izvcrao Изв. Крымск. Астрофиз. Обсерв. Izv. Krymsk. Astrofiz. Observ. Известия Крымской астрофизической обсерватории Izvestiya Krymskoi Astrofizicheskoi Observatorii 0367-8466 3034-4107 Киселев Н.Н., пос. Московский, Москва, РФ RU 355 Материалы конференции Сonference proceedings Investigation of physical conditions of the Fraunhofer lines formation in the solar photosphere Kovalchuk M.M. Hirnyak M.B. Astronomical Observatory of the Ivan Franko National University of Lviv, Kyrylo and Mephodiy str.,8, Lviv, Ukraine Astronomical Observatory of the Ivan Franko National University of Lviv, Kyrylo and Mephodiy str.,8, Lviv, Ukraine 01 07 2013 109 2 72 72 27 10 2017 Copyright (c) 2013 , Copyright (c) 2013 Kovalchuk M., Hirnyak M. 2013 , Kovalchuk M., Hirnyak M. Метаданные этой статьи доступны по лицензии Creative Commons «Attribution» («Атрибуция») 4.0 Всемирная. Авторское право и право на публикацию текстов, представленных в журнале  "Известия Крымской астрофизической обсерватории", сохраняются за авторами, при этом право первой публикации предоставляется журналу. Тексты могут свободно использоваться при условии правильного цитирования с указанием авторства в соответствии с лицензией Creative Commons «Attribution» («Атрибуция») 4.0 Всемирная. The metadata for this submission is licensed under a Creative Commons Attribution 4.0 International License. Copyright and publishing rights for texts published in Izvestiya Krymskoi Astrofizicheskoi Observatorii is retained by the authors, with first publication rights granted to the journal.Texts are free to use with proper attribution and link to the licensing (Creative Commons Attribution 4.0 International).

The quantitative investigation of physical conditions in the solar atmosphere is carried out. The basis for this investigation is a catalogue of profiles and equivalent widths of lines obtained by means of solution of the radiative transfer equation using observational lines of the Fraunhofer solar spectrum. The lines with different intensities and different excitation and ionization potentials are used for gaining information about different heights of the solar atmosphere. The agreement of theoretical profiles and equivalent widths with observational data gave possibility to find out mechanisms of formation of absorption lines, account influence of non-Local Thermodynamical Equilibrium effects, etc. The solar atmosphere model (VAL – 80) was used for calculations.