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Usual procedure of the Stark broadening theory usage for astrophysical purpose is to determine Stark width of particular spectral line with some theoretical calculation method, and then to compare measured spectral line with synthetic line simulated with Voight profile obtained by some spectral synthesis code and a proper model atmosphere code. We suggested here inverse approach – to determine Stark width from the best fitting of synthetic line with measured one. This method is applicable in the case when astrophysical spectrum of the object containing the isolated line we consider about is available, especially if we are not sure how much our calculation method is accurate. We tested the possibility of the use of this method in the example of Zr IV λ1184 line identified in Feige 87 spectrum. Stark width obtained in this way is compared with values estimated using the approximative formulae from Majlinger et al (2017). Finally we discussed influence of Stark broadening on abundance determination comparing our result of zirconium abundance determined from considering spectral line with some previously published results (Chayer et al, 2006, Pereira et al, 2006). References: Chayer, P., Fontaine, M., Fontaine, G., et al., 2006, Baltic Astron., 15, 131 Majlinger, Z. ; Dimitrijević, S. M. ; Simić, Z., 2017, Atoms, 5, 49 Pereira, C., Wesemael, F., Bergeron, P., 2006, Baltic Astron., 15, 123 |
