Modeling of the Continuous Absorption of Electromagnetic Radiation in Dense Hydrogen Plasma by Mihajlov A. A., Sakan N. M., Srećković V. A., Vitel Y.

“…The results can be applied to the plasma of partially ionized layers of stellar atmospheres.…”
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2D MODELLING OF THE GAS FLOW STRUCTURE IN THE SYMBIOTIC STAR Z ANDROMEDAE by E. Yu. Kilpio

“…Since the mechanisms of gas acceleration in stellar atmospheres are not well studied, the parametric representation of gas accelerating force was used. …”
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DV AQUARII REVISITED by G. Polubek

“…Roche geometry of the binary system is assumed and a grid of the newest Kurucz models of stellar atmospheres is used in the calculations.…”
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Automated stellar spectra parameterisation for Gaia-RVS by Wyse R.F.G., Gilmore G., Hill V., Bijaoui A., de Laverny P., Recio-Blanco A., Kordopatis G., Ordenovic C.

“…Degeneracies in the stellar atmospheric parameters can pollute large spectroscopic surveys, introducing possible biases in the derived distances, kinematics and chemical abundances. …”
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NLTE CALCULATION FOR O II by S. A. Korotin

“…One result of our calculations is a number of useful relationships between the NLTE oxygen abundance, line equivalent width, and stellar atmospheric parameters.…”
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Stark Broadening of Zn III Spectral Lines by Milan S. Dimitrijević, Magdalena D. Christova

“…The obtained results have been used for the investigation of the influence of Stark broadening on Zn III spectral lines in stellar atmospheres and for the considerations of Stark width similarites within supermultiplets and transition arrays.…”
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Stark Widths of Ar II Spectral Lines in the Atmospheres of Subdwarf B Stars by Rafik Hamdi, Nabil Ben Nessib, Sylvie Sahal Bréchot, Milan S. Dimitrijević

“…Ar II spectral lines are observed in many kinds of stellar atmospheres such as the atmospheres of B-Type stars and subdwarf B stars. …”
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THE EFFECTIVE TEMPERATURE DETERMINATION OF O-B STARS BY H AND He RADIO RECOMBINATION LINES OBSERVATIONS by A. P. Tsivilev

“…Then, comparing this ratio with a prediction of model stellar atmospheres, the effective temperature and other stellar parameters are determined. …”
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Directly Deriving Parameters from SDSS Photometric Images by Fan Wu, Yude Bu, Mengmeng Zhang, Zhenping Yi, Meng Liu, Xiaoming Kong

“…Stellar atmospheric parameters (effective temperature, surface gravity, and metallicity) are fundamental for understanding the formation and evolution of stars and galaxies. …”
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LINE FORMATION IN SPECTRA OF X-RAY NOVAE by V. F. Suleimanov, V. V. Shimansky

“…Local (for given radius) disk atmospheres as model stellar atmospheres, heated due to external X-ray radiation are treated. …”
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Stark Broadening of Several Ne II, Ne III and O III Spectral Lines for the Stark-B Database by Dimitrijević Milan S., Kovačević Andjelka, Simić Zoran, Sahal-Bréchot Sylvie

“…In order to complete Stark broadening data for Ne II and O III lines, needed for analysis of stellar atmospheres, we determined the missing parameters for the broadening by collisions with protons and ionized helium for 15 Ne II and 5 O III multiplets. …”
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Understanding Sun-as-a-Star Variability of Solar Balmer Lines by S. Criscuoli, S. Marchenko, M. DeLand, D. Choudhary, G. Kopp

“…Precise, high-cadence, long-term records of stellar spectral variability at different temporal scales lead to better understanding of a wide variety of phenomena including stellar atmospheres and dynamos, convective motions, and rotational periods. …”
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AGB Stars and Their Circumstellar Envelopes: An Operative Approach to Computing Their Atmospheres by Lucio Crivellari, Sergio Cristallo, Luciano Piersanti

“…In this paper, we present an iterative sequential procedure, operative and physically sound, tailored to compute extended stellar atmospheres. It will constitute the backbone of the in fieri TEIDE package to be implemented into our VULCAN code. …”
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FBILI method for the two-level atom line formation in media with low velocity fields by Pirković I., Atanacković O.

“…In order to test the accuracy and the convergence properties of the method we solved several astrophysically important benchmark problems of the NLTE line formation: in a plan-parallel differentially expanding medium of finite thickness, and in spherically symmetric stellar atmospheres, both static and expanding. We compared our solutions with those obtained by other authors using different numerical methods. …”
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ON THE GF-VALUES FOR SOME DIATOMIC MOLECULAR SPECTRA by L. A. Kuznetsova, A. V. Shavrina

“…In view of rich structure of the energy levels and the variety of transition types which are observable, molecules are the useful tool for investigation of physical parameters of stellar atmospheres, interstellar and circumstellar matter. such as gas  density, its temperature, chemical and isotopic composition, ionization degree, radiation field density, kinematics, etc. …”
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Atomic diffusion in the atmosphere of Feige 86 by Németh Péter

“…Therefore, to advance our general understanding of diffusion in stellar atmospheres we urge for new ultraviolet spectroscopy of Feige 86 at the highest possible resolution with HST/STIS.…”
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Comparisons and Comments on Electron and Ion Impact Profiles of Spectral Lines by Sahal-Bréchot Sylvie, Dimitrijević Milan S., Nessib Nebil Ben

“…We also provide fitting formulae which are essential for the modeling codes of stellar atmospheres and envelopes.…”
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Stark broadening parameter tables for Ne II and Ne III spectral lines by Dimitrijević M.S.

“…Perturbers selected here, are the main perturbers in solar and stellar atmospheres.…”
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A New Analysis of Stark and Zeeman Effects on Hydrogen Lines in Magnetized DA White Dwarfs by Ny Kieu, Joël Rosato, Roland Stamm, Jelena Kovačević-Dojcinović, Milan S. Dimitrijević, Luka Č. Popović, Zoran Simić

“…We perform new calculations in conditions relevant to magnetized DA stellar atmospheres using models inspired from magnetic fusion plasma spectroscopy. …”
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SPECTRAL INVESTIGATIONS OF CM DRA by M. K. Kuznetsov, Y. V. Pavlenko, D. Pinfield, H. Jones

“…We refined the parameters (effective temperature, rotational velocity and metallicity) of the components of the system CM Dra using the method of stellar atmospheres. The data that we obtained are in good agreement with the results obtained by other authors. …”
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