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The life and scientific and professional activities of Danilo Zulević (1937 - 1998), research fellow of the Belgrade Astronomical Observatory, are presented, followed by the Bibliography of his works, the list of bibliographical items wherein his name is mentioned and the list of his name’s citations in the Science Citation Index.

Using a semiclassical approach, we have calculated electron-, proton-, and He II-impact line widths and shifts for 52 Be III multiplets as a function of temperature and perturber density. The electron temperatures are 10,000 K 20,000 K; 50,000 K; 100,000 K 200,000K and 300,000 K and perturber densities are from 10(exp)11 cm(exp)-3 up to 10(exp)21 cm(exp)-3.

Using a semiclassical approach, we have calculated electron-, proton-, He II-, Mg II-, Si II- and Fe II-impact line widths and shifts for 10 Ne II and 6 Ne III multiplets as a function of temperature and perturber density. For Ne II temperatures are: 5,000 K; 10,000 K; 20,000 K; 30,000 K; 50,000 K and 100,000 K and perturber densities from 1015 cm-3 up to 1020 cm-3. For Ne III temperatures are: 20,000 K; 50,000 K; 100,000 K; 200,000 K; 300,000 K and 500,000 K and perturber densities from 1017 cm-3 up to 1021 cm-3. Perturbers selected here, are the main perturbers in solar and stellar atmospheres.

Electron-, proton-, and ionized helium-impact broadening parameter tables for 101 In II multiplets, are presented as a function of temperature for the perturber density of 1016cm-3. Calculations have been performed within the semiclassical perturbation approach.

The influence of gravitational microlensing on the X-ray spectral line profiles originated from a relativistic accretion disc has been studied. Using a disc model, we show that microlensing can induce noticeable changes in the line shapes when the Einstein ring radius associated with the microlens is of a size comparable to that of the accretion disc. Taking into account the relatively small size of the X-ray accretion disc, we found that compact objects (of about a Solar mass) which belong to the bulge of the host galaxy can produce significant changes in the X-ray line profile of AGN.

Electron-, proton-, and ionized helium-impact broadening parameter tables for neutral calcium spectral lines, have been presented as a function of the temperature and the perturber density. Calculations have been performed within the semiclassical perturbation approach.

In order to provide the Stark broadening data for ion lines from complex spectra, here we present calculated Stark widths and shifts for 37 Kr II lines. The calculations were performed by using the modified semiempirical approach. Also the obtained results have been compared with existing experimental and theoretical data.

Activities of Milan Nedeljković, the founder of Belgrade Astronomical Observatory and his published works are discussed. The Bibliography of his works, as well as a Bibliography of selected works on Milan Nedeljković, are enclosed.

Electron-, proton-, and ionized helium-impact broadening parameter tables for In II spectral lines, are presented as a function of the temperature and the perturber density. Calculations have been performed within the semiclassical perturbation approach.

The life and scientific, professional and other activities of Vasilije Oskanjan (1921-1989), one-time director of the Belgrade Astronomical Observatory, research fellow of the Belgrade and Byurakan Observatories, are presented, followed by the Bibliography of his works, the list of bibliographical items wherein his name is mentioned and the list of his name’s citations in the Science Citation Index in the period 1946 - July 1999.

By using the semiclassical perturbation approach, Stark broadening parameters due to the interaction with a selection of perturbers of interest for recently published experimental results for Li - like B III, C IV, N V and O VI 3s2S-3p2Po, and for Be - like B II, C III, N IV and O V 3s3S-3p3Po multiplets, have been calculated. The results are presented as a function of temperature for a perturber density of 1017cm−3. The influence of resonance contribution for B II, differences in Stark broadening parameters if we take oscillator strengths calculated within the Coulomb approximation or taken from TOP Database, and the influence of transitions with different parent terms, have been discussed as well.

Using a semiclassical approach, we have calculated electron−, proton− and He II−impact line widths and shifts for 32 Zn I multiplets as a function of temperature and perturber density.

Using a semiclassical approach, we have calculated electron−, proton−, and He III−impact line widths and shifts for 6 Kr VIII multiplets as a function of temperature and perturber density.

Using a semiclassical approach, we have calculated electron−, proton−, and He III−impact line widths and shifts for 9 Ar VIII transitions as a function of temperature and perturber density.

Using a semiclassical approach, we have calculated electron−, proton−, He II−, Mg II-, Si II- and Fe II-impact line widths and shifts for 189 Ca I multiplets as a function of temperature. Perturbers selected here, are the main perturbers in solar and stellar atmospheres.

Using the semiclassical perturbation formalism, we have calculated electron-, proton-, and ionized helium-impact line widths and shifts for six Au I lines as a function of temperature and perturber density. Electron-impact broadening parameters for eight Au II transitions have been calculated within the modified semiempirical approach.

Using a semiclassical approach, we have calculated electron−, proton−, and He III−impact line widths and shifts for 4 K VIII and 30 K IX multiplets as a function of temperature and perturber density.

The life and scientific, professional and other activities of professor Ivan Atanasijević (1919-1998), the founder of radio astronomy in Serbia, professor of the Belgrade and Nimegen University, are presented, followed by Bibliography of his works.

By using the semiclassical-perturbation formalism, we have calculated electron-, proton-, and He III-impact line widths and shifts for 4 Sc X, 10 Sc XI, 4 Ti XI and 27 Ti XII multiplets, significant for investigation and modeling of different plasmas in astrophysics and physics. For Sc X calculations have been performed within the temperature range from 200,000 K to 5,000,000 K, and for perturber densities 1019cm−3 - 1022cm−3. Stark broadening data for Sc XI are tabulated for temperatures from 500,000 K to 5,000,000 K, and perturber densities 1018cm−3 - 1022cm−3. For Ti XI calculations were performed within the temperature range from 500,000 K to 5,000,000 K, and perturber densities 1018cm−3 - 1022cm−3, while for Ti XII results are given for temperatures from 500,000 K to 6,000,000 K, and perturber densities 1018cm−3 - 1023cm−3.

Using a semiclassical approach, we have calculated electron-, proton-, and ionized helium-impact line widths and shifts for 20 In III multiplets for perturber densities 1014− 1020 cm−3 and 2 Tl III multiplets for perturber densities 1017 − 1020 cm−3, and temperatures T = 20,000 − 500,000 K, in both cases. We have calculated as well, electron-, proton-, and He III-impact line widths and shifts for 2 Pb IV multiplets, for perturber densities 1017− 1020 cm−3 and temperatures T = 50,000 − 1,000,000 K.

By using the semiclassical-perturbation formalism, we have calculated electron-, proton-, and He III-impact line widths and shifts for 14 O VII multiplets and 18 Mg XI multiplets, of importance for research, diagnostic and modeling of various astrophysical, laser produced, fusion and laboratory plasmas. For O VII calculations were performed for temperature range from 100,000 K to 2,000,000 K. and perturber densities (1017cm−3 - 1023cm−3. For Mg XI calculations were performed for temperature range from 500,000 K to 5,000,000 K. and perturber densities 1018cm−3 - 1024cm−3.

In this paper we present the electron-impact widths for 28 transitions of singly-, doubly-, and triply- ionized vanadium estimated by using the modified semiempirical method. The electron-impact widths have been estimated for the electron density of 1023m−3 and presented as a function of electron temperature.

Using a semiclassical approach, we have calculated electron−, proton−, and He III−impact line widths and shifts for 2 F VI and 10 Cl VII multiplets as a function of temperature and perturber density.

The life and scientific, professional and other activities of Nenad Dj. Janković (1911-1997), who worked on the history of astronomy, ethno astronomical research, popularization of astronomy and the development of amateur astronomy in Serbia, are presented, followed by Bibliography of his works and Bibliography of works where he is mentioned.

Using a semiclassical approach, we have calculated electron−, proton−, and He III−impact line widths and shifts for 57 Na X multiplets as a function of temperature (200 000 K - 5 000 000 K) and perturber density (1017cm−3 - 1024cm−3.