided in this paper represents an astrophysically relevant quantity.

The results presented in this paper confirm previous findings that CO and CO2 are formed after ion bombardment and UV photolysis of C-grains covered by water and oxygen ice (Mennella et al. 2004, 2006; Gomis & Strazzulla 2005; Fulvio et al. 2012; Raut et al. 2012). Similarly, in our experiments with H2O and O2 ice deposits, the intensity of the aliphatic C–H stretching modes of the CH2 and CH3 functional groups at 2950, 2925, and 2860 cm-1 decreases. The same trend is observed for the associated C–H bending modes at 1457 and 1378 cm-1.

The surface chemistry model predicts that CO molecules, which are present in the grain mantle, react with accreting atomic oxygen to form CO2. In the case of energetic processing of ice mantles, carbon dioxide forms by reaction of C-bearing molecules (primarily CO) with O atoms, OH radicals and coming from the dissociation of other molecules present in the mantles (mainly H2O and O2 in the polar and nonpolar phases, respectively). A common aspect of these formation schemes is the presence of C atoms in C-bearing species (mainly CO) in the ice mantles. However, the performed study reveals the formation of CO from reactions between solid carbon and oxygen-bearing ice at the interface. This has been explicitly demonstrated by the detection of 13CO and 13CO2. The CO turns into CO2 by further oxidation. The findings should have strong influence on existing chemical models for the formation of CO and CO2.

Lee et al. (2010) have shown that the bulk composition of the Earth is very carbon poor compared to the material available at formation. The deficiencies of solid carbon extends into the asteroid belt. It implies that carbon is already missing in the initial steps of planet formation including the growth of submicron silicate and carbon grains in the solar nebula. The authors have discussed a mechanism wherein pristine carbon grains are primarily destroyed by oxygen atoms. Our experimental results on ion-induced erosion of solid carbon provide another mechanism for the destruction of carbonaceous solids and the abundant formation of CO and CO2. The formed CO and possibly CO2 could be the origin of more complex organic materials finally incorporated into planetesimals and cometesimals (Bergin et al. 2014). This represents an additional source for organic carbonaceous material in meteorites and comets.

4.2. The survival of carbon dust on the surface of icy objects in the solar system

The surfaces of most of the satellites of Jupiter, Saturn, and Uranus are dominated by the presence of water ice, with traces of other species among which are carbon dioxide (CO2), and non-ice species that include sulfur and carbon-bearing solid materials (for a recent review see Clark et al. 2013). Carbon dioxide has been detected on the surfaces of some icy objects such as Europa, Ganymede and Callisto (McCord et al. 1997, 1998; Hibbitts et al. 2002, 2003): on the surface and in the exosphere around the Saturnian satellites Rhea and Dione (Teolis et al. 2010; Teolis & Waite 2012) and on Ariel, a Uranian satellite (Grundy et al. 2003).

Most of these icy objects are embedded in the magnetospheres of their respective planets and consequently are exposed to very intense fluxes of energetic ions and electrons. Energetic processing produces a number of effects such as sputtering (Baragiola 2005; Johnson et al. 2008), structural alteration (Baratta et al. 1991; Moore & Hudson 1992; Leto & Baratta 2003; Famá et al. 2010) and chemical processing (Moore et al. 2001; Strazzulla et al. 2001; Jones et al. 2011) that, for decades, have been simulated in the laboratory (for a recent review see Strazzulla 2011). As an example, chemical alteration leads to the formation of hydrogen peroxide (H2O2) as demonstrated by many experimental results (Moore & Hudson 2000; Gomis et al. 2004; Loeffler et al. 2006; Zheng et al. 2006) and has been found on the surface of Europa (Carlson et al. 1999), Ganymede and Callisto (Hendrix et al. 1999).

The results presented are relevant to contributing to a better understanding of the so-called “carbon cycle” in which the carbon-bearing species observed on the icy moon-carbon-based solid materials, carbonates (and carbon chains), and CO2 are continuously recycled. It has already been suggested that the observed carbon dioxide is produced by radiolytic processes induced at the interface between water ice and solid carbon (Gomis & Strazzulla 2005), possibly delivered as carbonaceous grains from micrometeorites and interplanetary and/or interstellar dust bombardment. These results reinforce that suggestion and allow us to evaluate the “lifetime” of carbonaceous materials present on the surfaces of the icy moons. In fact, once deposited on the icy surfaces, a carbonaceous grain will be rapidly covered by the abundant water ice and irradiated by the environmental energetic

ion (and electron) populations. The lifetime of a carbon layer covered by water ice is given by (1)where τ (years) is the lifetime of a carbon layer of thickness d (atoms cm-2), Φ represents the ion flux (ions cm-2 s-1), and Y the total yield of C atoms removed per impact. The high-energy magnetospheric ion populations bombarding the surfaces of the icy moon are dominated by protons at energies of 10−1000 keV that are perfectly simulated by the present experiments. As examples, Madey et al. (2002) report the flux of ions at the surface of Europa and Dione to be 3 × 108 and 1012 cm-2 s-1, respectively. Assuming that the yield of carbon atom removal is, for all of the ions, the same as measured in the present experiment, i.e. 4.7 carbon atoms/ion, we can evaluate by Eq. (1) the lifetime of a grain (or a layer) having a thickness of 1020 atoms cm-2, i.e. of about ten micrometers. The result is τ = 2.2 × 103 years for a grain on the surface of Europa and τ = 0.7 years on Dione. These are very short times that allow the carbon atoms delivered as solid material on the surfaces to be converted in icy species (mostly CO2 and CO) and become available for a further radiolytic-induced chemical (or even biological) processing. Once formed, carbon dioxide is in fact mixed with water ice (and other trace species). Energetic processes then induce the formation of carbonic acid as demonstrated by several experiments (Boduch et al. 2011; Gerakines et al. 2000; Peeters et al. 2010; Pilling et al. 2010; Zheng & Kaiser 2007); this could be a first step in further chemical evolution particularly where additional icy species are present. Irradiated mixtures also present a “red” continuum in the UV that mimic some astronomical observations well, as recently demonstrated (Jones et al. 2014).

It is obviously relevant to evaluate the number of carbon atoms that, when delivered on the surfaces of icy satellites, is converted to CO2 first and is then available for a chemical evolution. In a recent review of the space weathering of solar system bodies, Bennett et al. (2013) report the available data on the mass flux of dust on the surfaces of several objects in the solar system (see their Table 3). While those fluxes are not known for objects in the Jupiter system, they are available for the Saturnian and Uranian systems. At Dione the flux is estimated to be 1.4 × 1016 g cm-2 s-1 (Porter et al. 2010). Assuming that 1% of the delivered mass is made of carbon and in view of the fast transformation of solid carbon in carbon dioxide, we can estimate the total amount of carbon that is converted in 3.5 × 109 years (i.e. from the end of the late heavy bombardment). The result is that as much as 0.15 g cm-2 can be converted on the surface of Dione. When integrated over the surface area of the satellite (4 × 1016 cm2), this number results in 6 × 1015 g. This is a large number that induces us to conclude that this process is extremely relevant and allows large quantities of solid carbon to be converted and participate in the chemical evolution of icy bodies.

4.3. Consequences of ion-induced structural changes of carbonaceous dust

Our experimental studies have demonstrated that ice-covered or bare fullerene-like carbon grains undergo strong structural modification upon 200 keV proton bombardment. The fullerene-like carbon grains are very small and rich in defects. They are characterized by very large and reactive surfaces and therefore, the process of CO and CO2 formation from the carbon reservoir of the grains is very efficient. A similar reactivity is expected for hydrogenated amorphous carbon, but grains composed of large and plane graphene layers or of graphitic subunits should show less reactivity owing to a higher stability of the aromatic –C=C– bonds compared to single bonds and a low content of –C–H groups. Therefore, a less efficient CO and CO2 formation at the end of the lifetime of a grain and a saturation effect could be possible. However, quantitative studies of the erosion of graphitic materials are still missing. The bombardment of icy and bare carbonaceous grains irradiated with comparable fluences of 200 keV protons show slight differences in structural modifications. The graphitization of bare grains is less efficient than icy carbon grains. Generally, the electronic energy loss of the penetrating ions causes ionization, bond breaking, and annealing in the target material. Consequently, the restructuring of carbon bonds and the final graphitization of grains can be expected. However, the different levels of graphitization between icy and bare grains have not been completely understood so far. The ice layer and the formation of CO and CO2 may also influence the graphitization process.

The observed structural changes have a strong influence on the spectral properties of carbonaceous material. The absorption efficiency in the IR up to the submillimeter range is higher for graphitic material than for hydrogenated amorphous or fullerene-like carbon materials and the strength of C–H bands due to C–H vibrations (such as 3.4, 3.3, 6.8, and 7.3 μm) is decreased (Jaeger et al. 1998). The absorption efficiency Qabs of carbonaceous particles in the far-IR follows the power law Qabs/a ~ λ− β, where a is the radius of the particles. The spectral index β depends strongly on the internal structure of the carbon materials. Beta ascends from about one to two for spherical grains with increasing graphitization as predicted by theory. However, absorption coefficients of graphitic materials depend strongly on the morphology of the grains in the far-IR range. Calculations of the absorption efficiency of a continuous distribution of ellipsoids that simulates the agglomeration of grains show that graphitized carbon grains have a much lower index. This is caused by percolation effects, which are present in graphitized samples that contain free charge carriers. In the case of conducting materials such as graphite, an increase in the far-IR opacity and a flat absorptivity are expected for aggregated particles or deviations in the shape of particles from a sphere (Stognienko et al. 1995; Henning et al. 1995). Therefore, structural modifications of carbonaceous materials and erosion of grains have to be considered in the relevant dust models.

5. Conclusions

The formation of CO and CO2 molecules was studied upon the 200 keV H+ bombardment of O2 and H2O ice-coated carbonaceous grains at the interface between ice and grains. The grains were produced from 13C graphite targets by gas-phase condensation. We showed that CO and CO2 were formed, and the total number of CO and CO2 molecules removed from the carbon upon ion irradiation was determined to be 4 × 1017 atoms (see Sect. 3.2). These molecules are exclusively formed from the carbon grains. We have determined the number of originally available carbon atoms based on the volume of the carbon layer that was irradiated. The fraction of atoms that are transferred into molecules from the solid corresponds to about 50%. In our study, we have removed a carbon layer of about 60 nm from the original carbon film with 5.32 × 1016 ions corresponding to 1.13 × 10-15 nm/ion erosion rate for an oxygen ice layer.

The lifetime of a grain (or a layer) having a thickness of 1020 atoms cm-2, i.e. of about ten micrometers on icy objects of the solar system, was calculated on the basis of our experimental results. The result is τ = 2.2 × 103 years for a grain on the surface of Europa and τ = 0.7 years on Dione. The calculated lifetimes demonstrate that the solid carbon can easily dissipate by conversion into CO2 and CO and finally become available for further radiolytic-induced processing.

Furthermore, structural and morphological changes in the icy and bare carbonaceous grains processed by ion irradiation with 200 keV H+ were studied. Graphitization of the upper layer and graded processing of the carbon material in dependence on the penetration depth of the ions were observed. Less graphitization, characterized by longer graphene layers and more closed fullerene molecules/structures, compared with the original material were observed beneath the graphitic layer. The structural changes strongly affect the spectral properties of the carbonaceous material, especially in the far-IR.

The presented results based on bombardment experiments with 200 keV protons also have consequences for the formation of more complex molecules in molecular clouds, protoplanetary disks, and the solar system and for recent dust models of the ISM (Draine 2009; Jones et al. 2013).

Acknowledgments

T.S. is supported by the European Community FP7-ITN Marie-Curie Program (LASSIE project, grant agreement No. 238258). We thank Gabriele Born (Astrophysikalisches Institut Jena) and Frank Steiniger (Universitaetsklinikum Jena) for their contributions in the sample preparation and FESEM diagnostics, respectively.

References

  1. Baragiola, R. A. 2005, Nucl. Instr. Meth. Phys. Res. B, 232, 98 [NASA ADS] [CrossRef] [Google Scholar]
  2. Baratta, G. A., Leto, G., Spinella, F., Strazzulla, G., & Foti, G. 1991, A&A, 252, 421 [NASA ADS] [Google Scholar]
  3. Bennett, C. J., Pirim, C., & Orlando, T. M. 2013, Chem. Rev., 113, 9086 [CrossRef] [Google Scholar]
  4. Bergin, E. A., Cleeves, L. I., Crockett, N., & Blake, G. 2014, Faraday Discussions, 168, 61 [NASA ADS] [CrossRef] [Google Scholar]
  5. Boduch, P., da Silveira, E. F., Domaracka, A., et al. 2011, Adv. Astron., 2011, 327641 [NASA ADS] [CrossRef] [Google Scholar]
  6. Carlson, R. W., Anderson, M. S., Johnson, R. E., et al. 1999, Science, 283, 2062 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  7. Chiar, J. E., Adamson, A. J., Kerr, T. H., & Whittet, D. C. B. 1994, ApJ, 426, 240 [NASA ADS] [CrossRef] [Google Scholar]
  8. Chiar, J. E., Adamson, A. J., Kerr, T. H., & Whittet, D. C. B. 1995, News Letter Astron. Soc. New York, 4, 21 [Google Scholar]
  9. Chiar, J. E., Gerakines, P. A., Whittet, D. C. B., et al. 1998, ApJ, 498, 716 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  10. Clark, R. N., Carlson, R., Grundy, W., & Noll, K. 2013, in The Science of Solar System ices, ed. M. Gudipati (Astrophysics and Space Science Library), 356, 3 [Google Scholar]
  11. de Graauw, T., Whittet, D. C. B., Gerakines, P. A., et al. 1996, A&A, 315, L345 [NASA ADS] [Google Scholar]
  12. D’Hendecourt, L. B., Allamandola, L. J., & Greenberg, J. M. 1985, A&A, 152, 130 [NASA ADS] [Google Scholar]
  13. Draine, B. T. 2003, ARA&A, 41, 241 [NASA ADS] [CrossRef] [Google Scholar]
  14. Draine, B. T. 2009, in Cosmic Dust – Near and Far, eds. T. Henning, E. Grün, & J. Steinacker, ASP Conf. Ser., 414, 453 [Google Scholar]
  15. Draine, B. T., & Lee, H. M. 1984, ApJ, 285, 89 [NASA ADS] [CrossRef] [Google Scholar]
  16. Ehrenfreund, P., Breukers, R., D’Hendecourt, L., & Greenberg, J. M. 1992, A&A, 260, 431 [NASA ADS] [Google Scholar]
  17. Ehrenfreund, P., Boogert, A. C. A., Gerakines, P. A., Tielens, A. G. G. M., & van Dishoeck, E. F. 1997, A&A, 328, 649 [NASA ADS] [Google Scholar]
  18. Ennis, C., Bennett, C. J., Jones, B. M., & Kaiser, R. I. 2011, ApJ, 733, 79 [NASA ADS] [CrossRef] [Google Scholar]
  19. Famá, M., Loeffler, M. J., Raut, U., & Baragiola, R. A. 2010, Icarus, 207, 314 [NASA ADS] [CrossRef] [Google Scholar]
  20. Fulvio, D., Sivaraman, B., Baratta, G. A., Palumbo, M. E., & Mason, N. J. 2009, Spectrochim. Acta Part A: Molecular Spectroscopy, 72, 1007 [NASA ADS] [CrossRef] [Google Scholar]
  21. Fulvio, D., Raut, U., & Baragiola, R. A. 2012, ApJ, 752, L33 [NASA ADS] [CrossRef] [Google Scholar]
  22. Gail, H.-P., Zhukovska, S. V., Hoppe, P., & Trieloff, M. 2009, ApJ, 698, 1136 [NASA ADS] [CrossRef] [Google Scholar]
  23. Gerakines, P. A., Schutte, W. A., & Ehrenfreund, P. 1996, A&A, 312, 289 [NASA ADS] [Google Scholar]
  24. Gerakines, P. A., Whittet, D. C. B., Ehrenfreund, P., et al. 1999, ApJ, 526, 1062 [NASA ADS] [CrossRef] [Google Scholar]
  25. Gerakines, P. A., Moore, M. H., & Hudson, R. L. 2000, A&A, 357, 793 [NASA ADS] [Google Scholar]
  26. Gerakines, P. A., Moore, M. H., & Hudson, R. L. 2001, J. Geophys. Res., 106, 33381 [NASA ADS] [CrossRef] [Google Scholar]
  27. Gomis, O., & Strazzulla, G. 2005, Icarus, 177, 570 [NASA ADS] [CrossRef] [Google Scholar]
  28. Gomis, O., Satorre, M. A., Strazzulla, G., & Leto, G. 2004, Planet. Space Sci., 52, 371 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
  29. Groenewegen, M. A. T., Waelkens, C., Barlow, M. J., et al. 2011, A&A, 526, A162 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  30. Grundy, W. M., Young, L. A., & Young, E. F. 2003, Icarus, 162, 222 [NASA ADS] [CrossRef] [Google Scholar]
  31. Guertler, J., Henning, T., Koempe, C., et al. 1996, A&A, 315, L189 [NASA ADS] [Google Scholar]
  32. Hendrix, A. R., Barth, C. A., & Hord, C. W. 1999, J. Geophys. Res., 104, 14169 [NASA ADS] [CrossRef] [Google Scholar]
  33. Henning, T., Michel, B., & Stognienko, R. 1995, Planet. Space Sci., 43, 1333 [NASA ADS] [CrossRef] [Google Scholar]
  34. Henning, T., Jäger, C., & Mutschke, H. 2004, in Astrophysics of Dust, eds. A. N. Witt, G. C. Clayton, & B. T. Draine, ASP Conf. Ser., 309, 603 [Google Scholar]
  35. Herbst, E. 2005, in ESA SP 577, ed. A. Wilson, 205 [Google Scholar]
  36. Hibbitts, C. A., Klemaszewski, J. E., McCord, T. B., Hansen, G. B., & Greeley, R. 2002, J. Geophys. Res. (Planets), 107, 5084 [NASA ADS] [CrossRef] [Google Scholar]
  37. Hibbitts, C. A., Pappalardo, R. T., Hansen, G. B., & McCord, T. B. 2003, J. Geophys. Res. (Planets), 108, 5036 [NASA ADS] [CrossRef] [Google Scholar]
  38. Hincelin, U., Wakelam, V., Hersant, F., et al. 2011, A&A, 530, A61 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  39. Hudgins, D. M., Sandford, S. A., Allamandola, L. J., & Tielens, A. G. G. M. 1993, ApJS, 86, 713 [NASA ADS] [CrossRef] [Google Scholar]
  40. Ioppolo, S., Palumbo, M. E., Baratta, G. A., & Mennella, V. 2009, A&A, 493, 1017 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  41. Ioppolo, S., van Boheemen, Y., Cuppen, H. M., van Dishoeck, E. F., & Linnartz, H. 2011, MNRAS, 413, 2281 [NASA ADS] [CrossRef] [Google Scholar]
  42. Ioppolo, S., Sangiorgio, I., Baratta, G. A., & Palumbo, M. E. 2013, A&A, 554, A34 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  43. Jäger, C., Mutschke, H., & Henning, T. 1998, A&A, 332, 291 [NASA ADS] [Google Scholar]
  44. Jäger, C., Mutschke, H., Henning, T., & Huisken, F. 2008, ApJ, 689, 249 [NASA ADS] [CrossRef] [Google Scholar]
  45. Jenkins, E. B. 2009, ApJ, 700, 1299 [NASA ADS] [CrossRef] [Google Scholar]
  46. Jiang, G. J., Person, W. B., & Brown, K. G. 1975, J. Chem. Phys., 62, 1201 [NASA ADS] [CrossRef] [Google Scholar]
  47. Johnson, R. E., Famá, M., Liu, M., et al. 2008, Planet. Space Sci., 56, 1238 [NASA ADS] [CrossRef] [Google Scholar]
  48. Jones, B. M., Bennett, C. J., & Kaiser, R. I. 2011, ApJ, 734, 78 [NASA ADS] [CrossRef] [Google Scholar]
  49. Jones, B. M., Gusmeroli, A., Arp, C. D., et al. 2013, International Journal of Remote Sensing, 34, 8267 [NASA ADS] [CrossRef] [Google Scholar]
  50. Jones, B. M., Kaiser, R. I., & Strazzulla, G. 2014, ApJ, 781, 85 [NASA ADS] [CrossRef] [Google Scholar]
  51. Kerr, T. H., & Adamson, A. J. 1993, in Astronomical Infrared Spectroscopy: Future Observational Directions, ed. S. Kwok, ASP Conf. Ser., 41, 219 [Google Scholar]
  52. Lamberts, T., Cuppen, H. M., Fedoseev, G., et al. 2014, A&A, 570, A57 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  53. Lee, J.-E., Bergin, E. A., & Nomura, H. 2010, ApJ, 710, L21 [NASA ADS] [CrossRef] [Google Scholar]
  54. Leto, G., & Baratta, G. A. 2003, A&A, 397, 7 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  55. Li, A., & Greenberg, J. M. 1997, A&A, 323, 566 [NASA ADS] [Google Scholar]
  56. Loeffler, M. J., Baratta, G. A., Palumbo, M. E., Strazzulla, G., & Baragiola, R. A. 2005, A&A, 435, 587 [NASA ADS] [CrossRef] [EDP Sciences] [MathSciNet] [Google Scholar]
  57. Loeffler, M. J., Raut, U., Vidal, R. A., Baragiola, R. A., & Carlson, R. W. 2006, Icarus, 180, 265 [NASA ADS] [CrossRef] [Google Scholar]
  58. Madey, T. E., Johnson, R. E., & Orlando, T. M. 2002, Surface Science, 500, 838 [NASA ADS] [CrossRef] [Google Scholar]
  59. McCord, T. B., Carlson, R., Smythe, W., et al. 1997, Science, 278, 271 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  60. McCord, T. B., Hansen, G. B., Clark, R. N., et al. 1998, J. Geophys. Res., 103, 8603 [NASA ADS] [CrossRef] [Google Scholar]
  61. Mennella, V., Colangeli, L., Palumbo, P., et al. 1996, in The Role of Dust in the Formation of Stars, eds. H. U. Käufl, & R. Siebenmorgen, 317 [Google Scholar]
  62. Mennella, V., Palumbo, M. E., & Baratta, G. A. 2004, ApJ, 615, 1073 [NASA ADS] [CrossRef] [Google Scholar]
  63. Mennella, V., Baratta, G. A., Palumbo, M. E., & Bergin, E. A. 2006, ApJ, 643, 923 [NASA ADS] [CrossRef] [Google Scholar]
  64. Moore, M. H., & Hudson, R. L. 1992, BAAS, 24, 1042 [NASA ADS] [Google Scholar]
  65. Moore, M. H., & Hudson, R. L. 2000, Icarus, 145, 282 [NASA ADS] [CrossRef] [Google Scholar]
  66. Moore, M. H., Khanna, R., & Donn, B. 1991, J. Geophys. Res., 96, 17541 [NASA ADS] [CrossRef] [Google Scholar]
  67. Moore, M. H., Ferrante, R. F., & Nuth, III, J. A. 1996, Planet. Space Sci., 44, 927 [NASA ADS] [CrossRef] [Google Scholar]
  68. Moore, M. H., Hudson, R. L., & Gerakines, P. A. 2001, Spectrochim. Acta, 57, 843 [NASA ADS] [CrossRef] [Google Scholar]
  69. Noble, J. A., Dulieu, F., Congiu, E., & Fraser, H. J. 2011, ApJ, 735, 121 [NASA ADS] [CrossRef] [Google Scholar]
  70. Palumbo, M. E., & Baratta, G. A. 2000, A&A, 361, 298 [NASA ADS] [Google Scholar]
  71. Palumbo, M. E., & Strazzulla, G. 1993, A&A, 269, 568 [NASA ADS] [Google Scholar]
  72. Palumbo, M. E., Baratta, G. A., Brucato, J. R., et al. 1998, A&A, 334, 247 [NASA ADS] [Google Scholar]
  73. Peeters, Z., Hudson, R. L., Moore, M. H., & Lewis, A. 2010, Icarus, 210, 480 [NASA ADS] [CrossRef] [Google Scholar]
  74. Pilling, S., Seperuelo Duarte, E., Domaracka, A., et al. 2010, A&A, 523, A77 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  75. Pontoppidan, K. M., Boogert, A. C. A., Fraser, H. J., et al. 2008, ApJ, 678, 1005 [NASA ADS] [CrossRef] [Google Scholar]
  76. Porter, S. B., Desch, S. J., & Cook, J. C. 2010, Icarus, 208, 492 [NASA ADS] [CrossRef] [Google Scholar]
  77. Raut, U., & Baragiola, R. A. 2011, ApJ, 737, L14 [NASA ADS] [CrossRef] [Google Scholar]
  78. Raut, U., Loeffler, M. J., Famá, M., & Baragiola, R. A. 2011, J. Chem. Phys., 134, 194501 [NASA ADS] [CrossRef] [Google Scholar]
  79. Raut, U., Fulvio, D., Loeffler, M. J., & Baragiola, R. A. 2012, ApJ, 752, 159 [NASA ADS] [CrossRef] [Google Scholar]
  80. Sabri, T., Gavilan, L., Jäger, C., et al. 2014, ApJ, 780, 180 [NASA ADS] [CrossRef] [Google Scholar]
  81. Sandford, S. A., & Allamandola, L. J. 1990, Icarus, 87, 188 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  82. Sandford, S. A., Allamandola, L. J., Tielens, A. G. G. M., & Valero, G. J. 1988, ApJ, 329, 498 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  83. Satorre, M. A., Palumbo, M. E., & Strazzulla, G. 2000, Ap&SS, 274, 643 [NASA ADS] [CrossRef] [Google Scholar]
  84. Smith, M. A. H., Rinsland, C. P., Fridovich, B., & Rao, K. N. 1985, in Molecular Spectroscopy: Modern Research, ed. K.N. Rao, Vol. 3 (New York: Academic Press), 112 [Google Scholar]
  85. Stognienko, R., Henning, T., & Ossenkopf, V. 1995, A&A, 296, 797 [NASA ADS] [Google Scholar]
  86. Strazzulla, G. 2011, Nucl. Instr. Meth. Phys. Res. B, 269, 842 [NASA ADS] [CrossRef] [Google Scholar]
  87. Strazzulla, G., Leto, G., & Palumbo, M. E. 1993, Adv. Space Res., 13, 189 [NASA ADS] [CrossRef] [Google Scholar]
  88. Strazzulla, G., Brucato, J. R., Palumbo, M. E., & Satorre, M. A. 1997, A&A, 321, 618 [NASA ADS] [Google Scholar]
  89. Strazzulla, G., Baratta, G. A., & Palumbo, M. E. 2001, Spectrochim. Acta, 57, 825 [NASA ADS] [CrossRef] [Google Scholar]
  90. Teixeira, T. C., Emerson, J. P., & Palumbo, M. E. 1998, A&A, 330, 711 [NASA ADS] [Google Scholar]
  91. Teolis, B. D., & Waite, J. H. 2012, AGU Fall Meeting Abstracts, A2 [Google Scholar]
  92. Teolis, B. D., Jones, G. H., Miles, P. F., et al. 2010, Science, 330, 1813 [NASA ADS] [CrossRef] [Google Scholar]
  93. Tielens, A. G. G. M., Tokunaga, A. T., Geballe, T. R., & Baas, F. 1991, ApJ, 381, 181 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
  94. Vandenbussche, B., Ehrenfreund, P., Boogert, A. C. A., et al. 1999, A&A, 346, L57 [NASA ADS] [Google Scholar]
  95. Watanabe, N., & Kouchi, A. 2002, ApJ, 567, 651 [NASA ADS] [CrossRef] [Google Scholar]
  96. Whittet, D. C. B. 1993, in Observations of Molecular Ices, eds. T. J. Millar, & D. A. Williams, 9 [Google Scholar]
  97. Whittet, D. C. B. 2010, ApJ, 710, 1009 [NASA ADS] [CrossRef] [Google Scholar]
  98. Whittet, D. C. B., & Walker, H. J. 1991, MNRAS, 252, 63 [NASA ADS] [CrossRef] [Google Scholar]
  99. Whittet, D. C. B., Gerakines, P. A., Tielens, A. G. G. M., et al. 1998, ApJ, 498, L159 [NASA ADS] [CrossRef] [Google Scholar]
  100. Whittet, D., Bergin, E., Chiar, J., et al. 2007, Spitzer Proposal, 40432 [Google Scholar]
  101. Yamada, H., & Person, W. B. 1964, J. Chem. Phys., 41, 2478 [NASA ADS] [CrossRef] [Google Scholar]
  102. Zheng, W., & Kaiser, R. I. 2007, Chem. Phys. Lett., 450, 55 [NASA ADS] [CrossRef] [Google Scholar]
  103. Zheng, W., Jewitt, D., & Kaiser, R. I. 2006, ApJ, 648, 753 [NASA ADS] [CrossRef] [Google Scholar]
  104. Zhukovska, S., & Gail, H.-P. 2007, in Why Galaxies Care About AGB Stars: Their Importance as Actors and Probes, eds. F. Kerschbaum, C. Charbonnel, & R. F. Wing, ASP Conf. Ser., 378, 499 [Google Scholar]
  105. Zhukovska, S., & Henning, T. 2013, A&A, 555, A99 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
  106. Ziegler, J. F., Ziegler, M. D., & Biersack, J. P. 2010, Nucl. Instr. Meth. Phys. Res. B, 268, 1818 [NASA ADS] [CrossRef] [Google Scholar]

All Tables

Table 1

Ion bombardment experiments with 200 keV H+ ions performed at INAF, Catania.

In the text
Table 2

List of molecules observed after irradiation with 200 keV H+ ions in different ices together with their band positions and strengths used to evaluate their column densities.

In the text

All Figures

thumbnail Fig. 1

Scheme of the laser ablation setup used for the condensation of graphite.
Open with DEXTER
In the text
thumbnail Fig. 2

Schematic top view of the vacuum chamber used for the ion irradiation of the 13C grain/ice layer with 200 keV H+ at the INAF-Osservatorio Astrofisico di Catania.
Open with DEXTER
In the text
thumbnail Fig. 3

IR spectra of amorphous 13C (solid line), amorphous 13C after H2O ice deposit (dotted line) and after O2 ice deposit (gray solid line) along with irradiation of 200 keV H+ (experiment No. 3 in Table 1).
Open with DEXTER
In the text
thumbnail Fig. 4

Column densities of 13CO (lower graph) and 13CO2 (upper graph) versus the fluence. The formation rates of both molecules were derived from the fit of the experimental data with a standard deviation of δR = ± 0.38 (molecules/ion).
Open with DEXTER
In the text
thumbnail Fig. 5

Topographic view produced from a FESEM micrograph showing the erosion of the carbon layer after ion bombardment with 6.76 × 1016 protons/cm2. The left part is the bombarded area whereas the right and bright surface represents the nonirradiated part of the sample. The scale on the right side corresponds to the layer thickness.
Open with DEXTER
In the text
thumbnail Fig. 6

HRTEM image of fullerene-like carbon grains before ion bombardment. The inset demonstrates the cross-linking between the bent graphene layers. The arrows mark individual fullerenes between the grains.
Open with DEXTER
In the text
thumbnail Fig. 7

HRTEM images of the carbon structures after ice deposition and irradiation-induced processing (sample 3e in Table 1). The upper image shows a strongly processed area of carbon material representing graphitic structures. The lower image displays material that is less processed compared to the top layer. It still shows a similarity to the original fullerene-like material but with longer graphene layers.
Open with DEXTER
In the text
thumbnail Fig. 8

FESEM image of carbon grains before (lower image) and after 200 keV proton bombardment with 6.76 × 1016 ions/cm2 (top image).
Open with DEXTER
In the text
thumbnail Fig. 9

Series of images presenting material with different levels of proton-induced processing. The three types of carbon structures were observed underneath the graphitic layer after complete bombardment of sample 3 with the total fluence of 6.76 × 1016 ions/cm2. The particles are still visible, but they contain longer graphene layers compared to those observed in the original grains. In addition, one can see the formation of more closed buckyonions and fullerenes. The right micrograph finally shows grains, which are still similar to the unprocessed fullerene-like grains.
Open with DEXTER
In the text
thumbnail Fig. 10

Graphitic structures observed after bombardment of bare carbonaceous grains with 200 keV protons at total fluence of 6.76 × 1016 ions/cm2 (left). Fullerenes and bucky onions (middle), detected beneath the graphite layer, demonstrate the conversion of curved fullerene fragments into more closed structures (right).
Open with DEXTER
In the text

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