Identification of Three Weak Lines and Their Influences on Diagnostics of Electron Temperature and Density in Astrophysical Plasmas

Details Identification of Three Weak Lines and Their Influences on Diagnostics of Electron Temperature and Density in Astrophysical Plasmas Identification of Three Weak Lines and Their Influences on Diagnostics of Electron Temperature and Density in Astrophysical Plasmas

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004chphl..21.2063l&link_type=abstract

Chinese Physics Letters, Volume 21, Issue 10, pp. 2063-2066 (2004).

Physics

Scientific paper

By comparing of the spectra from the Chandra LETGs observation with the synthetic spectra of argon, we identify two weak emission lines, that is, the Ar XV 27.470 A line with transition 2s3p 1P1-2s2 1S0 and the Ar XVI 27.872 A line with transition 3d 2D3/2-2p 2P1/2, which blend with the N VII Lyα emission line. Several second-order spectral lines are also identified, one of which is the second-order Fe XVIII 14.534 A line with transition 2p4(3P)3d 2F5/2-2p5 2P3/2, which blends with the inter-combination line of He-like N VI. In order to study the effects of these new identified weak lines on the electron temperature and density, we diagnose the two parameters using the intensity ratio of triplets of the He-like N VI and that of resonance lines of H- and He-like N. In the literature, there is a discrepancy of the temperatures deduced from N VI from other He-like ions, such as C V and O VII. The discrepancy disappears after the contribution of these weak lines is taken into account.

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