The Escape of O⁺ and CO⁺ Ions from Mars and Titan Atmospheres by Coulomb Explosion of CO₂²⁺ Molecular Dications

• Authors: S. Falcinelli
• Languages of publication: EN

Abstracts

EN

Main properties of multiply charged molecular ions (energetics, structure, stability, lifetime and fragmentation dynamics) are relevant to know and to model the behavior of gaseous plasmas, planetary ionospheres, and astrophysical environments. Experimental measurements of the kinetic energy released of fragment ions produced by the Coulomb explosion of molecular dications (doubly charged molecular species) originating by double photoionization of CO₂ molecules, are reported and discussed. The kinetic energy released, as a function of the UV photon energy in the range of 34-50 eV, is extracted from the electron-ion-ion coincidence spectra recorded by using tunable synchrotron radiation coupled with ion imaging techniques at the GasPhase beam line of ELETTRA Synchrotron Light Laboratory Trieste, Italy. This kind of experiment allows assessing the probability of escape for simple ionic species in the ionosphere of Mars and Titan. The kinetic energy released, measured in the case of O⁺ and CO⁺ fragment ions, are ranging between 1.0-5.0 and 0.4-3.0 eV, respectively. These values are large enough to allow such ionic species in participating in the atmospheric escape from Mars (only O⁺ ions) and Titan (both O⁺ and CO⁺ ions) into space. In the case of Mars, we suggest a possible rationalization for the observed behavior of the O⁺ and CO₂²⁺ ion density profiles by Viking 1 lander and Mariner 6 spacecraft.

Keywords

EN

31.15.ag; 31.50.Bc; 33.15.Ta; 33.80.Eh; 37.20.+j; 95.30.Cq; 95.30.Dr; 95.30.Ft; 95.30.Ky; 94.05.Rx; 94.20.Cf; 94.20.D-; 94.20.dv; 94.20.W-; 94.20.wg

Discipline

• 95.30.Cq: Elementary particle processes
• 94.20.wg: Ionosphere/atmospheric interactions
• 31.15.ag: Excitation energies and lifetimes; oscillator strengths
• 95.30.Dr: Atomic processes and interactions
• 37.20.+j: Atomic and molecular beam sources and techniques
• 94.05.Rx: Experimental techniques and laboratory studies(see also 52.72.+v—in physics of plasmas)
• 33.15.Ta: Mass spectra
• 94.20.W-: Ionospheric dynamics and interactions
• 33.80.Eh: Autoionization, photoionization, and photodetachment
• 94.20.dv: Ion chemistry and composition; ionization mechanisms
• 95.30.Ky: Atomic and molecular data, spectra, and spectral parameters (opacities, rotation constants, line identification, oscillator strengths,gfvalues, transition probabilities, etc.)
• 94.20.D-: Ionospheric structure, composition
• 31.50.Bc: Potential energy surfaces for ground electronic states
• 94.20.Cf: Ionospheric modeling and forecasting
• 95.30.Ft: Molecular and chemical processes and interactions

• Publisher: Institute of Physics, Polish Academy of Sciences
• Journal: Acta Physica Polonica A
• Year: 2017
• Volume: 131
• Issue: 1
• Pages: 112-116

Dates

published

2017-01

Contributors

author

S. Falcinelli

• Department of Civil and Environmental Engineering, University of Perugia, Via G. Duranti 93, 06125 Perugia, Italy

References

• [1] B. Brunetti, P. Candori, R. Ferramosche, S. Falcinelli, F. Vecchiocattivi, A. Sassara, M. Chergui, Chem. Phys. Lett. 294, 584 (1998), doi: 10.1016/S0009-2614(98)00916-6
• [2] F. Biondini, B.G. Brunetti, P. Candori, F. De Angelis, S. Falcinelli, F. Tarantelli, F. Pirani, F. Vecchiocattivi, J. Chem. Phys. 122, 164308 (2005), doi: 10.1063/1.1884605
• [3] B. Brunetti, P. Candori, D. Cappelletti, S. Falcinelli, F. Pirani, D. Stranges, F. Vecchiocattivi, Chem. Phys. Lett. 539-540, 19 (2012), doi: 10.1016/j.cplett.2012.05.020
• [4] S. Falcinelli, A. Bartocci, S. Cavalli, F. Pirani, F. Vecchiocattivi, J. Chem. Phys. 143, 164306 (2015), doi: 10.1063/1.4933429
• [5] S. Falcinelli, A. Bartocci, S. Cavalli, F. Pirani, F. Vecchiocattivi, Chem. Eur. J. 22, 764 (2016), doi: 10.1002/chem.201503692
• [6] S. Falcinelli, F. Pirani, F. Vecchiocattivi, Atmosphere 6, 299 (2015), doi: 10.3390/atmos6030299
• [7] M. Alagia, N. Balucani, P. Candori, S. Falcinelli, F. Pirani, R. Richter, M. Rosi, S. Stranges, F. Vecchiocattivi, Rendic. Lincei Sci. Fis. Natur. 24, 53 (2013), doi: 10.1007/s12210-012-0215-z
• [8] V. Vuitton, O. Dutuit, M.A. Smith, N. Balucani, in: Titan: Surface, Atmosphere and Magnetosphere, Eds. I. Müller-Wodarg, C.A. Griffith, E. Lellouch, T.E. Cravens, Cambridge University Press, 2013, Ch. 7, doi: 10.1017/CBO9780511667398.010
• [9] S. Falcinelli, M. Rosi, P. Candori, F. Vecchiocattivi, J.M. Farrar, F. Pirani, N. Balucani, M. Alagia, R. Richter, S. Stranges, Lect. Notes Comput. Sci. LNCS 8579, 554 (2014), doi: 10.1007/978-3-319-09144-0_38
• [10] M. Larsson, W.D. Geppert, G. Nyman, Rep. Prog. Phys. 75, 066901 (2012), doi: 10.1088/0034-4885/75/6/066901
• [11] S. Falcinelli, in: Recent Advances in Energy, Environment and Financial Planning - Mathematics and Computers in Science and Engineering Series, Eds. F. Batzias, N.E. Mastorakis, C. Guarnaccia, Vol. 35, WSEAS Press, Athens 2014, p. 84
• [12] L. Pei, E. Carrascosa, N. Yang, S. Falcinelli, J.M. Farrar, J. Phys. Chem. Lett. 6, 1684 (2015), doi: 10.1021/acs.jpclett.5b00517
• [13] P. Candori, S. Falcinelli, F. Pirani, F. Tarantelli, F. Vecchiocattivi, Chem. Phys. Lett. 436, 322 (2007), doi: 10.1016/j.cplett.2007.01.061
• [14] S. Falcinelli, F. Fernandez-Alonso, K. Kalogerakis, R.N. Zare, Mol. Phys. 88, 663 (1996), doi: 10.1080/00268979650026208
• [15] P. Tosi, R. Correale, W. Lu, S. Falcinelli, D. Bassi, Phys. Rev. Lett. 82, 450 (1999), doi: 10.1103/PhysRevLett.82.450
• [16] M.M. Teixidor, F. Pirani, P. Candori, S. Falcinelli, F. Vecchiocattivi, Chem. Phys. Lett. 379, 139 (2003), doi: 10.1016/S0009-2614(03)01348-4
• [17] M. Alagia, B.G. Brunetti, P. Candori, S. Falcinelli, M.M. Teixidor, F. Pirani, R. Richter, S. Stranges, F. Vecchiocattivi, J. Chem. Phys. 120, 6985 (2004), doi: 10.1063/1.1669383
• [18] M. Alagia, F. Biondini, B.G. Brunetti, P. Candori, S. Falcinelli, M. Moix Teixidor, F. Pirani, R. Richter, S. Stranges, F. Vecchiocattivi, J. Chem. Phys. 121, 10508 (2004), doi: 10.1063/1.1809116
• [19] M. Alagia, P. Candori, S. Falcinelli, F. Pirani, M.S. Pedrosa Mundim, R. Richter, M. Rosi, S. Stranges, F. Vecchiocattivi, Phys. Chem. Chem. Phys. 13, 8245 (2011), doi: 10.1039/c0cp02678f
• [20] L. Pauling, J. Chem. Phys. 1, 56 (1933), doi: 10.1063/1.1749219
• [21] C.A. Nicolaides, Chem. Phys. Lett. 161, 547 (1989), doi: 10.1016/0009-2614(89)87036-8
• [22] P. Stauber, S.D. Doty, E.F. van Dishoeck, A.O. Benz, Astron. Astrophys. 440, 949 (2005), doi: 10.1051/0004-6361:20052889
• [23] R. Thissen, O. Witasse, O. Dutuit, C.S. Wedlund, G. Gronoff, J. Lilensten, Phys. Chem. Chem. Phys. 13, 18264 (2011), doi: 10.1039/C1CP21957J
• [24] L. Schio, C. Li, S. Monti, P. Salén, V. Yatsyna, R. Feifel, M. Alagia, R. Richter, S. Falcinelli, S. Stranges, V. Zhaunerchyk, V. Carravetta, Phys. Chem. Chem. Phys. 17, 9040 (2015), doi: 10.1039/c4cp05896h
• [25] M. Alagia, E. Bodo, P. Decleva, S. Falcinelli, A. Ponzi, R. Richter, S. Stranges, Phys. Chem. Chem. Phys. 15, 1310 (2013), doi: 10.1039/c2cp43466k
• [26] S. Falcinelli, M. Rosi, P. Candori, J.M. Farrar, F. Vecchiocattivi, F. Pirani, N. Balucani, M. Alagia, R. Richter, S. Stranges, Planet. Space Sci. 99, 149 (2014), doi: 10.1016/j.pss.2014.04.020
• [27] R.R. Blyth, R. Delaunay, M. Zitnik, J. Krempasky, R. Krempaska, J. Slezak, K.C. Prince, R. Richter, M. Vondracek, R. Camilloni, L. Avaldi, M. Coreno, G. Stefani, C. Furlani, M. de Simone, S. Stranges, M.-Y. Adam, J. Electron Spectrosc. Relat. Phenom. 101-103, 959 (1999), doi: 10.1016/S0368-2048(98)00381-8
• [28] M. Alagia, P. Candori, S. Falcinelli, M. Lavollée, F. Pirani, R. Richter, S. Stranges, F. Vecchiocattivi, Chem. Phys. Lett. 432, 398 (2006), doi: 10.1016/j.cplett.2006.10.100
• [29] M. Alagia, P. Candori, S. Falcinelli, M. Lavollée, F. Pirani, R. Richter, S. Stranges, F. Vecchiocattivi, Phys. Chem. Chem. Phys. 12, 5389 (2010), doi: 10.1039/b926960f
• [30] M. Alagia, P. Candori, S. Falcinelli, M. Lavollée, F. Pirani, R. Richter, S. Stranges, F. Vecchiocattivi, J. Chem. Phys. 126, 201101 (2007), doi: 10.1063/1.2743616
• [31] M. Alagia, P. Candori, S. Falcinelli, M. Lavollée, F. Pirani, R. Richter, S. Stranges, F. Vecchiocattivi, J. Phys. Chem. A 113, 14755 (2009), doi: 10.1021/jp9048988
• [32] M. Lavollée, Rev. Sci. Instrum. 70, 2968 (1990), doi: 10.1063/1.1149855
• [33] M. Lundqvist, P. Baltzer, D. Edvardsson, L. Karlsson, B. Wannberg, Phys. Rev. Lett. 75, 1058 (1995), doi: 10.1103/PhysRevLett.75.1058
• [34] T.A. Field, J.H.D. Eland, Chem. Phys. Lett. 211, 436 (1993), doi: 10.1016/0009-2614(93)87087-J
• [35] M. Alagia, C. Callegari, P. Candori, S. Falcinelli, F. Pirani, R. Richter, S. Stranges, F. Vecchiocattivi, J. Chem. Phys. 136, 204302 (2012), doi: 10.1063/1.4720350
• [36] O. Witasse, O. Dutuit, J. Lilensten, R. Thissen, J. Zabka, C. Alcaraz, P.-L. Blelly, S.W. Bougher, S. Engel, L.H. Andersen, K. Seiersen, Geophys. Res. Lett. 29, 1263 (2002), doi: 10.1029/2002GL014781
• [37] T.E. Cravens, I.P. Robertson, J.H. Jr. Waite, R.V. Yelle, W.T. Kasprzak, C.N. Keller, S.A. Ledvina, H.B. Niemann, J.G. Luhmann, R.L. McNutt, W.-H. Ip, V. De La Haye, I. Mueller-Wodarg, J.-E. Wahlund, V.G. Anicich, V. Vuitton, Geophys. Res. Lett. 33, L07105 (2006), doi: 10.1029/2005GL025575
• [38] P. Franceschi, R. Thissen, J. Zabka, J. Roithová, Z. Herman, O. Dutuit, Int. J. Mass Spectrom. 228, 507 (2003), doi: 10.1016/S1387-3806(03)00157-X
• [39] A.E. Slattery, T.A. Field, M. Ahmad, R.I. Hall, J. Lambourne, F. Penent, P. Lablanquie, J.H.D. Eland, J. Chem. Phys. 122, 084317 (2005), doi: 10.1063/1.1850895
• [40] S. Falcinelli, F. Pirani, M. Alagia, L. Schio, R. Richter, S. Stranges, N. Balucani, F. Vecchiocattivi, Atmosphere 7, 112 (2016), doi: 10.3390/atmos7090112
• [41] S. Falcinelli, F. Pirani, M. Alagia, L. Schio, R. Richter, S. Stranges, F. Vecchiocattivi, Chem. Phys. Lett. 666C, 1 (2016), doi: 10.1016/j.cplett.2016.09.003
• [42] S. Falcinelli, M. Rosi, S. Cavalli, F. Pirani, F. Vecchiocattivi, Chem. Eur. J. 22, 12518 (2016), doi: 10.1002/chem.201601811

Identifiers

DOI

10.12693/APhysPolA.131.112