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 Angstrom line with transition 2s3p P-1(1) - 2s(2) S-1(0) and the Ar XVI 27.872 Angstrom line with transition 3d D-2(3/2) - 2p P-2(1/2), which blend with the N VII Lyalpha emission line. Several second-order spectral lines are also identified, one of which is the second-order Fe XVIII 14.534 Angstrom line with transition 2p(4)(P-3)3d F-2(5/2) - 2p(5) P-2(3/2), which blends with the inter-combination line of He-like N VI. hi 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 W and that of resonance lines of H- and He-like N. In the literature, there is a discrepancy of the temperatures deduced from N W 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.
1.Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China 2.Natl Univ Def Technol, Dept Appl Phys, Changsha 410073, Peoples R China
Liang, GY,Zhao, G,Shi, JR,et al. Identification of three weak lines and their influences on diagnostics of electron temperature and density in astrophysical plasmas[J]. CHINESE PHYSICS LETTERS,2004,21(10):2063-2066.