Soft X-ray and Optical Laboratory Spectra to Simulate the Solar Wind on Comets: O5+ + CO

Details Soft X-ray and Optical Laboratory Spectra to Simulate the Solar Wind on Comets: O5+ + CO Soft X-ray and Optical Laboratory Spectra to Simulate the Solar Wind on Comets: O5+ + CO

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..774..281e&link_type=abstract

X-RAY DIAGNOSTICS OF ASTROPHYSICAL PLASMAS: Theory, Experiment, and Observation. AIP Conference Proceedings, Volume 774, pp. 28

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2

Solar Wind, Comets, X-Ray Sources (Astronomical), Ultraviolet Sources (Astronomical), Oxygen, Carbon Compounds, X-Ray Spectra, Ultraviolet Spectra, Heliopause And Solar Wind Termination, X-Ray, Ultraviolet, Atomic And Molecular Data, Spectra, And Spectral Parameters

Scientific paper

UV/soft x-ray and optical measurements of relative line emission cross sections from collisions of O5+ with CO vapor have been made, as part of a laboratory study of interactions between minority solar-wind ions and gases found in comets. The interaction of O5+ with CO yields prototypical information applicable to other highly-charged solar wind ion interactions. The data are at least approximately consistent with a simple classical Coulomb ``over-the-barrier'' model prediction: strong XUV emission (~13-25 nm range) is observed in collisions in the slow and fast solar wind velocity range. We attribute this light to electron capture from the target molecule by the projectile ion into an excited n=4 level, plus cascade into n=3, resulting in emission lines from (O4+ )*. The optical spectra, taken at higher velocities, show a lack of line emission from projectile states in the visible range (400-850nm) the visible lines observed can be attributed primarily to excitation of atoms from the molecular target following dissociation.

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