Polycyclic aromatic hydrocarbon processing in a hot gas
E. R. Micelotta^{1,2}  A. P. Jones^{2}  A. G. G. M. Tielens^{1,3}
1  Sterrewacht Leiden, Leiden University, PO Box 9513, 2300 RA Leiden,
The Netherlands
2  Institut d'Astrophysique Spatiale, Université Paris Sud and CNRS
(UMR 8617), 91405 Orsay, France
3  NASA Ames Research Center, MS 2453, Moffett Field, CA 94035, USA
Received 20 January 2009 / Accepted 16 October 2009
Abstract
Context. PAHs are thought to be a ubiquitous and
important dust component of the interstellar medium. However, the
effects of their immersion in a hot (postshock) gas have never before
been fully investigated.
Aims. We study the effects of energetic ion and
electron collisions on PAHs in the hot postshock gas behind
interstellar shock waves.
Methods. We calculate the ionPAH and electronPAH
nuclear and electronic interactions, above the carbon atom loss
threshold, in H II regions and in
the hot postshock gas for temperatures ranging from 10^{3}10^{8} K.
Results. PAH destruction is dominated by He
collisions at low temperatures (
K), and by electron
collisions at higher temperatures. Smaller PAHs are destroyed faster
for T < 10^{6} K,
but the destruction rates are roughly the same for all PAHs at higher
temperatures. The PAH lifetime in a tenuous hot gas (
cm^{3},
K), typical of the
coronal gas in galactic outflows, is found to be about thousand years,
orders of magnitude shorter than the typical lifetime of such objects.
Conclusions. In a hot gas, PAHs are principally
destroyed by electron collisions and not by the absorption of Xray
photons from the hot gas. The resulting erosion of PAHs occurs via C_{2}
loss from the periphery of the molecule, thus preserving the aromatic
structure. The observation of PAH emission from a million degree, or
more, gas is only possible if the emitting PAHs are ablated from dense,
entrained clumps that have not yet been exposed to the full effect of
the hot gas.
Key words: shock waves  dust, extinction  ISM: jets and outflows
1 Introduction
The midinfrared spectral energy distribution of the general interstellar medium of galaxies is dominated by strong and broad emission features at 3.3, 6.2, 7.7 and 11.3 m. These features are now univocally attributed to vibrational fluorescence of UV pumped, large (50 Catoms) polycyclic aromatic hydrocarbon (PAHs) molecules. These large molecules are very abundant ( by number relative to Hnuclei) and ubiquitous in the ISM (for a recent review see Tielens 2008). Besides large PAH molecules, the spectra also reveal evidence for clusters of PAHs  containing some hundreds of carbon atoms  and very small grains (30 Å). Indeed, PAHs seem to represent the extension of the interstellar dust size distribution into the molecular domain (e.g. Draine & Li 2001; Désert et al. 1990).
PAH molecules are an important component of the ISM, for example, dominating the photoelectric heating of neutral atomic gas and the ionization balance of molecular clouds. Small dust grains and PAHs can also be important agents in cooling a hot gas, at temperatures above K (e.g. Dwek 1987), through their interactions with thermal electrons and ions. The energy transferred in electron and ion collisions with the dust is radiated as infrared photons. The evolution of dust in such hot gas ( K), e.g., within supernova remnants and galactic outflows, is critical in determining the dust emission from these regions and therefore the cooling of the hot gas. The destruction of PAHs and small dust grains in a hot gas may also be an important process in the lifecycle of such species (Jones et al. 1996; Dwek et al. 1996).
Observationally, there is little direct evidence for PAH emission unequivocally connected to the hot gas in supernova remnants. Reach et al. (2006) have identified four supernova remnants with IR colors that may indicate PAH emission. Tappe et al. (2006) have detected spectral structure in the emission characteristics of the supernova remnant N132D in the Large Magellanic Cloud that they attribute to spectral features of PAHs with sizes of 4000 Catoms. Bright 8 m emission has been observed by IRAC/Spitzer associated with the Xray emission from the stellar winds of the ionizing stars in the M 17 H II region (Povich et al. 2007). Likely, this emission is due to PAHs  probably, in entrained gas ablated from the molecular clouds to the north and west of the stellar cluster. Finally, bright PAH emission has been detected associated with the hot gas of the galactic wind driven by the starburst in the nucleus of the nearby irregular galaxy, M 82 (Beirão et al. 2008; Galliano et al. 2008; Engelbracht et al. 2006).
Electron and ion interactions with dust and the implications of those interactions for the dust evolution and emission have already been discussed in the literature (e.g. Draine & Salpeter 1979; Dwek 1987; Jones et al. 1994,1996; Dwek et al. 1996). In this work we extend this earlier work to the case for PAHs, using our study of PAH evolution due to ion and electron interactions in shock waves in the ISM (Micelotta et al. 2010, hereafter MJT). Here we consider the fate of PAHs in the hot gas behind fast nonradiative shocks and in a hot gas in general.
The aim of this paper is to study the PAH stability against electron and ion collisions (H, He and C) in a thermal gas with temperature T in the range 10^{3}10^{8} K.
The paper is organized as follows: Sects. 2 and 3 describe the treatment of ion and electron interactions with PAHs, Sect. 4 illustrates the application to PAH processing in a hot gas and Sect. 5 presents our results on PAH destruction and lifetime. The astrophysical implications are discussed in Sect. 6 and our conclusions summarized in Sect. 7.
2 Ion interaction with PAHs
2.1 Electronic interaction
The ion  PAH collision can be described in terms of two simultaneous processes which can be treated separately (Lindhard et al. 1963): nuclear stopping or elastic energy loss and electronic stopping or inelastic energy loss.
The nuclear stopping consists of a binary collision between the incoming ion (projectile) and a single atom in the target material. A certain amount of energy will be transferred directly to the target atom, which will be ejected if the energy transferred is sufficient to overcome the threshold for atom removal. The physics of the nuclear interaction for a PAH target was presented in the companion paper (MJT). A summary of the theory is provided in Sect. 2.2 and we here present the results of our calculation.
In this paper we focuse on the electronic stopping, which consists of the interaction between the projectile and the electrons of the target PAH, with a subsequent energy transfer to the whole molecule. The resulting electronic excitation energy will be transferred to the molecular vibrations of the PAH through radiationless processes (e.g., interconversion & intramolecular vibrational redistribution). The vibrationally excited molecule will decay through either (IR) photon emission or through fragmentation (i.e., Hatom or C_{2}H_{n} loss, where n = 0, 1, 2).
No specific theory describes the energy transfer to a PAH via electronic excitation, so we adopt the same approach developed by e.g. Schlathölter et al. (1999) and Hadjar et al. (2001) who modelled electronic interactions in fullerene, C_{60}. To calculate the energy transferred to a PAH, we treat the large number of delocalized valence electrons in the molecule as an electron gas, where the inelastic energy loss of traveling ions is due to long range coupling to electronhole pairs (Ferrell 1979).
In the energy range we consider for this study, the energy
transferred scales linearly with the velocity v of
the incident ion and can be described in term of the stopping power S,
which is widely used in the treatment of ionsolid collisions. The
stopping power represents the energy loss per unit length and is
defined as
where dT is the energy loss over the pathlength ds (Sigmund 1981). The total energy loss can then be obtained integrating Eq. (1)
The friction coefficient (Puska & Nieminen 1983) depends on the density parameter which is a function of the valence electron density n_{0}. The choice of the valence electron density is a delicate issue for PAHs. In the case of fullerene, this is assumed to be the spherically symmetric jellium shell calculated by Puska & Nieminen (1993), which can be approximated by the following expression (Hadjar et al. 2001):
where r (in atomic units, a.u.^{}) is the distance from the fullerene center. The electron density decays outside the shell and toward the center in such a way that the major contribution comes from the region with 4 < r < 9.
The similarity in
electronic structure and bonding allows us to apply this jellium model
also to PAHs. However, the spherical geometry
is clearly not appropriate for PAHs, which we model instead as a thick
disk analogously to the distribution from Eq. (3)
where x is the coordinate along the thickness of the disk. This electron density peaks at the center of the molecule and vanishes outside, leading to a thickness 4.31 . The radius R of the disk is given by the usual expression for the radius of a PAH: , where is the number of carbon atoms in the molecule (Omont 1986). For a 50 Catoms PAH, .
Figure 1: The coordinate system adopted to calculate the energy transferred to a PAH via electronic excitation by ion collisions and by impacting electrons. The molecule is modeled as a disk with radius R and thickness d. The trajectory of the incoming particle is identified by the angle , while the angle corresponds to the diagonal of the disk. 

Open with DEXTER 
To calculate the energy transferred from Eq. (2), we adopt
the coordinate system shown in Fig. 1, where the
pathlength through the
PAH s is expressed as a function of the
coordinate x and of the angle
between the axes of the molecule and the direction of the incoming ion.
In this way for each trajectory given by
the corresponding energy transferred can be computed. We have
and the electron density is then given by
The density parameter can be rewritten as The friction coefficient has been calculated by Puska & Nieminen (1983) for various projectile ions and r_{s} values. It can be interpolated by the exponential function
where is the value of when r_{s} = 1.5. For hydrogen, helium and carbon the fit parameter R_{2} equals 2.28, 0.88 and 0.90, respectively.
The energy transferred is then given by the following equation
with from Eq. (6). The constant 27.2116 converts the dimensions of from atomic units to eV. For a given velocity of the incident particle, the value of will be maximum for (s = 2R, the longest pathlength) and minimum for (s = d, the shortest pathlength). The deposited energy also increases with the pathlength across the molecule, and then will be higher for larger PAHs impacted under a glancing collision.
The energy transferred determines the PAH dissociation probability upon electronic excitation, which is required to quantify the destruction induced by inelastic energy loss in the hot gas (see Sect. 4).
2.2 Nuclear interaction above threshold
In the present study we have to consider not only the electronic interaction described above, but the nuclear part of the ionic collision as well. The theory of nuclear interaction above threshold has been described in detail in MJT. We summarize here for clarity the essential concepts and the equations which will be used in the following.
For the nuclear interaction we consider only collisions above
threshold, i.e. collisions able to transfer more than the minimum
energy
required to remove a Catom from the PAH. To calculate the PAH
destruction due to nuclear
interaction, we use the rate of collisions above threshold between PAHs
and ions in a thermal gas, as given by Eq. (30) in MJT:
where f(v,T) is the Maxwellian velocity distribution function for ion, i, in the gas, is the Coulombian correction factor, is the nuclear interaction cross section per atom above threshold (Eq. (22) in MJT where E is the kinetic energy corresponding to v), and the factor 1/2 takes the averaging over the orientation of the disk into account.
For we adopt a value of 7.5 eV (see discussion in MJT, Sect. 2.2.1). The kinetic energy required for the incoming ion to transfer is the critical energy E_{0}. The lower integration limit v_{0} in Eq. (8) is the critical velocity corresponding to , which is the minimum kinetic energy for the projectile to have the nuclear interaction cross section different from zero (cf. Sect. 2.2 in MJT).
3 Electron collisions with PAHs
Fast electrons are abundant in a hot gas. Because of their low mass, they can reach very high velocities with respect to the ions, and hence high rates of potentially destructive collisions. We consider gas temperatures up to 10^{8} K, corresponding to a thermal electron energy of 10 keV, well below the relativistic limit of 500 keV. Under these lowenergy conditions, with respect to the relativistic regime, elastic collisions between electrons and target nuclei are not effective. The energy transfer occurs through inelastic interactions with target electrons (as for electronic excitation by impacting ions), which lead to a collective excitation of the molecule, followed eventually by dissociation or relaxation through IR emission.
The calculation of the energy transferred by such ``slow'' electrons is in fact a delicate matter. The theory developed under the first Born approximation (Bethe 1930) can be applied only to the most energetic electrons (around few keV) but is unsuitable for the rest of our range. At low energies (<10 keV), where the first Born approximation is no longer valid, the Mott elastic cross section must be used instead of the conventional Rutherford cross section (Mott & Massey 1949; Czyzewski et al. 1990). The Monte Carlo program CASINO (Hovington et al. 1997) computes the Mott cross sections in the simulation of electron interactions with various materials. Unfortunately the stopping power dE/dx is not included in the program output. An empirical expression for dE/dx has been proposed by Joy & Luo (1989), which nevertheless is reliable only down to 50 eV, while we are interested in the region between 10 and 50 eV as well.
We decided thus to derive the electron stopping power from
experimental results.
Measurements of the electron energy loss in PAHs are not available in
our energy
range of interest, so we use the measurement of dE/dx
in solid carbon for electrons
with energy between 10 eV and 2 keV (Joy 1995). The data points are well
fitted (to within few %) by the following function:
where E is the electron energy (in keV). The values of the fitting parameters are reported in Table 1. S(E) has the same functional form as the ZBL reduced stopping cross section for nuclear interaction (cf. Sect. 2.1 in MJT). The datapoints and the fitting function are shown in the top panel of Fig. 2.
Table 1: Analytical fit to the electron stopping power in solid carbon.
Figure 2: Top panel  Experimental measurement of dE/dx in solid carbon for electrons with energy between 10 eV and 2 keV, from Joy (1995), overlaid with the fitting function S(E) (solid line). Bottom panel  Integral F calculated numerically as a function of the energy of the incident electron, E. 

Open with DEXTER 
The stopping power increases sharply at low electron energies, reaches its maximum at 0.1 keV, and decreases smoothly afterwards. Between 0.01 and 0.1 keV a small variation of the energy of the incident electron will translate into a large change in the transferred energy per unit length. The shape of S(E) implies that only those electrons with energies that fall in a well defined window will efficiently transfer energy, while electrons below 0.02 keV and above 2 keV are not expected to contribute significantly to PAH excitation.
Once the stopping power dE/dx is known, we can calculate the energy transferred by an electron of given energy when travelling through the PAH. We adopt the same configuration used for electronic interaction, shown in Fig. 1. The trajectory of the incoming electron is defined by its impact angle and by the geometry of the molecule.
Because the thickness of the PAH is nonnegligible with
respect to its radius,
the stopping power is not constant along the electron path. To
calculate the energy loss we thus follow the procedure described below.
We have ,
then
(10) 
Thus, where is the maximum pathlength through the PAH. From inspection of Fig. 1, one can see that, if , , otherwise . E_{0} is the initial energy of the impacting electron, E_{1} is the electron energy after having travelled the distance , which needs to be calculated so we can then determine the energy transferred to the PAH
The integral F, calculated numerically as a function of E, is shown in the bottom panel of Fig. 2. We recognize that for low energies, F rises sharply, reflecting the small energy stopping power in this energy range (cf., top panel in Fig. 2). For higher energies, F(E) rises slowly (and linearly) with increasing energy over the relevant energy range. We note that the initial rise depends strongly on the (uncertain) details of the stopping power at low energies. However, it is of no consequence in our determination of the amount of energy deposited since we are only concerned with those collisions for which the energy deposition is in excess of the threshold energy (10 eV) over a pathlength of 1020 Å. Or to phrase it differently, at low energies a much larger pathlength has to be traversed (than is relevant for PAHs) in order to transfer sufficient energy to cause fragmentation. Then, since we know E_{0}, we can calculate F(E_{0}), and F(E_{1}) is then given by . We also calculated E as a function of F(E). We can then determine E_{1} from F(E_{1}) and, finally, from Eq. (11).
4 PAH destruction
4.1 Dissociation probability
Ion or electronic collisions (or UV photon absorption) can leave the molecule internally (electronically) excited with an energy . Internal conversion transfers this energy to vibrational modes, and the molecule can then relax through dissociation or IR emission. These two processes are in competition with each other. To quantify the PAH destruction due to ion and electron collisions we need to determine the probability of dissociation rather than IR emission.
In the microcanonical description of a PAH, the internal
energy, ,
is (approximately) related to the effective temperature of the system, ,
by the following equation
where is the binding energy of the fragment (Tielens 2005). This effective temperature includes a correction for the finite size of the heat bath in the PAH. The temperature is defined through the unimolecular dissociation rate, , written in Arrhenius form
where eV/K is the Boltzmann's constant (cf. Tielens 2005).
Consider the competition between photon emission at a rate
(photons s^{1})
and dissociation at a rate of
(fragments s^{1}). For simplicity,
we will assume that all photons have the same energy, .
The
probability that the PAH will fragment between the nth
and (n+1)th photon
emission is given by
The (unnormalized) probability per step p_{i} is given by and ), with the initial internal energy, coincident with the energy transferred into the PAH. The total dissociation probability is then given by
If we ignore the dependence of on E_{i}, the temperatures (Eq. (12)) drop approximately by . The probability ratio is approximately:
These equations become very difficult to solve in closed form. However, let us just assume that p_{i} does not vary and is given by . Then we have the total unnormalized dissociation probability
where we adopt photons s^{1} (Jochims et al. 1994), and the average temperature is chosen as the geometric mean
where and are the effective temperatures corresponding to (initial internal energy equal to the energy transferred) and (internal energy after the emission of photons). For the energy of the emitted IR photon we adopt the value eV, corresponding to a typical CC mode.
If the p_{i}'s were truly constant, then would be . However, they do decrease. So, rather we take it to be when the probability per step has dropped by a factor 10. A direct comparison between the full evaluation and this simple approximation yields , 20 and 40 for , 100 and 200 respectively. The quantity scales with because for a constant temperature (e.g., required to get the dissociation to occur), the internal energy has to scale with . As a result, the number of photons to be emitted also has to scale with .
The choice of the values to adopt for
and
is a delicate matter. In the laboratory the dissociation of highly
vibrationally excited PAHs is typically measured on timescales of
1100 s
because either the molecules are collisionally deexcited by ambient
gas or the molecules have left the measurement zone of the apparatus.
In contrast, in the ISM, the competing relaxation channel is through IR
emission and occurs typically on a timescale of 1 s. As is always the
case for reactions characterized by an Arrhenius law, a longer
timescale implies that the internal excitation energy can be lower.
This kinetic shift is well established experimentally and can amount to
many eV. Moreover, only small PAHs (up to 24 Catoms)
have been measured in the laboratory and the derived rates have to be
extrapolated to much larger (50 Catoms)
PAHs that are astrophysically relevant. In an astrophysical context,
the unimolecular dissociation of highly vibrationally excited PAHs 
pumped by FUV photons  has been studied experimentally by Jochims et al. (1994) and
further analyzed by Le Page
et al. (2001). Here, we will modify the analysis of Tielens (2005) for Hloss by UV
pumped PAHs to determine the parameters for carbon loss. The
dissociation rate  given by Eq. (13)  is governed
by two factors, the preexponential factor
and the energy .
The preexponential factor is given by
where is the entropy change which we set equal to 10 cal mole^{1} (Ling & Lifshitz 1998). We will ignore the weak temperature dependence of in the following and adopt s^{1}. The parameter can now be determined from a fit to the experiments by Jochims et al. (1994) on small PAHs. These experiments measured the appearance energy  the internal energy at which noticable dissociation of the PAH first occurred. The rate at which this happened was assumed to be 10^{4} s^{1}. Adopting this value, the appearance energy can be estimated from Eq. (13). The results of our analysis are shown in Fig. 3. The internal energy required to dissociate a PAH depends strongly on the PAH size. Likewise the kinetic shift associated with the relevant timescale at which the experiment was performed is quite apparent. Indeed, this kinetic shift can amount to tens of eV for relevant PAHs.
Figure 3: The appearance energy as a function of the number of Catoms in the PAH. The red line provides a fit to the experimental data using Eq. (13) for an assumed preexponential factor and a (fitted) Arrhenius energy, E_{0}=3.65 eV. The data points are the experimental results of Jochims et al. (1994). The blue line is the appearance energy for ISM conditions (e.g., at a rate of 1 s^{1}). 

Open with DEXTER 
The derived Arrhenius energy of 3.65 eV is small compared to the binding energy of a CH group in a PAH (4.2 eV, Ling & Lifshitz 1998). This is a well known problem in statistical unimolecular dissociation theories (cf. Tielens 2008). We emphasize that these results show that a typical interstellar PAH with a size of 50 Catoms would have a dissociation probability of 1/2 after absorption of an FUV photon of 12 eV (cf. Fig. 3). Hence, PAHs would be rapidly lost in the ISM through photolysis. It seems that the experiments on small PAHs cannot be readily extrapolated to larger, astrophysically relevant PAHs. Possibly, this is because experimentally C_{2}H_{2} loss has only been observed for very small catacondensed PAHs with a very open carbon skeleton (e.g., naphthalene, anthracene, and phenanthrene) which are likely much more prone to dissociation than the astrophysically more relevant pericondensed PAHs. Indeed, the small pericondensed PAHs, pyrene and coronene did not show any dissociation on the experimental timescales (Ling & Lifshitz 1998; Jochims et al. 1994).
Figure 4: The probability for dissociation of a 50 Catom PAH excited by 10 eV as a function of the Arrhenius energy, . 

Open with DEXTER 
Turning the problem around, we can determine the Arrhenius energy, , as a function of the dissociation probability by adopting an IR relaxation rate of 1 s^{1} and an internal excitation energy equal to a typical FUV photon energy (12 eV). The results for a 50 Catom PAH are shown in Fig 4. If we adopt a lifetime, , of 100 million years, a PAH in the diffuse ISM will have typically survived some UV photon absorptions (with cm^{2}, photons cm^{2} s^{1} in a Habing field). Hence, if the lifetime of the smallest PAHs in the ISM (e.g., with Catom) is set by photodissociation of the Cskeleton, the probability for dissociation has to be corresponding to an Arrhenius energy of 4.6 eV (Fig. 4). We note that in a PDR the photon flux is higher ( ) while the lifetime (of the PDR) is smaller ( yr), resulting in UV photons absorbed over the PDR lifetime. Survival of PAHs in a PDR environment would therefore require a somewhat larger E_{0} (or alternatively, only slightly larger PAHs could survive in such an environment).
We note that the binding energy of a CH group to small PAHs is estimated to be 4.2 eV and is probably somewhat larger for a 50 Catom condensed PAH. Loss of pure carbon, on the other hand, requires an energy of 7.5 eV, close to the binding energy of C to graphite. Loss of C from fullerenes has a measured of eV (Tomita et al. 2001). These latter two unimolecular dissociation channels are for all practical purposes closed under interstellar conditions. Finally, likely, Hloss will be the dominant destruction loss channel for large PAHs (E_{0}=3.3 eV), leading to rapid loss of all H's (Le Page et al. 2001; Tielens 2005). The resulting pure Cskeleton may then isomerize to much more stable carbon clusters, in particular fullerenes, and this may be the dominant ``loss'' channel for interstellar PAHs (cf. Tielens 2008, and references therein). It is clear that there are many uncertainties in the chemical destruction routes of interstellar PAHs and that these can only be addressed by dedicated experimental studies. For now, in our analysis of the unimolecular dissociation of PAHs  excited by electron or ion collisions  we will adopt eV as a standard value. We will however also examine the effects of adopting eV (e.g., p=1/2) and eV (e.g., ).
4.2 Collision rate
Once the dissociation probability is determined, we can calculate the
destruction rate through electronic excitation following electron or
ion collision. Adopting the configuration shown in Fig. 1, the destruction
rate is given by
with , running from 0 to 2 and from 0 to . Equation (20) can be rewritten as
The term v is the velocity of the incident particle, is the ion/electron relative abundance in the gas, and is the Coulombian correction factor, taking into account the fact that both target and projectiles are charged, and thus the collision cross section could be enhanced or diminished depending on the charge sign. The electron coulombian factor is always equal to 1 (to within 1%) because electrons have low mass. For a fixed temperature they reach higher velocities, with respect to the ions, and are thus less sensitive to the effects of the Coulombian field. The quantity is the angle between the vertical axes of the PAH and the direction of the projectile. The term is the geometrical cross section seen by an incident particle with direction defined by . The PAH is modelled as a thick disk with radius R and thickness d. The cross section is then given by
which reduces to for (faceon impact) and to for (edgeon impact). The term represents the total probability for dissociation upon electron collisions and electronic excitation, for a particle with velocity and incoming direction . It was calculated from Eq. (17) using the appropriated value of the energy transferred: for electrons (Eq. (11)) and for electronic excitation (Eq. (7)).
We are considering a hot gas and therefore we are interested
in the thermal
collision rate, given by
where is the electron/ion velocity corresponding to the electronic dissociation energy E_{0}. The temperature T is the same for both ions and electrons, but these latter will reach much larger velocities. From Eq. (21) we then expect to find a significantly higher collision rate with respect to the ion case.
Figure 5: Nuclear (dashed lines), electronic (solid lines) and electron (dasheddotted lines) rate constant for PAH carbon atom loss due to collisions with H, He, C and electrons in a thermal gas. The rate constants are calculated as a function of the gas temperature for three PAH sizes , 100, 200 Catoms, assuming the nuclear threshold energy T_{0} = 7.5 eV and the electronic dissociation energy E_{0} = 4.58 eV. 

Open with DEXTER 
5 Results
5.1 PAH destruction in a hot gas
To describe the destructive effects on PAHs of collisions with ions i (i = H, He, C) and electrons in a thermal gas we have to evaluate the rate constant for carbon atom loss.
For all processes the rate constant J is defined by the ratio , where is the thermal collision rate appropriate for nuclear and electronic excitation and electron collisions (cf. Eqs. (8) and (23)), and is the density of hydrogen nuclei. For electronic and electron interactions the rate must be multiplyied by a factor of 2, to take into account the fact that each collision leads to the loss of two carbon atoms.
The electron, nuclear and electronic rate constants for three PAH sizes (Nc = 50, 100 and 200 Catom) are shown in Fig. 5 as a function of the gas temperature. We assume for the nuclear threshold energy T_{0} the value of 7.5 eV (MJT), and for the electronic dissociation energy the value 4.58 eV (Sect. 4.1).
For the nuclear interaction, the threshold energy is independent from the PAH size, so the three curves start at the same temperature (not shown in the plot). The small separation between the curves is due to the fact that the PAH ``surface area''  and hence the rate constant  scales linearly with , therefore J is higher for bigger PAHs.
For nuclear (and electronic) interactions, the rate constants decrease from hydrogen to carbon because of the lower abundance of the heavier projectiles with respect to hydrogen (H:He:C = 1:0.1:10^{4}). On the other hand, the nuclear curves shift toward lower temperatures from lighter to heavier projectiles. This is the reflection of the fact that the critical energy of the particle, required to transfer the threshold energy T_{0}, decreases with increasing mass of the projectile itself. Then, a carbon atom with a temperature of K is hot enough to transfer the energy required for atom removal via nuclear interaction, whereas for hydrogen a temperature of at least 10^{4} K is necessary. The almostconstant behaviour after the initial rise reflects the large maximum observed in the nuclear cross section (cf. Fig. 2 in MJT).
The dissociation probability (Eq. (17)) depends on the binding energy of the fragment E_{0}, on the PAH size and on the energy transferred (through ), which in turns depends on the initial energy (velocity) of the projectile. For a thermal distribution, this latter will be determined by the gas temperature T.
The electronic rate constant curves for the different PAH sizes are well separated at the lowest temperatures. This reflects the fact that, for a fixed value of the transferred energy and of the electronic dissociation energy E_{0}, the dissociation probability decreases for increasing because either more energy is required in the bond that has to be broken or because the energy is spread over more vibrational modes and hence the internal excitation temperature is lower. On the other hand, the more energy that is deposited into the PAH, the higher is the dissociation probability. The energy transferred via electronic excitation (and then ) increases with the energy of the projectile up to a maximum value, corresponding to an incident energy of 100 keV for H (and higher for more massive particles), and decreases beyond that for higher energies. The energy content of a thermal gas at T = 10^{8} K is 9 keV, thus, in the temperature range considered in this study, the energy transferred increases with temperature (energy) and hence the dissociation probability increases as well. This is the basis for the monotonic rise of the electronic rate constant. After the initial separation, the three curves converge, because the rise in the transferred energy compensates the effect of increasing .
As discussed in Sect. 3, the energy transferred by impacting electrons rises sharply for energies in excess of 10 eV, peaks at 100 eV and decreases more slowly down to 10 keV. This results in a dissociation probability shaped as a step function: for keV, jumps from values close to zero up to 1. These limiting energies apply to a 50 Catom PAH; for the width of the step is smaller ( 1 keV), due to the fact that for a bigger PAH more energy has to be transferred for dissociation. This behaviour is reflected in the shape of the electron rate constant, where a steep rise is followed by a maximum, which is emphasised by the logarithmic scale used for the plot. As expected, the electron rate constant overcomes the electronic one, except for the highest gas temperatures. This results from the fact that, for a given temperature, electrons can reach higher velocities with respect to the ions (cf. Eqs. (21) and (23)).
To summarize, from Fig. 5 we can infer that, according to our model, the destruction process is dominated by nuclear interaction with helium at low temperatures (below K), and by electron collisions above this value. Small PAHs are easier destroyed than big ones for temperatures below 10^{6} K, while the difference in the destruction level reduces significantly for hotter gas.
Figure 6: Analytical fits to the calculated rate constants shown in Fig. 5. The ``Ionic'' curve is the fit to the sum of the nuclear and electronic rate constants, thus represents the total contribution from ion collisions to PAH destruction. 

Open with DEXTER 
The calculated rate constants, shown in Fig. 5, are
well fitted by the function ,
where f(T) is a polynomial of
order 5
For each PAH size we provide the fit to the electron rate constant; for the ions, the fit is over the sum of the nuclear and electronic rate constants, in order to provide an estimate of the global contribution from ionic collisions. The fits are shown in Fig. 6, and the fitting parameters are reported in Table 2. To provide an example of the accuracy of our fitting procedure, Fig. 7 shows the comparison between the calculated rate constant and the corresponding analytical fit, for electrons and helium impacting on a 50 Catom PAH. The He fit is over the sum of the nuclear and electronic rate constants. The average fitting discrepancy is 15% and the fits are therefore well within any uncertainties in the method.
Figure 8 shows the comparison between the carbon loss rate constants for a very big PAH, , and a 50 Catom molecule. We assume eV and eV. Because of the decrease of the dissociation probability when the PAH size increases, as expected, the electron and electronic rate constants are strongly suppressed, and both curves shift toward higher temperatures. Indeed, for such a big PAH, a much higher internal energy is required to reach the internal temperature where dissociation sets in. On the other hand, the nuclear rate constant increases linearly with the PAH size. As a result, for a 1000 carbon atoms PAH, the nuclear interaction is the dominant (and efficient) destruction mechanism up to K. In conclusion, electrons are responsible for the destruction of small/medium size PAH, while for big molecules this role is taken by ions.
Figure 7: Calculated rate constants for electrons and helium impacting on a 50 Catom PAH, overlaid are the corresponding analytical fits. The He fit is for the sum of the nuclear and electronic rate constants. The average discrepancy is 15%. 

Open with DEXTER 
As mentioned at the end of Sect. 4.1, we examined the effects of adopting different values for the Arrhenius energy, E_{0} = 3.65 and 5.6 eV, lower and higher, respectively, than our canonical value 4.6 eV. The results are shown in Fig. 9. The dissociation probability decreases for increasing E_{0}, because more energy is required in the bond that has to be broken. Hence, as expected, both the electron and electronic rate constants decrease in absolute value and shift toward highest temperatures. In particular the electronic thermal shift is very pronounced, indicating how sensitive this process is with respect to the assumed E_{0}. A variation in the adopted electronic excitation energy translates into a significant variation of the rate constant, reemphasizing the importance of experimental studies of this critical energy.
Figure 8: Carbon atom loss rate constant for electrons and hydrogen impacting against a 1000 Catom PAH. The rate constants for are shown for comparison. 

Open with DEXTER 
Table 2: Analytical fit parameters for the PAH carbon atom loss rate constant, calculated for electron and ion collisions.
Figure 9: Comparison between carbon atom loss rate constants calculated assuming three values for the electronic dissociation energy, : 3.65, 4.58 and 5.6 eV. The curves refer to electrons and hydrogen impacting against a 100 Catom PAH. The nuclear rate constant is calculated assuming eV. 

Open with DEXTER 
5.2 PAH lifetime
Under the effect of electron and ion collisions in a hot gas, the
number of carbon atoms in a PAH molecule varies with time. After a time
t, this number is
and the number of carbon atoms ejected from this PAH is
The quantity is the time constant appropriate for electron, nuclear and electronic interaction, given by
where and J are the thermal collision rate and the rate constant for electrons, nuclear and electronic interactions respectively, and is the hydrogen/electron density. For electrons and electronic excitation, the rate must be multipliyed by a factor of 2, because each interaction leads to the removal of two carbon atoms from the PAH. The nuclear rate scales linearly with , hence the corresponding fractional carbon atom loss is independent of PAH size.
For any given incoming ion and fixed PAH size , is univocally determined by the hydrogen/electron density and the gas temperature T. We assume that a PAH is destroyed after the ejection of 2/3 of the carbon atoms initially present in the molecule. This occurs after the time (Eq. (27)) which we adopt as the PAH lifetime against electron and ion bombardment in a gas with given density and temperature.
Table 3: Physical properties and PAH lifetime, , in objects showing PAH emission characteristics.
Table 3 summarizes relevant data and PAH lifetime, , for four objects characterized by warmtohot gas, Xray emission, and (bright) IR emission features. The lifetime has been calculated for PAHs with . (ref) has been evaluated adopting our reference values for the interaction parameters, E_{0} = 4.6 eV and T_{0} = 7.5 eV, (min) corresponds to the minimum values E_{0} = 3.65 eV and T_{0} = 4.6 eV, and (max) to the maximum values E_{0} = 5.6 eV and T_{0} = 15 eV. is the lifetime of the object.
Clearly, PAHs or related larger species can survive in these environments. Figure 10 shows the fractional Catom loss, due to electron and ion (H + He + C) collisions, for two widely different objects: the Orion Nebula (M 42) and the M 82 galaxy (cf. Table 3). The famous Orion Nebula is an H II region with high density ( cm^{3}) and low temperature (T = 7000 K) gas, while M 82 is a starburst galaxy, which shows outside the galactic plane, a spectacular bipolar outflow of hot and tenuous gas ( cm^{3}, K).
In M 82, PAHs are completely destroyed by electrons, even for the larger PAH, before electronic and nuclear contributions start to be relevant. The electron and electronic fractional losses decrease with PAH size, thus bigger molecules can survive longer, while the nuclear loss is independent of . The destruction timescale is very short: after one thousand years the PAHs should have completely disappeared.
In Orion the situation is reversed. At the temperature considered for this object, electrons and electronic excitation do not contribute to PAH erosion (cf. Fig. 5). The damage is caused by nuclear interaction due to He collisions, with a marginal contribution from carbon because of low abundance, and the timescale is much larger: only after 10 million years the PAH destruction becomes relevant. Of course, we have not evaluated the destruction of PAHs by Hionizing photons in the Orion H II region, which is expected to be very important.
The young (2500 yr) supernova remnant, N132D, in the Large Magellanic Clouds has been studied in detail at IR, optical, UV, and Xray wavelengths (Tappe et al. 2006; Morse et al. 1995). A Spitzer/IRS spectrum of the Southern rim shows evidence for the 1520 m plateau  often attributed to large PAHs or PAH clusters (Van Kerckhoven et al. 2000; Peeters et al. 2004)  and, tentatively, weak PAH emission features near 6.2, 7.7, and 11.2 m (Tappe et al. 2006). Tappe et al. (2006) attribute these features to emission from large (4000 Catom) PAHs either just swept up by the blast wave and not yet completely destroyed by the shock or in the radiative precursor of the shock. We calculate a lifetime of small (50200 Catom) PAHs in the relatively dense, hot gas of this young supernova remnant of 4 months (Table 3). In contrast, we estimate a lifetime of 150 yr for 4000 Catom species (cf. Eq. (27) and Fig. 8). It is clear that the PAHgrain size distribution will be strongly affected in this environment. Given advection of fresh material into the shocked hot gas, the observations are in reasonable agreement with our model expectations. We note that the observed shift to larger PAH sizes  so evident in the observations  implies that the emitting species are not associated with the precursor but are actualy tracing the postshock gas and are therefore likely heated through collisions with the hot electrons.
This discussion clearly shows that in a low density  high temperature gas, small PAHs are rapidly and completely destroyed. Survival of small PAHs in such environnement (and so the possibility to be detected) requires a protective environment and/or an efficient reformation mechanism.
6 Discussion
Figure 10: Nuclear and electronic fractional Catom loss as a function of time in the M 82 galaxy ( top) and in the Orion Nebula ( bottom), calculated for three PAH sizes , 100, 200 Catoms. The fractional carbon loss is defined as the number of carbon atoms ejected from the PAH after a given time divided by , and represents a direct indicator of the level of destruction of the PAH. Each curve shows the total contribution from collisions with H, He and C. In the nuclear case the fractional loss is independent from , so the three curves coincide, whereas for electrons and electronic interaction the fractional loss varies with the PAH size. In M 82 the PAH destruction is dominated by electron collisions and occurs on a very short timescale (thousand years). In Orion instead, because of the low gas temperature no electron and electronic contribution are possible (the rate constant is close to zero, see Fig. 5), and hence only nuclear interaction is responsible for the PAH erosion, which however takes place on a long timescale (some 10^{7} years). 

Open with DEXTER 
6.1 Xray absorption
As our calculations show, PAHs are rapidly destroyed in the hot gas associated with stellar winds and supernova explosions. Any PAHs observed near such regions have to be isolated from this hot gas and are presumably in cold gas entrained in these stellar and galactic winds. However, such PAHs would still be exposed to energetic Xray photons and these can be very destructive as well (BoechatRoberty et al. 2008; Voit 1992).
The photon absorption cross section of PAHs shows strong peaks at about 6 and 17.5 eV associated with transitions involving the and electronic manifolds and then another broad peak around 286 eV due to carbon Kshell transitions (Regier et al. 2007; de Souza et al. 2002; Keller et al. 1992). Each of these peaks can show various subpeaks due to electronic and vibrational structure. Here, we focus on the high energy peak. Because we are only concerned with the Planckaveraged cross section, all the fine detail will be washed out and we have elected to evaluate the Xray absorption rate adopting the measured absolute cross section of graphitic carbon taken from the NIST data base (Chantler 2000,1995). Figure 11 shows the (photon) averaged cross sections as a function of the black body temperature. As this figure illustrates, even the strong absorption edge due to the carbon Kshell is washed out by this averaging process, justifying our neglect of the fine detail in the absorption cross sections of individual PAHs. Our averaged cross section is also in good agreement with the recent study of BoechatRoberty et al. (2008) for benzene.
The photon absorption rate, ,
of a PAH exposed to an Xray photon flux,
is then given by,
(28) 
with the Planck average absorption cross section at temperature, . Consider now PAHs embedded in cold gas entrained in the stellar wind of the ionizing stars of the H II region M 17. The observed Xray luminosity is erg s^{1} and the Xray temperature is K (Townsley et al. 2003). With a projected emitting area of 42 pc^{2} this then implies an average Xray photon intensity of photons cm^{2} s^{1}. With an average cross section of cm^{2}/Catom, we calculate a photon absorption rate of photons/Catom/Myr. After Xray photon absorption, a PAH will typically lose a few Catoms and, hence, the estimated lifetime of PAHs entrained in the stellar winds from M 17 is 50 Myr. This is in excess of the stellar lifetime and the overall life time of the region. PAHs embedded in cold gas entrained in the galactic superwind of M 82 are exposed to somewhat harsher conditions. For M 82, at a distance of 3.6 Mpc, the observed soft (0.52.0 keV) Xray flux is 10^{11} erg cm^{2} s^{1} and the temperature is K. Evaluating the Xray flux at a distance of 3 kpc from the nuclear starburst region, we calculate a photon absorption rate of photons/Catom/Myr. Hence, in this environment, PAHs would be destroyed on a timescale of 20 Myr, comparable to or larger than the starburst lifetime. It is clear that PAHs in the hot gas are predominantly destroyed by collisions with the hot gas and that Xray photon absorption plays little role.
Finally, we note that here we have assumed that every Xray photon absorption will lead to photodissociation. Actually, Hshell electron ejection will be rapidly followed by the Auger effect filling the Kshell again and simultaneously ejecting a second electron. This process may leave the PAH internally excited with typically 1535 eV^{}. This energy is well above the measured appearance energy of PAH fragmentation for small PAHs under radiative cooling conditions (cf., Sect. 4.1) but larger PAHs may survive. Indeed, for an Arrhenius energy of 4.6 eV, a 50 Catom PAH requires about 24 eV of internal energy to dissociate with a probability of 1/2 (cf., Sect. 4.1). Hence, not every Xray photon absorption will lead to fragmentation, particularly for large PAHs. Further experiments on larger PAHs are required to settle this issue.
Figure 11: Planck averaged cross section of PAHs as a function of temperature. The cross section is on a per Catom basis. The strong carbon K shell band edge at 286 eV ( K) has been largely washed out by the averaging process. 

Open with DEXTER 
6.2 PAHs as tracers of cold entrained gas
The results in the previous subsection illustrate that PAHs can survive in the surface regions of cold gas clouds embedded in a hot gas for tens to hundreds of million years. The expansion of a stellar or galactic wind in an inhomogeneous environment will in a natural way lead to the entrainment of cold gas clumps (Hartquist & Dyson 1993; Chevalier & Clegg 1985; Smith et al. 1984; Marcolini et al. 2005; Strickland & Stevens 2000; Suchkov et al. 1994). The material in these clumps will only be mildly shocked  and PAH destruction by shocks is not expected as long as the shock velocity is less than about 100 km s^{1} (MJT)  and can be transported with the wind while losing its identity only slowly, mainly through evaporation into the hot gas driven by thermal conduction. Multiwavelength observations of such winds support this global view and much of the soft Xray and O VI absorbing and emitting gas is now thought to originate from the interaction interfaces between the tenuous hot gas and the cold dense clumps (Heckman et al. 2002; Chevalier & Clegg 1985).
A typical 0.5 keV Xray photon will penetrate a
column of about 10^{22} Hatoms/cm^{2}
and hence the ``PAHbright'' surfaces of such PDRs  which are
typically only a column of Hatoms/cm^{2}
thick  will be slowly depleted of PAHs on the timescale calculated in
Sect. 6.1.
However, at the same time, entrained clumps will slowly evaporate due
to thermal conduction. Considering classical thermal conduction, the
mass loss of a cloud due to evaporation into the hot gas is given by
(29) 
with T the temperature of the hot gas and R the radius of the clump (cf. Tielens 2005). Consider the galactic wind of M 82 and a typical structure with a size of 10 pc. Assuming thermal pressure equilibrium between the clump and the hot gas (e.g., ignoring ram pressure confinement which may actually be a factor of 10 larger), we estimate a density of 800 cm^{3} for a typical PDR temperature of 100 K for the galactic wind region of M 82. The lifetime of such a clump is then,
(30) 
Hence, ``fresh'' material will continuously be advected to the clump surface where ambient FUV photons can excite it. Thus, we conclude that such clumps can survive for a long time and that, proviso illumination by FUV photons, PAHs will form an excellent ``dye'' for tracing the presence of cold entrained material; or more specifically, for the exposed surfaces of photodissociation regions.
6.3 Comparison with previous studies
Dwek et al. (1996)
determines a sputtering rate for dust in a hot dust gas ( K)
that can be used to derive the lifetime,
of a grain of a given radius in a hot gas of a given density, i.e.
where a is the grain size and is the gas density. Clearly in this situation it is the smallest grain that suffer the fastest destruction. Hence, a treatment of the small grains, including PAHs, really needs to take into account the detailed physics of the interactions. For illustrative purposes, we can use Eq. (31) to show that grains with sizes typical of PAHs ( Å) should have lifetimes, in a tenuous hot gas ( cm^{3}), of the order of at least a few thousand years. We can see that this timescale is much longer than the typical PAH lifetimes that we derive here, i.e. few years for a 50 carbon atom PAH in a gas with cm^{3}. The timescale determination arrived at using Eq. (31) assumes that a PAH just behaves as a small grain. However, in the case of a grain, the sputtering yield is usually much less that unity because atoms displaced by knockon collisions in the solid can remain in the solid. The very much shorter lifetimes for the PAHs that we find can be ascribed to the fact that the transferred energy in incident electron and ion interactions always leads to the loss of carbon atoms from the PAH when that energy exceeds the relevant binding energy. In fact the equivalent PAH ``sputtering yield'' can be greater than unity because multiple atom ejection is possible. Indeed we assume here that the ejected species in the case of electronic interactions are C_{2} units.
The evolution of the dust and PAH thermal emission arising from a hot gas is affected by the changing dust size distribution. As pointed out by Dwek et al. (1996), it is the short wavelength emission, coming from the smallest grains, that is most affected by dust destruction. Our work now indicates that the destruction timescale is much shorter than that predicted by Dwek et al. because the erosion of the smallest grains and PAHs is enhanced by as much as three orders of magnitude compared to the earlier work. Thus, the gas cooling rates derived by Dwek (1987) will need to be reduced if a significant fraction of the dust mass is in the form of small grains and PAHs.
6.4 C_{2} groups loss
The primary channel for PAH erosion in a hot gas is the progressive loss of C_{2}H_{n} (n = 0, 1, 2) units following incident electron and ion excitation of the molecule. We note that this can only really occur from the periphery of the PAH (see the lower part of Fig. 11 in MJT for an illustration of this type of erosion). In this case we can see that a coherent aromatic structure will tend to be preserved, which is probably not the case where the inertial sputtering of C atoms is dominant. Thus, we conclude that PAH erosion in a hot gas will tend to preserve the aromatic structure throughout the destruction process.
As emphasized in MJT, PAH destruction may start with complete Hloss followed by isomerization to much more stable pure carbon clusters such as fullerenes (cf. Tielens 2008). While we have not assessed this point, we expect that such species will be more stable than PAHs in a hot gas.
7 Conclusions
We have extensively studied the stability of PAHs against electron and ion collisions (H, He and C) in a hot gas, such as the gas behind fast nonradiative shocks and in galactic outflows. Collisions can lead to carbon atom loss, with a consequent disruption and destruction of the molecule. We consider the case of a thermal gas with temperature T in the range 10^{3}  10^{8} K.
An ionic collision consists of two simultaneous processes which can be treated separately: a binary collision between the projectile ion and a single atom in the target (nuclear interaction) and energy loss to the electron cloud of the molecule (electronic interaction).
For the nuclear interaction, as described in MJT, we have modified the existing theory in order to treat collisions able to transfer energy above a specific threshold T_{0}. We adopt T_{0} = 7.5 eV as a reasonable value, but experimental determinations of this quantity are necessary.
The electronic energy transfer has been described in term of the stopping power of an electron gas with appropriate electron density (jellium approximation). For electron collisions, we derived an analytical expression for the measured electron stopping power in graphite and applied this to the case of PAHs.
The dissociation probability for a PAH excited by electronic interactions and electron collisions, has been derived using the theory of unimolecular reactions. The parameter E_{0}, which governs the dissociation probability, is not well constrained. We adopt a value of 4.6 eV consistent with extrapolations to interstellar conditions but better determinations, relevant to the astrophysical situation, are needed.
The PAH destruction process is dominated by electron collisions for gas temperatures above K, and by nuclear interaction with helium below this value. Small PAHs are more easily destroyed than larger ones below 10^{6} K, while the difference reduces significantly for a hotter gas. For a 1000 Catom PAH, nuclear interactions are the dominant destruction process.
In a hot and tenuous gas (e.g. M 82 galactic outflows), PAHs with sizes between 50 and 200 Catom are destroyed by electron collisions in few thousand years. In denser and colder regions (e.g. Orion), PAHs can survive for some 10^{7} yr before being destroyed by nuclear interaction processes.
Xray photon absorption plays little role in PAH destruction in the hot gas associated with stellar winds and supernova explosions, with respect to electron collisions. The PAH destruction process in a hot gas is therefore dominated by electron collisions. Any PAHs observed near such regions have to be isolated from this hot gas and are presumably in a cooler PDRtype gas entrained in the stellar and galactic winds. In this sense, PAHs represent a good tracer for the presence of entrained denser material.
Our calculated PAH lifetime in a hot tenuous gas ( K, cm^{3}), is much shorter than the lifetime of an equivalent dust grain of roughly the same size ( Å). Thus, might then imply that the destructive effects of ion and electron collisions with very small grains have previously been underestimated. The enhanced erosion of the smallest grain and PAHs implies that the gas cooling rates for a hot gas (T >10^{6} K)  which depend on the grain/PAH size distribution  may need to be reduced if a significant fraction of the dust mass is locked in small grains and PAHs.
PAH erosion in a hot gas occurs mainly through the ejection of C_{2} groups following electron collisions and electronic excitation. The C_{2} loss occurs at the periphery of the molecule, thus the aromatic structure will tend to be preserved throughout the destruction process.
AcknowledgementsWe are grateful to L. Allamandola and L. Verstraete for useful discussions, and we acknowledge our referee Tom Hartquist for careful reading and helpful comments. E.R.M. thanks G. Lavaux for support and technical assistance and acknowledges financial support by the EARA Training Network (EU grant MESTCT2004504604).
References
 Beirão, P., Brandl, B. R., Appleton, P. N., et al. 2008, ApJ, 676, 304 [NASA ADS] [CrossRef] [Google Scholar]
 Bethe, H. 1930, Ann. Physik, 5, 325 [Google Scholar]
 BoechatRoberty, H. M., Neves, R., Pilling, S., Lago, A. F., & de Souza, G. G. B. 2008, ArXiv eprints [Google Scholar]
 Chantler, C. T. 1995, J. Phys. Chem. Ref. Data, 24, 71 [NASA ADS] [CrossRef] [Google Scholar]
 Chantler, C. T. 2000, J. Phys. Chem. Ref. Data, 29(4), 597 [NASA ADS] [CrossRef] [Google Scholar]
 Chevalier, R. A., & Clegg, A. W. 1985, Nature, 317, 44 [NASA ADS] [CrossRef] [Google Scholar]
 Czyzewski, Z., O'Neill MacCallum, D., Romig, A., & Joy, D. C. 1990, J. Appl. Phys., 68, 3066 [NASA ADS] [CrossRef] [Google Scholar]
 de Souza, G. G. B., BoechatRoberty, H. M., Rocco, M. L. M., & Lucas, C. A. 2002, J. Electron Spec. Rel. Phen., 123, 315 [CrossRef] [Google Scholar]
 Désert, F.X., Boulanger, F., & Puget, J. L. 1990, A&A, 237, 215 [NASA ADS] [Google Scholar]
 Draine, B. T., & Li, A. 2001, ApJ, 551, 807 [NASA ADS] [CrossRef] [Google Scholar]
 Draine, B. T., & Salpeter, E. E. 1979, ApJ, 231, 438 [NASA ADS] [CrossRef] [EDP Sciences] [MathSciNet] [PubMed] [Google Scholar]
 Dwek, E. 1987, ApJ, 322, 812 [NASA ADS] [CrossRef] [Google Scholar]
 Dwek, E., Foster, S. M., & Vancura, O. 1996, ApJ, 457, 244 [NASA ADS] [CrossRef] [EDP Sciences] [MathSciNet] [PubMed] [Google Scholar]
 Engelbracht, C. W., Kundurthy, P., Gordon, K. D., et al. 2006, ApJ, 642, L127 [NASA ADS] [CrossRef] [Google Scholar]
 Ferrell, T. 1979, Solid State Commun., 32, 419 [NASA ADS] [CrossRef] [Google Scholar]
 Galliano, F., Madden, S. C., Tielens, A. G. G. M., Peeters, E., & Jones, A. P. 2008, ApJ, 679, 310 [NASA ADS] [CrossRef] [Google Scholar]
 Hadjar, O., Hoekstra, R., Morgenstern, R., & Schlathölter, T. 2001, Phys. Rev. A, 63, 033201 [NASA ADS] [CrossRef] [Google Scholar]
 Hartquist, T. W., & Dyson, J. E. 1993, QJRAS, 34, 57 [NASA ADS] [Google Scholar]
 Heckman, T. M., Norman, C. A., Strickland, D. K., & Sembach, K. R. 2002, ApJ, 577, 691 [NASA ADS] [CrossRef] [Google Scholar]
 Hovington, P., Drouin, D., & Gauvin, R. 1997, Scanning, 19, 1 [CrossRef] [Google Scholar]
 Hwang, U., Hughes, J. P., Canizares, C. R., & Markert, T. H. 1993, ApJ, 414, 219 [NASA ADS] [CrossRef] [Google Scholar]
 Jochims, H. W., Ruhl, E., Baumgartel, H., Tobita, S., & Leach, S. 1994, ApJ, 420, 307 [NASA ADS] [CrossRef] [Google Scholar]
 Jones, A. P., Tielens, A. G. G. M., Hollenbach, D. J., & McKee, C. F. 1994, ApJ, 433, 797 [NASA ADS] [CrossRef] [Google Scholar]
 Jones, A. P., Tielens, A. G. G. M., & Hollenbach, D. J. 1996, ApJ, 469, 740 [NASA ADS] [CrossRef] [Google Scholar]
 Joy, D. C. 1995, Scanning, 17, 270 [CrossRef] [Google Scholar]
 Joy, D. C., & Luo, S. 1989, Scanning, 11, 176 [Google Scholar]
 Keller, J. W., Coplan, M. A., & Goruganthu, R. 1992, ApJ, 391, 872 [NASA ADS] [CrossRef] [Google Scholar]
 Le Page, V., Snow, T. P., & Bierbaum, V. M. 2001, ApJS, 132, 233 [NASA ADS] [CrossRef] [Google Scholar]
 Lindhard, J., Scharff, M., & Schiott, H. E. 1963, Mat. Fys. Medd. Dan. Vid. Selsk., 33, No. 14 [Google Scholar]
 Ling, Y., & Lifshitz, C. 1998, JPC A, 102, 708 [Google Scholar]
 Marcolini, A., Strickland, D. K., D'Ercole, A., Heckman, T. M., & Hoopes, C. G. 2005, MNRAS, 362, 626 [NASA ADS] [CrossRef] [Google Scholar]
 Micelotta, E. R., Jones, A. P., & Tielens, A. G. G. M. 2010, A&A, 510, A36 (MJT) [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Morse, J. A., Winkler, P. F., & Kirshner, R. P. 1995, AJ, 109, 2104 [NASA ADS] [CrossRef] [Google Scholar]
 Mott, N. F., & Massey, H. S. W. 1949, The theory of atomic collisions, ed. N. F. Mott, & H. S. W. Massey (Oxford: Clarendon Press) [Google Scholar]
 Omont, A. 1986, A&A, 164, 159 [NASA ADS] [Google Scholar]
 Peeters, E., Mattioda, A. L., Hudgins, D. M., & Allamandola, L. J. 2004, ApJ, 617, L65 [NASA ADS] [CrossRef] [Google Scholar]
 Povich, M. S., Stone, J. M., Churchwell, E., et al. 2007, ApJ, 660, 346 [NASA ADS] [CrossRef] [Google Scholar]
 Puska, M. J., & Nieminen, R. M. 1983, Phys. Rev. B, 27, 6121 [NASA ADS] [CrossRef] [Google Scholar]
 Puska, M. J., & Nieminen, R. M. 1993, Phys. Rev. A, 47, 1181 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Ranalli, P., Comastri, A., Origlia, L., & Maiolino, R. 2008, MNRAS, 386, 1464 [NASA ADS] [CrossRef] [Google Scholar]
 Reach, W. T., Rho, J., Tappe, A., et al. 2006, AJ, 131, 1479 [NASA ADS] [CrossRef] [Google Scholar]
 Regier, T. Z., Shi, J., Tersingi, A., et al. 2007, Canadian Light Source, 51 [Google Scholar]
 Schlathölter, T., Hadjar, O., Hoekstra, R., & Morgenstern, R. 1999, Phys. Rev. Lett., 82, 73 [NASA ADS] [CrossRef] [Google Scholar]
 Sigmund, P. 1981, Sputtering by Particle Bombardment Vol. 1, ed. R. Behrisch, in Topics in Applied Physics (SpringerVerlag), 47 [Google Scholar]
 Smith, L. J., Pettini, M., Dyson, J. E., & Hartquist, T. W. 1984, MNRAS, 211, 679 [NASA ADS] [Google Scholar]
 Strickland, D. K., & Stevens, I. R. 2000, MNRAS, 314, 511 [NASA ADS] [CrossRef] [Google Scholar]
 Suchkov, A. A., Balsara, D. S., Heckman, T. M., & Leitherer, C. 1994, ApJ, 430, 511 [NASA ADS] [CrossRef] [Google Scholar]
 Tappe, A., Rho, J., & Reach, W. T. 2006, ApJ, 653, 267 [NASA ADS] [CrossRef] [Google Scholar]
 Tielens, A. G. G. M. 2005, The Physics and Chemistry of the Interstellar Medium (University of Cambridge Press) [Google Scholar]
 Tielens, A. G. G. M. 2008, ARA&A, 46, 289 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Tomita, S., Andersen, J. U., Gottrup, C., Hvelplund, P., & Pedersen, U. V. 2001, Phys. Rev. Lett., 87, 073401 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Townsley, L. K., Feigelson, E. D., Montmerle, T., et al. 2003, ApJ, 593, 874 [NASA ADS] [CrossRef] [Google Scholar]
 Van Kerckhoven, C., Hony, S., Peeters, E., et al. 2000, A&A, 357, 1013 [NASA ADS] [Google Scholar]
 Voit, G. M. 1992, MNRAS, 258, 841 [NASA ADS] [CrossRef] [Google Scholar]
Footnotes
 ... a.u.^{}
 Length (a.u.) = a_{0} = 0.529 Å, Velocity (a.u.) = 0.2 , Energy (a.u.) = 27.2116 eV.
 ... 1535 eV^{}
 The resulting PAH dication will quickly recombine with electrons and Coulomb explosion is of no consequence for such large PAHs.
All Tables
Table 1: Analytical fit to the electron stopping power in solid carbon.
Table 2: Analytical fit parameters for the PAH carbon atom loss rate constant, calculated for electron and ion collisions.
Table 3: Physical properties and PAH lifetime, , in objects showing PAH emission characteristics.
All Figures
Figure 1: The coordinate system adopted to calculate the energy transferred to a PAH via electronic excitation by ion collisions and by impacting electrons. The molecule is modeled as a disk with radius R and thickness d. The trajectory of the incoming particle is identified by the angle , while the angle corresponds to the diagonal of the disk. 

Open with DEXTER  
In the text 
Figure 2: Top panel  Experimental measurement of dE/dx in solid carbon for electrons with energy between 10 eV and 2 keV, from Joy (1995), overlaid with the fitting function S(E) (solid line). Bottom panel  Integral F calculated numerically as a function of the energy of the incident electron, E. 

Open with DEXTER  
In the text 
Figure 3: The appearance energy as a function of the number of Catoms in the PAH. The red line provides a fit to the experimental data using Eq. (13) for an assumed preexponential factor and a (fitted) Arrhenius energy, E_{0}=3.65 eV. The data points are the experimental results of Jochims et al. (1994). The blue line is the appearance energy for ISM conditions (e.g., at a rate of 1 s^{1}). 

Open with DEXTER  
In the text 
Figure 4: The probability for dissociation of a 50 Catom PAH excited by 10 eV as a function of the Arrhenius energy, . 

Open with DEXTER  
In the text 
Figure 5: Nuclear (dashed lines), electronic (solid lines) and electron (dasheddotted lines) rate constant for PAH carbon atom loss due to collisions with H, He, C and electrons in a thermal gas. The rate constants are calculated as a function of the gas temperature for three PAH sizes , 100, 200 Catoms, assuming the nuclear threshold energy T_{0} = 7.5 eV and the electronic dissociation energy E_{0} = 4.58 eV. 

Open with DEXTER  
In the text 
Figure 6: Analytical fits to the calculated rate constants shown in Fig. 5. The ``Ionic'' curve is the fit to the sum of the nuclear and electronic rate constants, thus represents the total contribution from ion collisions to PAH destruction. 

Open with DEXTER  
In the text 
Figure 7: Calculated rate constants for electrons and helium impacting on a 50 Catom PAH, overlaid are the corresponding analytical fits. The He fit is for the sum of the nuclear and electronic rate constants. The average discrepancy is 15%. 

Open with DEXTER  
In the text 
Figure 8: Carbon atom loss rate constant for electrons and hydrogen impacting against a 1000 Catom PAH. The rate constants for are shown for comparison. 

Open with DEXTER  
In the text 
Figure 9: Comparison between carbon atom loss rate constants calculated assuming three values for the electronic dissociation energy, : 3.65, 4.58 and 5.6 eV. The curves refer to electrons and hydrogen impacting against a 100 Catom PAH. The nuclear rate constant is calculated assuming eV. 

Open with DEXTER  
In the text 
Figure 10: Nuclear and electronic fractional Catom loss as a function of time in the M 82 galaxy ( top) and in the Orion Nebula ( bottom), calculated for three PAH sizes , 100, 200 Catoms. The fractional carbon loss is defined as the number of carbon atoms ejected from the PAH after a given time divided by , and represents a direct indicator of the level of destruction of the PAH. Each curve shows the total contribution from collisions with H, He and C. In the nuclear case the fractional loss is independent from , so the three curves coincide, whereas for electrons and electronic interaction the fractional loss varies with the PAH size. In M 82 the PAH destruction is dominated by electron collisions and occurs on a very short timescale (thousand years). In Orion instead, because of the low gas temperature no electron and electronic contribution are possible (the rate constant is close to zero, see Fig. 5), and hence only nuclear interaction is responsible for the PAH erosion, which however takes place on a long timescale (some 10^{7} years). 

Open with DEXTER  
In the text 
Figure 11: Planck averaged cross section of PAHs as a function of temperature. The cross section is on a per Catom basis. The strong carbon K shell band edge at 286 eV ( K) has been largely washed out by the averaging process. 

Open with DEXTER  
In the text 
Copyright ESO 2010