J/A+AS/133/227 J/A+AS/133/227 Stark broadening of K VIII and K IX M S Dimitrijevic S Sahal-Brechot Astron. Astrophys. Suppl. Ser. 133 227 1998 1998A&AS..133..227D VI/82 : Stark broadening of H lines J/A+AS/105/243 : Stark broadening of BeI lines J/A+AS/105/245 : Stark broadening of Al XI and Si XII J/A+AS/107/349 : Stark broadening of Ne VIII and Na IX J/A+AS/109/551 : Stark broadening of OIV and OV J/A+AS/115/351 : Stark broadening of C V and P V J/A+AS/116/359 : Stark broadening of Xe II lines J/A+AS/117/127 : Stark broadening of solar Mg I lines J/A+AS/119/369 : Stark broadening of Be III and B III J/A+AS/119/529 : Stark broadening of Sr I spectral lines J/A+AS/120/373 : Stark width in Sc II, Y II and Zr II spectra J/A+AS/122/163 : Stark broadening of Ba I and Ba II lines J/A+AS/122/533 : Stark broadening of P IV spectral lines J/A+AS/127/295 : Stark broadening of Kr II lines J/A+AS/127/543 : Stark broadening of S V lines J/A+AS/128/203 : Stark broadening of Mn, Ga & Ge multiplets J/A+AS/128/359 : Stark broadening of Ca IX and Ca X lines J/A+AS/129/155 : Stark broadening of Si XI and Si XIII lines J/A+AS/130/539 : Stark broadening of Na X Atomic physics atomic data line: profiles By using the semiclassical-perturbation formalism, we have calculated electron-, proton-, and He III-impact line widths and shifts for 4 K VIII and 30 K IX multiplets, of interest for analysis, investigation and modeling of different plasmas in solar and stellar subphotospheric layers research and plasma physics. The obtained results are presented as a function of temperature and perturber density. Results are compared with other theoretical estimates, based on regularities and systematic trends.

N Perturber density cm-3 El Element --- Tr Transition --- lambda Wavelength 0.1nm C Parameter C number=1 C/FWHM gives an estimate of the maximum perturber density for which the line may be treated as isolated and tabulated data may be used 0.1nm/cm3 T Temperature K n_We Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- We FWHM for electron impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_de Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- de shift for electron impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm n_Wp Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- Wp FWHM for proton impacts (2) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_dp Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dp shift for proton impacts (3) number=5 Values for NV>0.5 are not given, because in this case the impact approximation is no longer valid 0.1nm n_WHe++ Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- WHe++ FWHM for He III-impacts number=2 FWHM denotes Full Width at Half Maximum 0.1nm n_dHe++ Validity flag number=4 An asterisk in this column indicates that 0.1<NV<0.5, (V=collision volume); beware of the fact that the limit of validity of the impact approximation is attained for the value that follows --- dHe++ shift for He III-impacts number=3 A positive (resp. negative) shift is towards the red (resp. blue) 0.1nm Patricia Bauer CDS 1998Jun08Dr Milan Dimitrijevic <mdimitrijevic@aob.bg.ac.yu> J_A+AS_133_227.xml