Laboratory studies of cometary x-ray emission mechanisms using the ASTRO-E spare microcalorimeter

Details Laboratory studies of cometary x-ray emission mechanisms using the ASTRO-E spare microcalorimeter Laboratory studies of cometary x-ray emission mechanisms using the ASTRO-E spare microcalorimeter

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprn17022b&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

Beginning in 2000 the spare GSFC ASTRO-E 6x6 microcalorimeter array has been successfully interfaced with the LLNL electron beam ion trap facility. This has opened up the possibility for simulating the X-ray emission from comets produced by charge-exchange recombination between solar wind heavy ions and cometary gases and recording the resulting spectra with high resolution. Our measurements have focused on the K-shell emission following the interaction of bare C, N, O and their hydrogenlike counter parts with such gases as CO_2, N_2, and CH_4. We find that the emission not only reflects the composition and intensity of the solar wind, but also is a diagnostic of the solar wind velocity. Moreover, the detailed emission depends on the chemical composition of the cometary gases. The measurements provide an excellent test bed for analyses of the data that will be obtained following the launch of ASTRO-E2. This work was supported by NASA's Planetary Atmospheres Program and performed by UC-LLNL under the auspices of DOE under Contract No. W-7405-Eng-48.

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