Ref: ASTROimport-247

Ultraviolet emission lines of Si II in cool star and solar spectra

Laha, S. ; Keenan, F. P. ; Ferland, G. J. ; Ramsbottom, C. A. ; Aggarwal, K. M. ; Ayres, T. R. ; Chatzikos, M. ; van Hoof, P. A. M. ; Williams, R. J. R.

published in Monthly Notices of the Royal Astronomical Society, 455, pp. 3405-3412 (2016)

Abstract: Recent atomic physics calculations for Si II are employed within the CLOUDY modelling code to analyse Hubble Space Telescope (HST) STIS ultraviolet spectra of three cool stars, ß Geminorum, a Centauri A and B, as well as previously published HST/GHRS observations of a Tau, plus solar quiet Sun data from the High Resolution Telescope and Spectrograph. Discrepancies found previously between theory and observation for line intensity ratios involving the 3s23p 2PJ-3s3p2 4P_{J^' }} intercombination multiplet of Si II at ˜ 2335 Å are significantly reduced, as are those for ratios containing the 3s23p 2PJ-3s3p2 2D_{J^' }} transitions at ˜1816 Å. This is primarily due to the effect of the new Si II transition probabilities. However, these atomic data are not only very different from previous calculations, but also show large disagreements with measurements, specifically those of Calamai et al. for the intercombination lines. New measurements of transition probabilities for Si II are hence urgently required to confirm (or otherwise) the accuracy of the recently calculated values. If the new calculations are confirmed, then a long-standing discrepancy between theory and observation will have finally been resolved. However, if the older measurements are found to be correct, then the agreement between theory and observation is simply a coincidence and the existing discrepancies remain.

DOI: 10.1093/mnras/stv2566
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The record appears in these collections:
Royal Observatory of Belgium > Astronomy & Astrophysics
Science Articles > Peer Reviewed Articles

 Record created 2016-07-01, last modified 2016-07-01