Report

Importance of Surface Morphology in Interstellar H2 Formation

See allHide authors and affiliations

Science  12 Dec 2003:
Vol. 302, Issue 5652, pp. 1943-1946
DOI: 10.1126/science.1090820

Abstract

Detailed laboratory experiments on the formation of HD from atom recombination on amorphous solid water films show that this process is extremely efficient in a temperature range of 8 to 20 kelvin, temperatures relevant for H2 formation on dust grain surfaces in the interstellar medium (ISM). The fate of the 4.5 electron volt recombination energy is highly dependent on film morphology. These results suggest that grain morphology, rather than the detailed chemical nature of the grain surface, is most important in determining the energy content of the H2 as it is released from the grain into the ISM.

The formation of molecular hydrogen in interstellar molecular clouds is the key first step in both the formation of stars and in the evolution of molecular complexity in the interstellar medium (ISM). It is widely accepted that (i) there is no efficient gas phase route for H2 formation from H atoms at the low temperatures and densities of the ISM and (ii) H2 is formed by H atom recombination on dust grains that are integrally associated with the interstellar molecular clouds (1). To account for the astronomically observed H2 formation rate in clouds (2, 3), the surface recombination of H atoms on grains to produce H2 must be a very efficient process at T ∼ 10 K (1). However, previous laboratory experiments on H2 formation on surfaces of astrophysical relevance were interpreted as implying that the recombination is thermally activated (4), requiring T ≥ 20 K (5) for surfaces thought to be important in dark interstellar clouds. The formation of each H2 molecule also releases 4.5 eV of energy. How this energy is partitioned amongst the various degrees of freedom is crucial in understanding the temporal and chemical evolution of molecular clouds (6). For example, partitioning of the reaction energy into H2 kinetic energy heats the cloud, while vibrational excitation of the H2 or excitation of the grain surface are rapidly (on astronomical time scales) dissipated via radiation that escapes the cloud. Thus, the time scale for collapse of a cloud to yield cores of high density where stars ultimately form depends critically on the energy disposal in H2 formation (6). In addition, if a large fraction of the 4.5 eV goes into local heating of the grain, this can thermally catalyze other chemical reactions on the grain and/or desorb other atoms or molecules adsorbed in close vicinity on the grains (7). Unfortunately, at present no definitive aspects of this energy partitioning can be directly inferred from observational astronomy.

The chemical nature of the dust grains is not well characterized, but astronomical data and studies of meteorites show that they are principally composed of silicate and carbonaceous material. In diffuse (low density) clouds, the dust grains are bare, but in dark (dense) clouds, the grains are covered with “ice” mantles, principally amorphous solid water with added CO, CO2, methanol, and other molecules (8, 9). Though the size distribution of the interstellar grains is accepted to follow a power law, their morphology is not well determined. Hence, it is unknown whether the typical ∼0.1 μm diameter particles thought to be important in the formation of H2 in the ISM are solid compact particles, porous structures, open fractal-like structures, or other possible modifications.

Here, we present laboratory experiments on H+D recombination that simulate the formation of H2 in the ISM. On amorphous solid water (ASW) films, which are believed to be good analogs for ice mantles on interstellar grains in dark clouds (9), we find a very efficient recombination mechanism that occurs at surface temperatures as low as 8 K and that implies fast mobility of  H and D atoms at this temperature. In porous ASW films, the major fraction of HD produced is subsequently retained as a physisorbed molecule in the pores and is not released into the gas phase until the film is externally heated above the HD molecular desorption temperature. In this case, most of the 4.5 eV recombination energy is lost to the ASW film. On nonporous ASW films, however, the experimental results show minimal retention of the HD formed by atom recombination on the surface of the ASW film. This result implies prompt ejection of the HD formed into the gas phase with its nascent energy distribution. Theory indicates that the nascent reaction energy is principally partitioned into HD internal and translational excitation (10). Thus, the overall mechanism for formation of gas phase HD and its energy distribution depends critically on film morphology. We argue that this same dependence on morphology should exist for H2 formation on ice-covered grains in dense interstellar clouds. In addition, we suggest that the dependence of the H2 energy distribution on grain morphology should also apply for H2 formation on bare grains in diffuse clouds, so that the dominant effect controlling the energy of  H2 formed throughout the ISM may not be the detailed chemical nature of the grain surfaces but rather their morphology.

In our experiments, ASW films are grown on a Cu substrate attached to a flowing liquid He cryostat by depositing H20 onto the substrate from a capillary array “doser” (11). Under our H2O deposition conditions and a surface temperature Ts ≤ 10 K, modestly porous ASW films are grown [ξpor ≅ 0.05, where ξpor is defined as the percentage increase in internal surface area per monolayer (ML) of ASW relative to the external surface area of the film] (12). With H2O deposition at Ts = 120 K, nonporous ASW films are grown (12). HD formation is induced by exposing the films to separate H and D atomic beams (13) that spatially overlap at the center of the ASW surface in an ultra–high vacuum chamber (≤10–10 torr). After dosing with H+D beams, we perform both temperature programmed desorption (TPD) measurements and laser induced thermal desorption (LITD) measurements (14).

The TPD spectrum of HD resulting from H+D recombination on porous ASW exhibits a large signal peaking at a temperature of 28 K (Fig. 1A). Turning off either or both discharges producing H and D atoms causes the large HD TPD peak to disappear; therefore, the signal arises from recombination of H and D atoms on the external or internal (pore) surfaces of the ASW film. The dashed line (Fig. 1) shows the TPD spectra for D2 after only molecular D2 dosing. HD molecules formed by atom recombination on the ASW films are desorbed at the same temperature as D2 molecules that are adsorbed molecularly. In equivalent experiments for dosing on a nonporous ASW film (Fig. 1B), the intensity of the HD TPD signal is extremely weak.

Fig. 1.

(A) HD QMS signal during TPD after a 10 min dose of H+D (solid line), after a 10 min dose of H2 + D2 (dotted line), and D2 QMS signal after a 10 min dose of D2 (dashed line) onto a ∼2000 monolayer (ML) porous ASW film. The D2 QMS signal has been offset for clarity. (B) HD QMS signal during TPD after a 5 min dose of H+D (solid line) and D2 QMS signal after a 5 min dose of D2 (dashed line) onto a ∼300 ML nonporous ASW film. The D2 QMS signal has been offset for clarity.

We show elsewhere (15) that in the low D2 coverage limit, there is a substantial increase in the TPD peak temperature with increasing thickness of porous ASW films and a strong sensitivity of the TPD spectra to thermal annealing, which reduces porosity. The origin of this phenomenon is attributed to fast diffusion of the D2 molecules producing a uniform distribution of adsorbed molecules on the total surface of the ASW film (both pore walls and external surface). During the TPD ramp, molecules adsorbed on the pore walls undergo a random walk of desorption-readsorption cycles until they reach the outer surface and desorb into the gas phase. This cycling causes the TPD peak for D2 to appear at substantially higher temperatures for the porous ASW relative to the nonporous ASW film (16). The dependence of the TPD spectra on both porous ASW film thickness and thermal annealing for HD formed by H+D recombination is identical to that for D2 from molecular dosing.

The observation that the HD formed by atom recombination always desorbs at the same temperature as D2 molecularly dosed onto the surface irrespective of the film thickness or thermal history suggests that H and D atoms are mobile on the film surface at temperatures below the molecular desorption temperature and undergo a Langmuir-Hinshelwood or hot atom (17) recombination to form HD, which is then retained in the pores until the temperature is externally ramped to a high enough temperature to cause molecular desorption. This retention of the formed molecules was seen to be efficient for an ASW film thickness as low as 30 monolayers. To determine the temperature at which the atoms become mobile and recombine, sequential dosing of D and H atoms was compared to simultaneous H+D dosing for porous ASW (Fig. 2). Even at 8 K, sequential dosing leads to a large decrease of HD intensity in the TPD relative to that for simultaneous dosing. Simultaneous dosing, followed by extended waiting periods (30 min), showed no decreases in HD intensity, implying that the decrease was not due to desorption of atoms or HD during the waiting period. The results imply fast recombination either via the Langmuir-Hinshelwood or hot atom mechanism, i.e., that the isotope dosed initially recombines forming D2 or H2 molecules and that this process leaves no free atoms to react when the second isotope is dosed later (18). Thus, these results show that even at 8 K the atoms are mobile enough to recombine. Because of the small intensity of the HD desorption peak on nonporous ASW, it was not possible to do similar experiments on this surface. However, there is no reason to suspect that surface atom mobility is less on the nonporous surface than on the porous ASW. We believe that these experiments rule out an interpretation that the major route to HD formation on ASW requires thermally activated H atom diffusion to induce a Langmuir-Hinshelwood recombination at temperatures above 20 K, as has been suggested previously (5).

Fig. 2.

Integrated HD TPD (QMS) signal after H+D dosing on a ∼ 2000 ML porous ASW film versus surface temperature during the atom deposition for the following dose conditions: (◼) 5 min simultaneous dose of H+D; (⚫) 5 min dose of D atoms followed by a 2 min wait period and then a 5 min H atom dose; and (▲) 5 min dose of H atoms followed by a 2 min wait period and then a 5 min D atom dose.

The overall efficiency of the molecular HD formation process on a surface is expressed as Sη, where S is the sticking probability of the H or D atom on the surface (assuming they are equal), and η is the probability of an adsorbed atom recombining with another adsorbed atom on the surface. Because we measure the HD in TPD, we only measure the fraction of HD formed by recombination that is retained in the porous structure by adsorption on the internal pore surfaces of the film and is then subsequently desorbed thermally during the TPD. Denoting this fraction as μ implies that the integrated HD TPD intensity is proportional to μSη. We determine absolute values of μSη using a single D atom beam for relative measurements combined with a single D2 sticking measurement for absolute scaling. By comparing the integrated D2 TPD intensity obtained when dosing with discharge on (D atoms + residual D2 beam) to that obtained when dosing with discharge off (D2 only) and knowing the extent of dissociation in the beam, we obtain μSDη/SD2, where SD is the sticking probability for D atoms and SD2 is the sticking probability for D2 molecules. Measurement of SD2 (19) gives the absolute measurements for μSDη shown in Fig. 3. μSDη is large (∼0.35) on porous ASW and decreases slightly at Ts ≥ 17 K, but it is nearly zero (within experimental error) on nonporous ASW. The same results were obtained qualitatively by measuring the HD intensity in TPD with simultaneous dosing of H and D atoms; i.e., the retained fraction of HD for nonporous ASW is minimal relative to that for porous ASW (Fig. 1), and the HD production drops off gradually at Ts ≥ 17 K for porous ASW. The decrease in μSDη with Ts is ascribed to thermal desorption of atoms competing with their recombination, i.e., to a decrease in η with Ts. For pure physisorption systems (such as D and D2 interacting with ASW), we anticipate that SDSD2 because of the increased elastic scattering of the D atom relative to D2 (20) such that μη ≥ 0.6 for porous ASW (19) and μη ∼ 0 for nonporous ASW. Because there is no reason to suspect that η ≤ 1 at low Ts for either film, we interpret these results as implying that μ ≥ 0.6 for porous ASW and μ ∼ 0 for nonporous ASW. Thus, prompt desorption dominates for nonporous ASW films, whereas retention in the films dominates for the porous ASW.

Fig. 3.

Recombination efficiency, μSD η, into retained D2 on a ∼2000 ML porous ASW film (⚫) and (▲) on a ∼2000 ML nonporous ASW film.

A direct measurement of the kinetic energy of the desorbing HD molecules formed by H+D recombination on the porous ASW surface (Fig. 4A) and of molecularly adsorbed D2 (Fig. 4B) was obtained from LITD and time of flight (TOF) data. A peak temperature of 45 ± 10 K is estimated for the laser-induced temperature jump (21). The smooth curves on the figure give the LITD signal anticipated for thermal desorption from a surface at this temperature. Similar kinetic energy distributions are obtained both for HD formation by H+D and in molecular D2 adsorption, and both are nearly equivalent to that anticipated from thermal desorption at the peak temperature of the laser-induced temperature jump. Therefore, we infer that all of the nascent kinetic energy from H+D formation is lost to the porous ASW before desorption into the gas phase.

Fig. 4.

TOF spectra from a ∼200 ML porous ASW film after (A) 10 min H+D dose and (B) 10 min D2 dose. The smooth curves are simulated TOF spectra expected for molecules coming off a 45 K surface with a thermal Maxwell-Boltzman velocity distribution.

On the basis of the observations presented above, the following picture of HD formation on ASW emerges: H and D atoms are mobile and efficiently recombine even at temperatures as low as 8 K. For porous ASW, the dominant fraction of the recombination occurs within the pores at the surface of pore walls. Once formed, the HD is retained in the porous structure until molecular desorption thermally occurs. This is induced to occur on a reasonable laboratory time scale by raising the temperature by an external temperature ramp. Upon initial HD formation, 4.5 eV energy is released into both internal and translational energy of the HD, as well as some small amount into the lattice. The fraction partitioned into kinetic energy is dissipated in collisions with the pore walls as the HD molecularly adsorbs. Similarly, because nonradiative vibrational and rotational relaxation times for molecules physisorbed on surfaces are less than milliseconds (22, 23), especially on H2O surfaces, any vibrational or rotational excitation produced in HD formation will also be fully relaxed before molecular desorption. Thus, the HD formed in the recombination desorbs in thermal equilibrium with the surface, having lost essentially all of the 4.5 eV recombination energy to the ASW film before desorption. The possible minor fraction of molecules that is not retained in the pores due to recombination on or near the external surface (1 – μ < 0.4) will presumably desorb with only a partially thermalized energy distribution whose details will depend on details of the path of the HD after formation to the external surface. For the nonporous ASW, we observe that μ ∼ 0, so the dominant fraction of formed HD desorbs with its nascent energy distribution, i.e., according to present theory with high internal and translational excitation of the HD (10). Thus, energy partitioning of the 4.5 eV exoergicity between HD excitation and the ASW depends critically on the morphology of the ASW film.

Because grains in dark clouds are believed to have ice mantles with a major component comprised of ASW, the conclusions from the laboratory experiments reported here should be directly relevant to the mechanism and energy partitioning in H2 formation in dark clouds. Thus, if the ASW film on the grain is porous, either because the underlying bare grain is highly porous or the ASW film grown on a compact grain is porous, then most (fraction μ) of the H2 formed will be retained in pores of the grain until it is desorbed thermally at a rate of approximately 10–7 s–1 at 10 K. Although this rate is slow by laboratory standards (and thus we only observe thermal desorption at higher temperatures in the experiments), this still implies thermal desorption in an astronomically short time (i.e., less than a year). Thus, most of the recombination energy will be deposited into the grain without much excitation of H2 in the gas phase being produced. Alternatively, for H2 formation on compact grain mantles, μ ∼ 0 and theory then predicts that most of the gas phase H2 is produced with nearly the full recombination energy partitioned into H2 excitation (10). In diffuse clouds H2 formation is thought to occur on the surface of bare carbonaceous and silicate grains. Recent experiments on the formation of interstellar carbon dust grain analogs suggest that these could very well be microporous structures showing nanometer-scale porosity (24). Because H and H2 are physisorbed on these surfaces (and internal pore surfaces) with similar binding energies to that of ASW, and energy transfer mechanisms between H2 and the pore surfaces are likely similar (16), we suggest that H2 retention in pores will be similar on the bare grains to that for ASW. Hence, the energy distribution in H2 formation could show a similar dependence on dust grain morphology for bare carbonaceous grains as seen here for ASW films. All that is required is that the morphology (pore structure) induces a life-time on the grain that is long compared with the overall energy relaxation time for the nascent H2 exoergicity. For silicates, both compact and fluffy grain particles have been found in meteorites and have been grown under laboratory conditions relevant to the ISM. However, the details of the morphology of these grains is unknown, so we can only speculate that the energy budget of H2 produced on these grains should depend in a similar way to internal morphology as for the ASW films. Therefore, we propose that the dominant effect controlling the initial energy distributions of gas phase H2 formed in the ISM may not be the detailed chemical nature of the grain surfaces but rather their morphology.

References and Notes

View Abstract

Stay Connected to Science

Navigate This Article