On Correlation Of Microturbulence And The Line Depth Of S II Line Profile In Iota Herculis

摘要

In this paper, we discuss about the correlation between microturbulence and the fluctuations of central depth of S II line profile of iota Herculis a B3 IV star, based on 144 spectra from the ELODIE archive data (May 17 to 21,1995) and 47 spectra from the archive data of Ritter Observatory （February 6,1994 to October 30,1995). The variations of central depth of S II line profile of this star are analyzed using the IRAF software, and the evaluations of microturbulence are determined by using the important equation of the full width at half-maximum (FWHM) of the line profile for Doppler broadening. From both datasets,we found that there is a connection between the variations of central depth of S II line profile and the microturbulence of iota Herculis. The central depth of S Ⅱ line profile becomes deeper when the microturbulent velocity increases and vice versa. We propose the connection between microturbulence and the fluctuations of central depth of S II line profile in this star is due to the sub-photospheric iron convection zones (FeCZ) which have the connection with the origin of microturbulence phenomenon, stellar temperature and the opacity of this star