Confronting atomic data with Fe L-shell spectra of stellar coronae

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dc.creatorBehar, E.
dc.creatorCottam, J.
dc.creatorPeterson, J. R.
dc.creatorSako, M.
dc.creatorKahn, S. M.
dc.creatorBar-Shalom, A.
dc.creatorKlapisch, M.
dc.creatorBrinkman, A. C.
dc.date2001-06-25
dc.date.accessioned2026-07-07T01:59:03Z
dc.date.available2026-07-07T01:59:03Z
dc.descriptionIt is common to suggest the uncertainties in the atomic data for explaining difficulties that arise in interpreting astrophysical x-ray spectra. The atomic data for the Fe L-shell ions have, over the years, been considered particularly suspect. In this paper, we confront Fe-L spectra calculated using the HULLAC atomic code assuming coronal conditions with recent observations of the stellar coronae of Capella and HR 1099, obtained with the high-resolution grating spectrometers on board Chandra and XMM-Newton. We find very good agreement, which indicates that Fe-L transition rates calculated with state-of-the-art codes, can generally be trusted in the analysis of x-ray spectra.
dc.descriptionSubmitted for the proceedings of "X-ray astronomy 2000",(Palermo Sep. 2000), Eds. R. Giacconi, L. Stella, S. Serio, ASP Conf. Series
dc.identifierhttps://arxiv.org/abs/astro-ph/0106448
dc.identifierhttp://arxiv.org/abs/astro-ph/0106448
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/2959
dc.subjectAstrophysics
dc.titleConfronting atomic data with Fe L-shell spectra of stellar coronae
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