Ionization and dissociation of cometary gaseous organic molecules by solar wind particles - I. Formic acid

• Published in: Monthly notices of the Royal Astronomical Society 2006-11, Vol.372 (3), p.1379-1388
• Main Authors: Pilling, S., Santos, A. C. F., Wolff, W., Sant'Anna, M. M., Barros, A. L. F., De Souza, G. G. B., De Castro Faria, N. V., Boechat-Roberty, H. M.
• Format: Article
• Language: English
• Subjects: astrochemistry; Astronomy; Atoms & subatomic particles; comets: general; Earth, ocean, space; Exact sciences and technology; Gases; molecular data; molecular process; Particle physics; Simulation; solar wind; Stars & galaxies; Wind
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2006.10949.x

In order to simulate the effects of energetic charged particles present in the solar wind colliding with the cometary gaseous formic acid molecule (HCOOH), laboratory experiments have been performed. The absolute ionization and dissociation cross-sections for this molecule interacting with solar wind particles were measured employing fast electrons in the energy range of 0.5 to 2 keV and energetic protons with energies varying from 0.128 to 2 MeV. Despite the fact that both projectiles lead to a very similar fragmentation pattern, differences in the relative intensities of the fragments were observed. Formic acid survives about four to five times more to the proton beam than to the energetic electron collision. The minimum momentum transfer in the electron impact case was estimated to be 3-38 per cent larger than the minimum momentum transfer observed with the equivelocity protons. The ultraviolet (UV) photodissociation rates and half-lives for HCOOH are roughly closer to the values obtained with energetic electrons. It is consequently important to take electron impact data into account when developing chemical models to simulate the interplanetary conditions.