Electron density determinations of stellar coronae using Fe XXI ndarrow2p (n=3,4,5,6) transitions

Details Electron density determinations of stellar coronae using Fe XXI ndarrow2p (n=3,4,5,6) transitions Electron density determinations of stellar coronae using Fe XXI ndarrow2p (n=3,4,5,6) transitions

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprb17057c&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

The idea of using L-shell iron spectroscopic information to infer the electron density has become very attractive following the availability of high-resolution data measured by current x-ray observatories. Following suggestions in [1], we developed the n darrow2p line (n=3,4,5,6) intensities in Fe XXI as a diagnostic that is sensitive to densities near 10^13 cm-3 and applied it to Chandra observations of HR1099. HULLAC code predictions of the density sensitivity were checked with the Livermore EBIT-II ion trap for low densities. Checks at high density are in progress at the Princeton NSTX tokamak. For HR1099 we find a density of about 2 to 8 x 10^13 cm-3. This is in the range of 10^12 - 10^13 cm-3 that was determined using the Fe XXI EUV line ratios (102/128 ÅÅobserved with EUVE [2]. This work was performed under the auspice of DOE by UC-LLNL under contract W-7405-Eng-48 and supported by DOE OFES and by NASA SARA grants to LLNL, GSFC, PPPL and Columbia University.\$[1]. Wargelin, et al, APJ 496 (1998). [2]. Ayres,et al, APJ, 549, (2001) 554)

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