Abstract
Some problems of the determination of the microturbulent velocities and abundances in atmospheres of the F-G-K stars and determination of their effective temperatures and rotational velocities in the framework of self-consistent approach are discussed. Firstly, we use independent determinations of iron abundances. using the fits to the observed profiles of Fe I and Fe II absorption lines. Secondly, abundances of other elements are determined for the found input parameters.
Highlights
Recent progress and advance of astrophysical hardware, especially high resolution echelle spectrographs and sophisticated algorithms of the reduction of the experimental data the study push us to the high precision investigation of the essential physical parameters of atmospheres of solar-like stars
And hereafter we use the terminology “the fine analysis” to define a special kind of the investigations based on the comparison of observed and computed profiles of spectral lines in stellar spectra
Detailed studies of the hosting star can attain benchmark status by detailed study of the properties of the primary, and evolutionary and bulk characteristics can be inferred for the companion
Summary
Recent progress and advance of astrophysical hardware, especially high resolution echelle spectrographs and sophisticated algorithms of the reduction of the experimental data the study push us to the high precision investigation of the essential physical parameters of atmospheres of solar-like stars. From other hand to model their spectra some sophisticated procedures and algorithms of the “fine analysis” pf observed spectra were developed (see [16], [8], [9]). We note the remarkable progress in obtaining more precise basic physical parameters from the latest evolutionary models (see [7], [1], [13]). In some cases only in that way we can obtain the information about the status of companions, whether they are brown dwarf or planetary
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