Hyperfine Structure Constants For High Excited Levels Of Neutral And Singly Ionized Manganese

The study of the hyperfine interaction of atoms is an effective way to understand the structure and properties of the nucleus as well as the effect of electron correlation.The precise and reliable hyperfine structure(HFS)constant is helpful to solve some complex problems caused by the interaction between electrons outside the nucleus and nucleus.With the development of modern astronomical observation techniques such as large ground-based telescopes and space telescopes,people have been able to obtain a large number of high-resolution celestial spectra,which makes many features of the spectrum can be distinguished.In addition to the basic atomic data such as the wavelength of the spectral line and the oscillator strengths,the analysis of astrophysical spectra also requires data on the spectral line broadening effect,such as the Zeeman effect,isotope shift and HFS constant.In the analysis of stellar abundance and the determination of physical parameters in stellar atmosphere,HFS constant is an indispensable and important atomic data.In recent years,a lot of research has focused on HFS constants of the levels of iron peak elements.The abundance of manganese(Mn)in the sun is 5.42±0.04,ranking fourth among the iron peak elements.In some chemically peculiar stars(such as Hg Mn stars),the abundant of manganese is even more than iron.A large number of spectral data show that hyperfine interaction can significantly affect the measured values of spectral line width and wavelength,and the lack of reliable HFS data in the study will lead to large errors in the measurement results of element abundance and turbulence velocity.As far as we know,the HFS constants of 152 levels of neutral manganese(Mn I)and 110 levels of singly ionized manganese(Mn II)have been reported.For 550 levels of Mn I and 585 levels of Mn II levels known at the present stage,there are still many levels of HFS constants that have not been determined,especially for the high excited levels.In this paper,a spectral analysis program based on HFS theory and least square method was developed,and the Fourier transform(FT)spectra were analyzed and fitted by this program.These spectral data came from the archival files in the digital library of National Solar Observatory on Kitt Peak,USA(http://diglib.nso.edu/),which were recorded by the 1.0 m FT spectrometer with hollow cathode lamps.In total,158 spectral lines were analyzed and their profiles were fitted to present HFS constants for 42 levels of Mn I in the energy range between 24779.32 and 65946.59cm^-1and 35 levels of Mn II between 43131.51 and 114349.29 cm^-1,of which 37results for Mn I and 32 results for Mn II are reported for the first time,to our best knowledge.For four and six levels,which belong to Mn I and Mn II respectively,the measurements contain magnetic dipole and electric quadrupole constants(A and B constants),and for other levels only A constants were determined.Most of the estimated uncertainties are less than 10%.The HFS constant data determined in this paper can not only promote the development of atomic theory and improve the understanding of the internal structure and properties of atoms,but also contribute to the study of astrophysics and nuclear physics.