XUV Spectra from an ECR ion source plasma and from charge transfer collisions

Details XUV Spectra from an ECR ion source plasma and from charge transfer collisions XUV Spectra from an ECR ion source plasma and from charge transfer collisions

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..dmp.j6036l&link_type=abstract

American Physical Society, 2002 Division of Atomic, Molecular and Optical , abstract #J6.036

Physics

Scientific paper

Cometary x-ray production has been observed by space-based telescopes (e.g. ROSAT) and attributed to electron capture from comet gases by solar-wind ions [1]. To understand and identify the underlying collision processes, we are studying soft x-ray line emission from highly-charged oxygen ions in an electron cyclotron resonance (ECR) plasma using a grazing incidence XUV spectrometer. The spectrometer is calibrated using the 1snp resonance series of He^+ (30.4, 25.6, 24.3 ... nm). Preliminary identifications of many of the oxygen lines observed in the ECR plasma are presented. For example, in the range from 14-30 nm, we see lines attributable to O^3+ and O^4+ predominantly, at low levels of ECR microwave power ( ˜50 W). We are also studying charge-transfer collisions of highly-charged ions with target gases found in comets, such as CO and H_2O. This work will include direct measurements of the soft x-ray emission following collisions, such as in the system Fe^10+ + CO. The work is supported at JPL through contract with NASA, and at the Univ. of Conn. by NASA EPSCOR Grant No. NCC5-601 to the Connecticut Space Grant Consortium. --- [1] For example, see T. E. Cravens, Geophys. Res. Lett. v.24, 105 (1997); C. M. Lisse, et al., Science v.292, 1343 (2001).

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