Variations of the Ha line in the spectra of the star HD14134 are investigated using ob- servations carried out in 2013-2014 and in 2016 with the 2-m telescope at Shamakhy Astrophysical Observatory. In the spectra of t...Variations of the Ha line in the spectra of the star HD14134 are investigated using ob- servations carried out in 2013-2014 and in 2016 with the 2-m telescope at Shamakhy Astrophysical Observatory. In the spectra of this star, the absorption and emission components of Hα are found to disappear and an inverse P Cyg profile of Ha is seen on some observational epochs. Our observations showed that when the Ha line disappeared or an inversion of the P-Cyg-type profile is observed in the spectra, the Hβ line is redshifted. When these events appeared, no synchronous variabilities were ob- served in the spectral parameters of other spectral lines formed in deeper atmospheric layers. In addition, the structures of Ha, CII （6578.05A, 6582.88A）, Sill （6347.1 A, 6371.36A） and Hβ lines are variable on a timescale of hours, but we did not detect significant variations in the other photospheric lines, as well as in the HeI （5875.72A） line. It is suggested that observational evidence for the non-stationary atmosphere of HD 14134 can be associated in part with non-spherical stellar wind.展开更多
基金supported by the scientific program for priority fields of research of the National Academy of Sciences of Azerbaijan
文摘Variations of the Ha line in the spectra of the star HD14134 are investigated using ob- servations carried out in 2013-2014 and in 2016 with the 2-m telescope at Shamakhy Astrophysical Observatory. In the spectra of this star, the absorption and emission components of Hα are found to disappear and an inverse P Cyg profile of Ha is seen on some observational epochs. Our observations showed that when the Ha line disappeared or an inversion of the P-Cyg-type profile is observed in the spectra, the Hβ line is redshifted. When these events appeared, no synchronous variabilities were ob- served in the spectral parameters of other spectral lines formed in deeper atmospheric layers. In addition, the structures of Ha, CII （6578.05A, 6582.88A）, Sill （6347.1 A, 6371.36A） and Hβ lines are variable on a timescale of hours, but we did not detect significant variations in the other photospheric lines, as well as in the HeI （5875.72A） line. It is suggested that observational evidence for the non-stationary atmosphere of HD 14134 can be associated in part with non-spherical stellar wind.
