Abstract
The atmosphere of HD 40589 (A0Iab) supergiant star of A spectral class was studied using the model atmosphere and parallax methods. The effective temperatures (Teff) and surface of gravity (log g) were determined using a comparison of the observed and calculated values of the photometric quantities [c1], Q and the equivalent widths of the hydrogen Balmer lines and parallax. Based on the Fe II lines the microturbulent velocity and metallicity [Fe/H] were determined. Metallicity of the program star is close to the metallicity of the Sun. This shows that our program star and the Sun are formed from the interstellar medium of a similar metallicity.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
