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tokens: by Werner, Rauch Kruk ( 2018 ) in the hot white dwarf in the peculiar binary nucleus of the planetary nebula EGB 6. Ar vii λ = 1065.55 spectral line is observed in ultraviolet spectra of hot PG 1159 and extremely hot helium rich white dwarfs (Werner, Rauch Kruk 2016 , 2017 ). Ar iii and Ar ii spectral lines are used in the determination of argon abundance in B-type star and subdwarf atmospheres (Heber Edelmann 2004 ; Blanchette et al. 2008 ; Lanz et al. 2008 ; Fossati et al. 2009 ). In our recent works, Hamdi et al. ( 2017 ) and Hamdi et al. ( 2018 ), we have reported Stark widths for 300 spectral lines of singly charged argon (Ar ii ). Our Stark widths were compared with experimental results and good agreements were found for most spectral lines. In order to complete the set of Stark broadening parameters of Ar ii spectral lines, we report here Stark shifts. Stark shifts are calculated using semiclassical perturbation approach (SCP) (Sahal-Bréchot 1969a , b ) and a set of atomic data is calculated using Hartree–Fock method with relativistic corrections (Cowan 1981 ). Our results are compared with experimental results for 100 spectral lines. Shifts by collisions with ionic perturbers are also taken into account. We also present results as a function of temperature for 161 spectral lines for collisions with electrons, protons, singly charged helium, and singly charged argon. In previous works (Hamdi et al. 2011 , 2013 , 2014 ), the same method was used and we have determined Stark broadening parameters for 114 spectral lines of Pb IV and 32 spectral lines of Ar iii . 2 THE IMPACT SEMICLASSICAL PERTURBATION METHOD A detailed description of this formalism with all the innovations is given in Sahal-Bréchot ( 1969a , b , 1974 , 1991 ), Fleurier, Sahal-Bréchot Chapelle ( 1977 ), Dimitrijević, Sahal-Bréchot Bommier ( 1991 ), Dimitrijević Sahal-Bréchot ( 1996 ), Sahal-Bréchot, Dimitrijević Ben Nessib ( 2014 ), and earlier papers. The profile F (ω) is Lorentzian for isolated lines: where i and f denote the initial and final states and E i and E f their corresponding energies and w is the half width. The shift ( d ) (in angular frequency units) of an electron-impact shifted spectral line can be expressed as: where N is the electron density, the Maxwellian velocity distribution function for electrons, denotes the impact parameter of the incoming electron. The phase shift due to the polarization potential ( r −4 ), is given in section 3 of chapter 2 in Sahal-Bréchot ( 1969a ) and R D is the Debye radius. The cut-off R 3 is described in section 1 of chapter 3 in Sahal-Bréchot ( 1969b ). Energy levels and oscillator strengths needed for SCP calculations of Stark shifts are obtained using Hartree–Fock method with relativistic corrections (HFR) (Cowan 1981 ). We use as for the width calculations an atomic model including 24 configurations: 3s 2 3p 5 ; 3s 2 3p 4 nl ( nl = 4p, 4f, 5p, 5f, 6p, 6f, 6h, 7p, 7f, 7h) (odd parity) and 3s 3p 6 ; 3s 2 3p 4 n ′ l ′ ( n