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Abstract

  1. Top of page
  2. Abstract
  3. Introduction
  4. Chemical Model
  5. Anion Production Processes
  6. Discussion
  7. Conclusion
  8. Acknowledgments
  9. Editorial Handling
  10. References

Negative ions (anions) were identified in the coma of comet 1P/Halley during in situ Electron Electrostatic Analyzer measurements performed by the Giotto spacecraft in 1986. These anions were detected with masses in the range 7–110 amu, but with insufficient mass resolution to permit unambiguous identification. We present details of a new chemical-hydrodynamic model for the coma of comet Halley that includes—for the first time—atomic and molecular anions, in addition to a comprehensive hydrocarbon chemistry. Anion number densities are calculated as a function of radius in the coma, and compared with the Giotto results. Important anion production mechanisms are found to include radiative electron attachment, polar photodissociation, dissociative electron attachment, and proton transfer. The polyyne anions C4H and C6H are found to be likely candidates to explain the Giotto anion mass spectrum in the range 49–73 amu. The CN anion probably makes a significant contribution to the mass spectrum at 26 amu. Larger carbon-chain anions such as C8H can explain the peak near 100 amu provided there is a source of large carbon-chain-bearing molecules from the cometary nucleus.


Introduction

  1. Top of page
  2. Abstract
  3. Introduction
  4. Chemical Model
  5. Anion Production Processes
  6. Discussion
  7. Conclusion
  8. Acknowledgments
  9. Editorial Handling
  10. References

Gas-phase negative ions have been detected in surprisingly large abundances during spacecraft fly-bys of solar system bodies. During the March 1986 encounter of the Giotto spacecraft with the coma of comet 1P/Halley, the RPA-1 Electron Electrostatic Analyzer (EEA) detected energy spectra consistent with the presence of cold anions in the coma with masses 7–110 amu and number densities up to 1 cm−3 (Chaizy et al. 1991). Atomic and molecular anions O, OH, CN, C2H, and larger CHON particles were proposed by Chaizy et al. (1991) as plausible candidates to explain the observations, but due to the limited mass resolution of the Giotto anion mass spectra, unambiguous identification of the detected anions was not possible. The Cassini spacecraft performed similar measurements using the CAPS Electron Spectrometer (ELS) within the atmospheres of Titan (Coates et al. 2007) and Enceladus (Coates et al. 2010), and detected negative ions with masses per unit charge ranging from approximately 10 to 10,000 amu q−1.

Molecular anions were first detected in the interstellar medium using microwave spectroscopy (McCarthy et al. 2006). They have since been found to be abundant in a range of environments outside the solar system, and are an important part of the molecular inventory of the galaxy (Cordiner and Charnley 2012). Carbon-chain anions have been found to be abundant in quiescent molecular clouds, prestellar cores, and protostars (Brünken et al. 2007; Gupta et al. 2009; Sakai et al. 2007, 2010; Cordiner et al. 2011), as well as the carbon-rich AGB star IRC+10216 (Remijan et al. 2007). Chemical models have been able to reproduce the observed anion abundances in interstellar and circumstellar environments, and have shown that molecular anions have important effects on the chemistry and ionization balance of the gas (Cordiner and Millar 2009; Walsh et al. 2009; Cordiner and Charnley 2012; McElroy et al. 2013). Whereas chemical kinetic models have been successful in explaining the abundances of small molecular anions in Titan's upper atmosphere (Vuitton et al. 2009), the origin and importance of anions in the coma of comet 1P/Halley, as well as for comets in general (Wekhof 1981), remains to be understood.

In this article, we utilize a combined chemical/hydrodynamic model for the coma of comet Halley to explore various anion production mechanisms and compute the abundances of atomic and molecular anions as a function of radius in the coma.

Chemical Model

  1. Top of page
  2. Abstract
  3. Introduction
  4. Chemical Model
  5. Anion Production Processes
  6. Discussion
  7. Conclusion
  8. Acknowledgments
  9. Editorial Handling
  10. References

Our model is based on the five-fluid coma model of Rodgers and Charnley (2002), which models the dynamics of a neutral fluid, a positively charged fluid, an electron fluid, and fluids of fast atomic and molecular hydrogen. These fluids emanate from the nucleus in a spherically symmetric outflow (see also Rodgers et al. 2004), and the abundances of various chemical species are calculated as a function of radius. The chemical network has been fully updated in the present study and incorporates reactions between 279 chemical species (composed of H, C, N, and O atoms, and electrons). The list of species consists of 154 cations, 23 anions (listed in Table 1) and 101 neutrals. Hydrocarbon chemistry is modeled for species containing up to eight C-atoms. Carbon-chain-bearing anions are included because of the importance of C2 and C3 in cometary comae (Weiler 2012), and because their gas-phase chemistry is better understood than other classes of anions such as PAHs. The abundances of the modeled species are linked by a total of 3823 chemical reactions, 3367 of which were taken from the latest version of the UMIST database for astrochemistry (RATE12; McElroy et al. 2013), including 685 reactions involving anions.

Table 1. Anions included in the model
H, O, OH, O2
C, C2, C3, C4, C5, C6, C7, C8
CH, C2H, C3H, C4H, C5H, C6H, C7H, C8H
CN, C3N, C5N

Solar photoreaction rates at 1 AU have been taken from Huebner et al. (1992) and Crovisier (1994) where available. New photodissociation rates were calculated for hydrocarbons based on the cross sections of Van Hemert and van Dishoeck (2008), integrated over the quiet sun solar irradiance spectrum (Woods et al. 2009). For the remaining neutral species, known photorates for structurally similar species were used, with product channels taken from the RATE12 database. Anion photodetachment rates were calculated using the square-root threshold law (Millar et al. 2007). We used measured cross sections above threshold for C2H, C4H, and C6H (from Best et al. 2011), and for OH (Trippel et al. 2006). Above-threshold photodetachment cross sections were assumed to be 10−17 cm2 for all other anions.

Mutual neutralization reactions have been included between all anions in the model and the most abundant cations, including H2O+, H3O+, NH4+, C2H2+, C2H4+, HCNH+, CH3OH2+, and CH3OCH4+, with rate coefficients of 7.5 × 10−8 (Tc/300)−0.5 cm3 s−1. In this formula Tc is the effective collision temperature, defined by

  • display math(1)

where Ti and Ta are the respective temperatures of the (cat)ionic and anionic reactants, and mi and ma are their respective masses.

A further 78 reactions involving anions have been added, including proton transfer, dissociative electron attachment, and polar photodissociation. A summary of the main chemical processes involving anions in the coma model is given in Table 2. The dominant anion formation processes are described in more detail in 'Anion Production Processes' section.

Table 2. Anion reaction types included in the coma model
AbbreviationReaction typeExample
REARadiative electron attachmentA  +  e[RIGHTWARDS ARROW] A +
PPDPolar photodissociationAB + hv [RIGHTWARDS ARROW] A + B+
DEADissociative electron attachmentAB + e [RIGHTWARDS ARROW] A + B
PTProton transferAH + B[RIGHTWARDS ARROW] A + BH
MNMutual neutralizationA + B+[RIGHTWARDS ARROW] A  +  B
AEDAssociative electron detachmentA + B [RIGHTWARDS ARROW] AB + e
ANAnion-neutralA + B [RIGHTWARDS ARROW] C + D
CTCharge transferA + B [RIGHTWARDS ARROW] A  +  B
PDPhotodetachmentA + [RIGHTWARDS ARROW] A  +  e

The contribution of anion chemistry to the energetics of the gas is negligible in the majority of models considered here due to the relatively small anion abundances. The kinetic temperature of the anions is assumed to be identical to the temperature of the neutral gas from which they are formed.

Our model for Halley assumes a spherical nucleus with radius 3.36 km, heliocentric distance 0.89 AU, temperature 192 K, and H2O production rate of Q(H2O) = 6.9 × 1029 s−1, appropriate to the time of the Giotto encounter on 13 March 1986 (Schmidt et al. 1988). Production rates of parent species are given in Table 3. These have been taken from the compilation of Haider and Bhardwaj (2005), with the addition of C8H2, that has been included as representative of a generic long-chain hydrocarbon molecule (see 'Radiative Electron Attachment').

Table 3. Production rates for parent species relative to H2O
SpeciesProduction rate SpeciesProduction rate
H2O1.0 C2H43.00 × 10−3
CH46.25 × 10−3 CO1.00 × 10−1
NH31.88 × 10−2 C2H64.00 × 10−3
C2H22.50 × 10−2 CH3OH2.13 × 10−2
HCN1.25 × 10−3 CO23.75 × 10−2
N21.25 × 10−3 C8H21.00 × 10−5

Anion Production Processes

  1. Top of page
  2. Abstract
  3. Introduction
  4. Chemical Model
  5. Anion Production Processes
  6. Discussion
  7. Conclusion
  8. Acknowledgments
  9. Editorial Handling
  10. References

Radiative Electron Attachment

Two main processes are responsible for initiation of the anion chemistry in the inner coma (at radial distances less than approximately 1000 km from the nucleus): radiative electron attachment and polar photodissociation. As a result of their large electron affinities, combined with a high vibrational density of states, carbon-chain-bearing molecules (including polyynes, CnH, for > 3), possess the ability to attach low-energy free electrons and undergo rapid radiative relaxation to form stable anions (Herbst and Osamura 2008). As shown in Fig. 1c, the C6H number density quickly reaches >1 cm−3 as a result of radiative electron attachment to C6H. The C6H molecule is formed in the coma from electron recombination of C6H4+—a moderately large hydrocarbon ion that arises in the model as a product of acetylene photochemistry. The neutral-neutral reaction

  • display math(2)

results in the formation of a large amount of C4H (reaching a production rate of approximately 10−4 Q(H2O)). However, due to its smaller size, C4H is theorized to possess a smaller radiative electron attachment rate than C6H (Herbst and Osamura 2008), causing C4H to be less abundant than C6H in the inner coma. The larger C8H anion is abundant in our model as a consequence of the inclusion of C8H2 as a parent. In the innermost regions of the coma (at radial distances <10 km), where few solar UV photons penetrate, C8H is produced as a result of charge transfer from H+ to C8H2, which forms C8H2+ ions that undergo subsequent electron recombination to C8H + H. At larger radii, photodissociation of C8H2 is the dominant source of C8H.

image

Figure 1. Modeled negative ion (anion) number densities in the coma of comet 1P/Halley as a function of distance from the nucleus.

Download figure to PowerPoint

The majority of the C3N in the model comes from radiative electron attachment to C3N, which is produced predominantly as a result of the neutral-neutral reaction

  • display math(3)

Polar Photodissociation

At distances greater than approximately 10 km from the nucleus, the penetration of solar UV radiation becomes sufficiently strong that polar photodissociation (PPD) of neutral molecules becomes an important source of negative ions. Also known as threshold ion pair production, PPD is the process by which absorption of radiation by a molecule AB results in the production of a pair of oppositely charged product species A and B+ (see Table 2). Polar photodissociation of H2O, HCN, CO, and CO2 was studied in the laboratory by Hunniford et al. (2007), Berkowitz et al. (1969), Dadouch et al. (1991), and Mitsuke et al. (1990), respectively. Our model incorporates rates for PPD calculated in the solar radiation field using the cross sections given by Vuitton et al. (2009), integrated over the applicable energy range for each process (taken from the original laboratory studies).

Polar photodissociation of H2O by photons in the energy range 36–100 eV produces both O and H (Hunniford et al. 2007). This is the dominant production mechanism for atomic anions in our coma model. The O number density as a function of radius is shown in Fig. 1a, which reaches a peak value of 0.4 cm−3 at a radius of approximately 80 km. Polar photodissociation of CO is the primary production mechanism for C throughout the coma.

Proton Transfer

Polar photodissociation of HCN is an important source of CN, but the dominant production mechanism for this anion in our model is via loss of protons from HCN through proton-transfer reactions. The transfer of protons from neutral species to anions can be highly exoergic depending on the acidity of the neutral in question, and such reactions are almost always extremely fast in the gas phase (Vuitton et al. 2009). For the anions in our model, we have included all relevant exoergic proton-transfer reactions, with rate coefficients taken from the RATE12 database and from Vuitton et al. (2009) where available. Reaction rates have been extrapolated to the additional anions in our model where necessary.

As a result of its high proton affinity, H quickly reacts with H2O to produce OH + H2. Consequently, OH reaches a large number density in the coma, similar to that of O. Abundant C2H is produced by proton transfer from C2H2 to O and OH. Proton transfer from HCN to C4H and C6H is the dominant source of CN for radii less than approximately 2000 km.

Dissociative Electron Attachment

For radii greater than approximately 2000 km, dissociative electron attachment (DEA) to HCN is the dominant source of CN. The onset of this formation process manifests as the emergence of a secondary peak in the CN number density at around 10,000 km (see Fig. 1b), dominating over the proton transfer and polar photodissociation formation channels at these radii. Dissociative electron attachment rates have been calculated for the anions in our model by convolving the (Maxwellian) electron energy distribution with experimentally derived cross sections for anion formation as a function of energy. References to much of the original laboratory data are summarized by Vuitton et al. (2009), who also provide the peak cross sections and energies. Additional DEA cross section data for C2H2, CO2, and O2 have been taken from May et al. (2008) and Rapp and Briglia (1965). Gaussian profiles have been assumed for the cross sections as a function of energy, which is a good approximation in most cases. A Gaussian FWHM of 1.0 eV has been used in the case of HC3N (and HC5N), for which no detailed cross section profile data have been published.

Dissociative electron attachment only becomes significant as a source of negative ions in the outer coma, where the electron energies become sufficient to overcome the energy barrier of this endothermic process. For example, DEA of HCN occurs at an electron energy of 2.5 eV, so the peak rate for CN formation from HCN occurs for electron temperatures Te = 2.9 × 104 K, but begins to become significant at Te > 1000 K, when sufficient electrons possess the required 2.5 eV. Energetic electrons are produced by photo-ionization of water molecules. However, their temperatures only obtain large values in the outer coma where the lower density results in a reduction in the amount of energy lost in inelastic collisions with H2O (Rodgers and Charnley 2002).

Secondary anion abundance peaks in the outer coma are also observed in our model for the following anions (see Fig. 1): OH (produced from DEA of H2O), C2H, C2 (from DEA of C2H2), and C3N (from DEA of HC3N). Secondary DEA peaks are not seen for the larger polyyne anions (CnH, for n > 3), because their large radiative electron attachment rates dominate the other anion formation processes.

Discussion

  1. Top of page
  2. Abstract
  3. Introduction
  4. Chemical Model
  5. Anion Production Processes
  6. Discussion
  7. Conclusion
  8. Acknowledgments
  9. Editorial Handling
  10. References

Chaizy et al. (1991) detected anions in the coma of comet Halley with masses in the range 7–110 amu, and despite the limited resolution of the mass spectra, identified three main peaks at (1) 7–19 amu, (2) 22–65 amu, and (3) 85–110 amu. They referred to these as the “17 amu group,” the “30 amu group,” and the “100 amu group,” respectively. The most likely candidate species to explain Peak 1 (17 amu group) are shown in Fig. 1a: O and OH, C and CH. In our model, O is the most abundant of these anions throughout much of the coma – OH is slightly more abundant in the inner regions (at a radial distance < 200 km from the nucleus) and outer regions (r > 10,000 km). Chaizy et al. (1991) derived anion number densities for Peak 1 starting at more than 1 cm−3 at = 3 × 103 km and falling to a few times 10−4 cm−3 at = 3 × 104 km, (as shown in their fig. 4). Outside of the comet's ionopause (at = 4500), our modeled Peak 1 anion abundances are about two orders of magnitude less than observed.

The mass range covered by Peak 2 (30 amu group) contains the relatively small di/tri-atomic anions C2, CN, and C2H, as well as some of the medium-sized carbon-chain-bearing anions: C4H and C3N. Over the range of the Giotto data (from r = 3 × 103 km to 3 × 104 km), the observed Peak 2 anion densities fall from approximately 10−2 to 10−5 cm−3. As can be seen in Fig. 1, our modeled number densities for CN and C4H match this trend quite well (within an order of magnitude) at all radii. Figure 4 of Chaizy et al. (1991) shows a rise in the observed number density of these “30 amu group” anions between 1 × 104 km and 2 × 104 km, which is consistent with the location of the rise in anion abundances (including that for CN), which occurs as a result of DEA in the outer coma.

Peak 3 (100 amu group) contains the larger carbon-chain-bearing anion C8H, and C6H lies at the overlap between Peak 2 and Peak 3. Our modeled number densities for these species as a function of radius are again consistent (within about an order of magnitude) with the number densities of anions in this mass range detected by Giotto.

The C8H2 molecule is included as a parent in the coma model, and is intended to be representative of the class of large carbon-chain-bearing species that could plausibly be present as a component of cometary nuclei (Mumma and Charnley 2011). Photodissociation of C8H2 is assumed to result in H-atom loss to produce the polyyne C8H, although alternative product channels are possible, including loss of various numbers of carbon atoms. Long carbon chains and polyynes (including C8H) undergo radiative electron attachment at similarly rapid rates (Herbst and Osamura 2008). Thus, C8H in our model can be considered as representative of the class of anions that arise in the coma as a consequence of the release of dusty, carbon-chain-rich material from the nucleus. The appearance of a strong anion mass peak in the Giotto observations at around 100 amu is thus readily explainable. As a final point, we note that if a sufficient quantity of long carbon chains is released from the nucleus (with a production rate greater than approximately 10−4 Q(H2O)), rapid radiative electron attachment ensues and molecular anions can be formed in such large abundances that they become the dominant carriers of negative charge in the inner coma (at distances <103 km from the nucleus). Evidence for the presence of abundant carbon chains in Halley was provided by Geiss et al. (1999), who derived a C4H production rate of 0.023 Q(H2O). In such a situation, the total abundance of anions is sufficiently large that their thermodynamic effects on the coma begin to become important. A proper treatment of these effects will require the inclusion of a separate anion fluid in future hydrodynamical coma models. The properties of such an anion fluid will be examined in detail by Cordiner and Charnley (Forthcoming).

The scatter on the anion number densities as a function of radius presented by Chaizy et al. (1991) is considerable, and often larger than the associated error bars. Uncertainty is inherent in their results due to the fact that the Giotto EESA was calibrated for use in electron spectroscopy rather than (heavy) ion spectroscopy. In fact, the efficiency of the EESA microchannel plate (MCP) detector for measuring negative ion fluxes is highly uncertain due to a lack of laboratory calibration for such purposes. Thus, the results of Chaizy et al. (1991) can only be considered approximate such that a direct quantitative comparison of our results may not be meaningful. Nevertheless, the agreement between observations and our model predictions is reasonably good, especially considering some of the uncertainties in the model. Based on laboratory measurements of polyyne anions and OH, the photodetachment cross sections employed for many of the other anions (including O, OH, CN, and C3N), are likely to be accurate to within a factor of a few at best. Because photo detachment is by far the dominant anion destruction mechanism, errors on these cross sections propagate in an approximately linear fashion to the modeled abundances of these species. For those species whose production is dominated by polar photodissociation, a potentially more significant source of error is the uncertainty in the PPD cross sections, which have been approximated and may only be accurate within 1-2 orders of magnitude. Thus, we highlight a need for dedicated laboratory measurements of these values. Due to a similar lack of laboratory measurements for electron attachment to neutrals at low energies and densities, the radiative electron attachment (REA) rates for all anions in the model are based on theoretical calculations. Previous endeavors to model observed anion abundances in dark molecular clouds and circumstellar envelopes have shown that the theoretical REA rates are reasonably accurate for C6H and C8H, but less so for C4H, the rate for which seems to have been overestimated.

Other possible sources of uncertainty in our model include a lack of measured rate coefficients for several important proton-transfer reactions, including the reactions of O and OH with C2H2, and the polyyne anions with HCN. In addition, our list of PPD and DEA reactions is incomplete due to a lack of laboratory studies of these processes for some abundant coma molecules such as NH3, H2CO, and CH3OH. Possible anionic products from PPD and DEA reactions involving these species may include NH2, CH, and CH3O, respectively, which are not included in our model.

The fact that our model produces about two orders of magnitude less Peak 1 anions (O, OH) than observed may be indicative of missing formation processes for these species. For example, Chaizy et al. (1991) hypothesized that anions could be produced in high-energy collisions between neutral species in the coma. The process of anion production through collisions between neutral species at energies up to 20 eV was reviewed by Wexler (1973). Cross sections for anion production in higher-energy impacts can also be significant (see Tawara 1978). Cross sections on the order of 10−18 cm2 were measured in the range 100–1000 eV by Gealy and Van Zyl (1987) for anion production in collisions between H and H2. This process could be an important source of anions in the coma given a sufficiently strong source of energetic atoms or molecules. Eviatar et al. (1989) deduced that such a flux of neutral species may be present in the coma of comet Halley as part of a theory to explain the fluxes of fast ions detected by Giotto. Given the dominance of water in the coma, collisional dissociation of H2O may thus be considered a plausible source of H, O, and OH. However, collisional dissociation of H2O—and other abundant coma molecules—has yet to be studied in the laboratory, so the existence of these hypothetical anion production channels (not to mention their cross sections), is presently unknown.

Conclusion

  1. Top of page
  2. Abstract
  3. Introduction
  4. Chemical Model
  5. Anion Production Processes
  6. Discussion
  7. Conclusion
  8. Acknowledgments
  9. Editorial Handling
  10. References

A reasonably good agreement has been achieved between observed and modeled anion abundances in the coma of comet 1P/Halley, despite uncertainties in various cross sections and rates for anion production and destruction. The dominant anion production mechanisms are found to be polar photodissociation of water and radiative electron attachment to carbon chains in the inner coma, followed by proton transfer from C2H2 and HCN to produce C2H and CN, respectively. In the outer regions of the coma where electron temperatures reach on the order of 103–105 K, dissociative electron attachment becomes a dominant process.

We find particularly good agreement for CN and C4H in the “30 amu group” identified by Chaizy et al. (1991), and for C6H and C8H in the “100 amu group.” We thus confirm the hypothesis that CN is a likely carrier of the 20-30 amu anion mass peak observed by Giotto in the 1986 encounter with comet Halley. The polyyne anions C4H and C6H are likely constituents of the mass spectrum in the range 49-73 amu. Larger carbon-chain-bearing anions such as C8 and C8H can explain the mass peak near 100 amu, provided a source of large carbon-chain-bearing molecules is present in the cometary nucleus.

If our interpretation of anion chemistry in the Giotto data is correct, then comets may contain significant abundances of long carbon-chain molecules. Measurements with the Ion and Electron Sensor on the Rosetta spacecraft during its scheduled 2014 encounter with comet 67P/Churyumov-Gerasimenko will provide additional insight into this issue. A more complete understanding of cometary anions will be facilitated by future laboratory measurements of absolute cross sections for anion photodetachment and polar photodissociation of H2O and other abundant coma molecules.

Acknowledgments

  1. Top of page
  2. Abstract
  3. Introduction
  4. Chemical Model
  5. Anion Production Processes
  6. Discussion
  7. Conclusion
  8. Acknowledgments
  9. Editorial Handling
  10. References

This research was supported by NASA's Planetary Atmospheres Program and the NASA Astrobiology Institute through the Goddard Center for Astrobiology.

References

  1. Top of page
  2. Abstract
  3. Introduction
  4. Chemical Model
  5. Anion Production Processes
  6. Discussion
  7. Conclusion
  8. Acknowledgments
  9. Editorial Handling
  10. References
  • Berkowitz J., Chupka W. A., and Walter T. A. 1969. Photoionization of HCN: The electron affinity and heat of formation of CN. Journal of Chemical Physics 50:14971500.
  • Best T., Otto R., Trippel S., Hlavenka P., von Zastrow A., Eisenbach S., Jézouin S., Wester R., Vigren E., Hamberg M., and Geppert W. D. 2011. Absolute photodetachment cross-section measurements for hydrocarbon chain anions. The Astrophysical Journal 742:6368.
  • Brünken S., Gupta H., Gottlieb C. A., McCarthy M. C., and Thaddeus P. 2007. Detection of the carbon chain negative ion C8H in TMC-1. The Astrophysical Journal 664:L43L46.
  • Chaizy P., Reme H., Sauvaud J. A., D'Uston C., Lin R. P., Larson D. E., Mitchell D. L., Anderson K. A., Carlson C. W., Korth A., and Mendis D. A. 1991. Negative ions in the coma of comet Halley. Nature 349:393396.
  • Coates A. J., Crary F. J., Lewis G. R., Young D. T., Waite J. H. Jr., and Sittler E. C. Jr. 2007. Discovery of heavy negative ions in Titan's ionosphere. Geophysical Research Letters 34:L22103.
  • Coates A. J., Jones G. H., Lewis G. R., Wellbrock A., Young D. T., Crary F. J., Johnson R. E., Cassidy T. A., and Hill T. W. 2010. Negative ions in the Enceladus plume. Icarus 206:618622.
  • Cordiner M. A. and Charnley S. B. 2012. Gas-grain chemical models for interstellar carbon chain anions. The Astrophysical Journal 749:120129.
  • Cordiner M. A. and Millar T. J. 2009. Density-enhanced gas and dust shells in a new chemical model for IRC+10216. The Astrophysical Journal 697:6878.
  • Cordiner M. A., Charnley S. B., Buckle J. V., Walsh C., and Millar T. J. 2011. Discovery of interstellar anions in Cepheus and Auriga. The Astrophysical Journal Letters 730:L18L22.
  • Crovisier J. 1994. Photodestruction rates for cometary parent molecules. Journal of Geophysical Research 99:37773781.
  • Dadouch A., Dujardin G., Hellner L., and Besnard-Ramage M. J. 1991. Highly excited quasistable states of neutral CO lying up to the double-ionization-energy level. Physical Review A 43(11):60576065.
  • Eviatar A., Goldstein R., Young D. T., Balsiger H., Rosenbauer H., and Fuselier S. 1989. Energetic ion fluxes in the inner coma of comet 1P/Halley. The Astrophysical Journal 339:545557.
  • Gealy M. W. and Van Zyl B. 1987. Cross sections for electron capture and loss. II. H impact on H and H2. Physical Review A 36:31003107.
  • Geiss J., Altwegg K., Balsiger H., and Graf S. 1999. Rare atoms, molecules and radiacals in the coma of P/Halley. Space Science Reviews 90:253268.
  • Gupta H., Gottlieb C. A., McCarthy M. C., and Thaddeus P. 2009. A survey of C4H, C6H and C6H- with the Green Bank Telescope. The Astrophysical Journal 691:14941500.
  • Haider S. A. and Bhardwaj A. 2005. Radial distribution of production rates, loss rates and densities corresponding to ion masses <40 amu in the inner coma of Comet Halley: Composition and chemistry. Icarus 177:196219.
  • Herbst E. and Osamura Y. 2008. Calculations on the formation rates and mechanisms for CnH anions in interstellar and circumstellar media. The Astrophysical Journal 679:16701679.
  • Huebner W. F., Keady J. J., and Lyon S. P. 1992. Solar photo rates for planetary atmospheres and atmospheric pollutants. Astrophysics and Space Science 195:1289.
  • Hunniford C. A., Scully S. W., Dunn K. F., and Latimer C. J. 2007. Fragment anion spectroscopy of water in the inner and outer valence regions. Journal of Physics B 40:12251232.
  • May O., Fedor J., Ibanescu B. C., and Allan M. 2008. Absolute cross sections for dissociative electron attachment to acetylene and diacetylene. Physical Review A 77:040701.
  • McCarthy M. C., Gottlieb C. A., Gupta H. C., and Thaddeus P. 2006. Laboratory and astronomical identification of the negative molecular ion C6H. The Astrophysical Journal 652:L141L144.
  • McElroy D., Walsh C., Markwick A. J., Cordiner M. A., Smith K., and Millar T. J. 2013. The UMIST database for astrochemistry 2012. Astronomy & Astrophysics 550:3649.
  • Millar T. J., Walsh C., Cordiner M. A., Ni Chuimin R., and Herbst E. 2007. Hydrocarbon anions in interstellar clouds and circumstellar envelopes. The Astrophysical Journal 662:L87L90.
  • Mitsuke K., Suzuki S., Imamura T., and Koyano I. 1990. Negative-ion mass spectrometric study of ion-pair formation in the vacuum ultraviolet. II. Journal of Chemical Physics 93:17101719.
  • Mumma M. J., and Charnley S. B. 2011. The chemical composition of comets—Emerging taxonomies and natal heritage. Annual Review of Astronomy and Astrophysics 49:471524.
  • Rapp D. and Briglia D. D. 1965. Total cross sections for ionization and attachment in gases by electron impact. II. Negative-ion formation. Journal of Chemical Physics 43:14801489.
  • Remijan A. J., Hollis J. M., Lovas F. J., Cordiner M. A., Millar T. J., Markwick-Kemper A. J., and Jewell P. R. 2007. Detection of C8H- and comparison with C8H toward IRC +10 216. The Astrophysical Journal 664:L47L50.
  • Rodgers S. D. and Charnley S. B. 2002. A model of the chemistry in cometary comae: Deuterated molecules. Monthly Notices of the Royal Astronomical Society 330:660674.
  • Rodgers S. D., Charnley S. B., Huebner W. F., and Boice D. C. 2004. Physical processes and chemical reactions in cometary comae. In Comets II, edited by Festou M. C., Keller H. U., and Weaver H. A. Tucson, Arizona: The University of Arizona Press. pp. 505522.
  • Sakai N., Sakai T., Osamura Y., and Yamamoto S. 2007. Detection of C6H toward the low-mass protostar IRAS 04368 + 2557 in L1527. The Astrophysical Journal 667:L65L68.
  • Sakai N., Shiino T., Hirota T., Sakai T., and Yamamoto S. 2010. Long carbon-chain molecules and their anions in the starless core, Lupus-1A. The Astrophysical Journal 718:L49L52.
  • Schmidt H. U., Wegman R., Huebner W. F., and Boice D. C. 1988. Cometary gas and plasma flow with detailed chemistry. Computer Physics Communications 49:1759.
  • Tawara H. 1978. Cross sections for charge transfer of hydrogen beams in gases and vapors in the energy range 10 eV – 10 keV. Atomic Data and Nuclear Data Tables 22:491525.
  • Trippel S., Mikosch J., Berhane R., Otto R., Weidemueller M., and Wester R. 2006. Photodetachment of cold OH in a multipole ion trap. Physical Review Letters 97:193003.
  • Van Hemert M. C. and van Dishoeck E. F. 2008. Photodissociation of small carbonaceous molecules of astrophysical interest. Chemical Physics 33:292302.
  • Vuitton V., Lavvas P., Yelle R. V., Galand M., Wellbrock A., Lewis G. R., Coates A. J., and Wahlund J. E. 2009. Negative ion chemistry in Titan's upper atmosphere. Planetary and Space Science 57:15581572.
  • Walsh C., Harada N., Herbst E., and Millar T. J. 2009. The effects of molecular anions on the chemistry of dark clouds. The Astrophysical Journal 700:725761.
  • Weiler M. 2012. The chemistry of C3 and C2 in cometary comae. Astronomy & Astrophysics 538:A149.
  • Wekhof A. 1981. Negative ions in comets. The Moon and Planets 24:157173.
  • Wexler S. 1973. Associative and non-associative ion pair formation by fast atoms. Berichte der Bunsen-Gesellschaft 778:606627.
  • Woods T. N., Chamberlin P. C., Harder J. W., Hock R. A., Snow M., Eparvier F. G., Fontenla J., McClintock W. E., and Richard E. C. 2009. Solar irradiance reference spectra (SIRS) for the 2008 whole heliosphere interval (WHI). Geophysical Research Letters 36:L01101.