Contributors to the solar-wind-induced spectrum of cometary x-rays: S and Ne L x-rays, Fe M x-rays and others

Details Contributors to the solar-wind-induced spectrum of cometary x-rays: S and Ne L x-rays, Fe M x-rays and others Contributors to the solar-wind-induced spectrum of cometary x-rays: S and Ne L x-rays, Fe M x-rays and others

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aps..dmp.o1076v&link_type=abstract

American Physical Society, 37th Meeting of the Division of Atomic, Molecular and Optical Physics, May 16-20, 2006, abstract #O1.

Physics

Scientific paper

Cravens explained the presence of well resolved x-ray lines from comets as being due to the transfer of electrons from cometary gases (CO, H2O, etc.) to create excited states of highly-charged C and O ions from the solar wind (1). However, these x rays, with energies in the 250 to 700 eV range, represent only a small fraction of the x rays observed compared with those found in the 50 - 250 eV range (2). Spectra obtained, using solar wind-type ions such as Ne^7+,8+, S^9+ and Fe^11+ from the JPL ECR ion source, suggest that soft x-ray lines from charge-transfer processes terminating on the n=2, and n=3 levels of solar wind ions may contribute significantly to cometary x-ray spectra in this range. 1. T.E. Cravens, Science 297, 1042 (2002). 2. K. Dennerl, J. Englhauser, Joachim Trumper, Science 277,1625 (1997).

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