000002090 001__ 2090
000002090 005__ 20160701171658.0
000002090 0247_ $$2DOI$$a10.1093/mnras/stv2566
000002090 037__ $$aASTROimport-247
000002090 100__ $$aLaha, S.
000002090 245__ $$aUltraviolet emission lines of Si II in cool star and solar spectra
000002090 260__ $$c2016
000002090 520__ $$aRecent atomic physics calculations for Si II are employed within the CLOUDY modelling code to analyse Hubble Space Telescope (HST) STIS ultraviolet spectra of three cool stars, ß Geminorum, a Centauri A and B, as well as previously published HST/GHRS observations of a Tau, plus solar quiet Sun data from the High Resolution Telescope and Spectrograph. Discrepancies found previously between theory and observation for line intensity ratios involving the 3s23p 2PJ-3s3p2 4P_{J^' }} intercombination multiplet of Si II at ˜ 2335 Å are significantly reduced, as are those for ratios containing the 3s23p 2PJ-3s3p2 2D_{J^' }} transitions at ˜1816 Å. This is primarily due to the effect of the new Si II transition probabilities. However, these atomic data are not only very different from previous calculations, but also show large disagreements with measurements, specifically those of Calamai et al. for the intercombination lines. New measurements of transition probabilities for Si II are hence urgently required to confirm (or otherwise) the accuracy of the recently calculated values. If the new calculations are confirmed, then a long-standing discrepancy between theory and observation will have finally been resolved. However, if the older measurements are found to be correct, then the agreement between theory and observation is simply a coincidence and the existing discrepancies remain. 
000002090 700__ $$a Keenan, F. P.
000002090 700__ $$a Ferland, G. J.
000002090 700__ $$a Ramsbottom, C. A.
000002090 700__ $$a Aggarwal, K. M.
000002090 700__ $$a Ayres, T. R.
000002090 700__ $$a Chatzikos, M.
000002090 700__ $$a van Hoof, P. A. M.
000002090 700__ $$a Williams, R. J. R.
000002090 773__ $$c3405-3412$$i3$$pMonthly Notices of the Royal Astronomical Society$$v455$$y2016
000002090 85642 $$ahttp://esoads.eso.org/abs/2016MNRAS.455.3405L
000002090 905__ $$apublished in
000002090 980__ $$aREFERD