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21 results on '"Astronomical Observatory Belgrade (AOB)"'

1. Atomic structure for carbon-like ions from Na vi to Ar xiii

Author

N. Ben Nessib, Abeer Al-Modlej, Milan S. Dimitrijević, H Alrashed, King Saud University [Riyadh] (KSU), Institut National des Sciences Appliquées et de Technologie [Tunis] (INSAT), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), and Astronomical Observatory Belgrade (AOB)

Subjects
Sun: flares, atomic processes, 7. Clean energy, 01 natural sciences, Ion, Ionization, 0103 physical sciences, atomic data, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Physics, [PHYS]Physics [physics], Solar flare, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Sun: corona, Astronomy and Astrophysics, Plasma, Sun: UV radiation, gamma rays, Stars, Space and Planetary Science, NIST, Plasma diagnostics, Atomic physics, Sun: X-rays
Abstract

We have calculated the energy levels, oscillator strengths, and transition probabilities for eight carbon-like ions (Na vi, Mg vii, Al viii, Si ix, P x, S xi, Cl xii and Ar xiii) using the Hartree–Fock pseudo-relativistic (HFR) and Thomas–Fermi–Dirac–Amaldi (TFDA) approaches. We used configuration expansions containing eight configurations, namely 2s2 2p2, 2s 2p3, 2s2 2p 3s, 2s2 2p 3p, 2s2 2p 3d, 2s2 2p 4s, 2s2 2p 4p, and 2s2 2p 5s. For each of the considered ions we obtained 59 energy levels, a number of which are not in the National Institute of Standards and Technology (NIST) data base. We compared our results with critically selected experimental data from NIST and with calculations made using the multiconfiguration Hartree–Fock (MCHF) method. We calculated weighted oscillator strengths and transition probabilities using two methods (HFR and TFDA) for the 2s2 2p2 and 2s 2p3 configurations for the eight C-like ions considered here. We analysed the atomic structure parameter trends, which allowed us to find missing data belonging to an isoelectronic sequence. The energy levels, oscillator strengths, and transition probabilities calculated here are in good agreement with the data from the NIST data base. Because emission and absorption features from C-like ions are often used for density and temperature diagnostics of various plasmas in astrophysics, and in studies of the solar corona, including solar flares, and of the coronae of other stars and of ionized outflows in active galactic nuclei etc., the obtained data will be useful for improving plasma diagnostics and modelling, in particular for the X-ray Universe.

Published
2021
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2. The role of some collisional processes in AGNs: Rate coefficients needed for modeling

Author

Vladimir A. Srećković, Lj. M. Ignjatović, Bratislav P. Marinković, Milan S. Dimitrijević, Astronomical Observatory Belgrade (AOB), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institute of Physics [Belgrade], and University of Belgrade [Belgrade]

Subjects
Work (thermodynamics), Hydrogen, Astrophysics::High Energy Astrophysical Phenomena, chemistry.chemical_element, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Molecular processes, symbols.namesake, 0103 physical sciences, Atom, Physics::Atomic Physics, 010303 astronomy & astrophysics, Instrumentation, Atomic data, Astrophysics::Galaxy Astrophysics, Galaxies: nuclei, Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Molecular data, Balmer series, Astronomy and Astrophysics, Atomic processes, Galaxies: active, Effective temperature, chemistry, 13. Climate action, Space and Planetary Science, Rydberg formula, symbols, Astrophysical plasma, Stars: atmospheres, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Recombination
Abstract

International audience; The importance of some atom hydrogen collisions in AGN has been investigated. The results are useful for better estimation of the hydrogen Balmer lines fluxes, which usage for effective temperature diagnostics in astrophysical plasma is limited by errors from the line formation models. The data could be also useful for modeling cooler and denser parts of AGN BLR clouds, as well as for the investigation of Rydberg states of hydrogen and for the study of their influence during the cosmological recombination epoch. The results of the present work suggest that the investigated processes are of interest for the research and modeling of such media.

Published
2021
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3. The supernova remnant population of the Small Magellanic Cloud

Author

Jean Ballet, Patrick J. Kavanagh, Milorad Stupar, Frank Haberl, Chandreyee Maitra, P. Maggi, Branislav Vukotić, Miroslav Filipovic, Manami Sasaki, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Western Sydney University, Astronomical Observatory Belgrade (AOB), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Extraterrestrische Physik (MPE), School of Cosmic Physics [Dublin], Dublin Institute for Advanced Studies (DIAS), Dr. Karl-Remeis-Sternwarte, Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU)-Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), School of Science and Health [Western Sydney University], Western Sydney University (UWS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ISM: abundances, supernovae: general, 0103 physical sciences, Magellanic Clouds, Astrophysics::Solar and Stellar Astrophysics, education, Large Magellanic Cloud, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, X-rays: ISM, Interstellar medium, Supernova, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Small Magellanic Cloud, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Aims: We present a comprehensive study of the supernova remnant (SNR) population of the Small Magellanic Cloud (SMC). We measure multiwavelength properties of the SMC SNRs and compare them to those of the Large Magellanic Cloud (LMC) population. Methods: This study combines the large dataset of XMM-Newton observations of the SMC, archival and recent radio continuum observations, an optical line emission survey, and new optical spectroscopic observations. We can thus build a complete and clean sample of 19 confirmed and 4 candidate SNRs. The homogeneous X-ray spectral analysis allows to search for SN ejecta and Fe K line emission, and to measure interstellar medium (ISM) abundances. We estimate the ratio of core-collapse to type Ia supernova rates of the SMC based on the X-ray properties and the local stellar environment of each SNR. Results : After the removal of unconfirmed or misclassified objects, and the addition of two newly confirmed SNRs based on multi-wavelength features, we present a final list of 21 confirmed SNRs and 2 candidates. While no Fe K line is detected even for the brightest and youngest SNR, we find X-ray evidence of SN ejecta in 11 SNRs. We estimate a ratio of 4.7$_{-1.9} ^{+0.6}$ core-collapse supernova to every type Ia SN, three times higher than in the LMC. The difference can be ascribed to the absence of the enhanced star formation episode in the SMC, which occurred in the LMC 0.5-1.5 Gyr ago. The hot-gas abundances of O, Ne, Mg, and Fe are 0.1-0.2 times solar. Their ratios with respect to SMC stellar abundances reflect the effects of dust depletion and partial dust destruction in SNR shocks. We find evidence that the ambient medium probed by SMC SNRs is less disturbed and less dense on average than in the LMC, consistent with the different morphologies of the two galaxies., Comment: Submitted to Astronomy & Astrophysics. 29 pages, 8 figures, 5 tables; 3 additional tables and 9 figures in Appendices

Published
2019
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4. X-CIGALE: Fitting AGN/galaxy SEDs from X-ray to infrared

Author

Yang, G, Boquien, M., Buat, V., Burgarella, D., Ciesla, L., Duras, F, Stalevski, M, Brandt, W, Papovich, C., Texas A&M University System, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astronomical Observatory Belgrade (AOB), Pennsylvania State University (Penn State), and Penn State System

Subjects
quasars:general, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], methods: observational, galaxies: nuclei, X-rays: general, methods: data analysis
Abstract

International audience; CIGALE is a powerful multiwavelength spectral energy distribution (SED) fitting code for extragalactic studies. However, the current version of CIGALE is not able to fit X-ray data, which often provide unique insights into AGN intrinsic power. We develop a new X-ray module for CIGALE, allowing it to fit SEDs from the X-ray to infrared (IR). We also improve the AGN fitting of CIGALE from UV-to-IR wavelengths. We implement a modern clumpy two-phase torus model, SKIRTOR. To account for moderately extincted type 1 AGNs, we implement polar-dust extinction. We publicly release the source code (named "X-CIGALE"). We test X-CIGALE with X-ray detected AGNs in SDSS, COSMOS, and AKARI-NEP. The fitting quality (as indicated by reduced χ 2) is good in general, indicating that X-CIGALE is capable of modelling the observed SED from X-ray to IR. We discuss constrainability and degeneracy of model parameters in the fitting of AKARI-NEP, for which excellent mid-IR photometric coverage is available. We also test fitting a sample of AKARI-NEP galaxies for which only X-ray upper limits are available from Chandra observations, and find that the upper limit can effectively constrain the AGN SED contribution for some systems. Finally, using X-CIGALE, we assess the ability of Athena to constrain the AGN activity in future extragalactic studies.; CIGALE est un code d'ajustement puissant pour la distribution d'énergie spectrale multi-longueur d'onde (SED) destiné aux études extragalactiques. Cependant, la version actuelle de CIGALE n’est pas en mesure d’adapter les données de rayons X, qui fournissent souvent des informations uniques sur la puissance intrinsèque d’AGN. Nous développons un nouveau module de rayons X pour CIGALE, lui permettant de modéliser les SED des rayons X à l’infrarouge (IR). Nous améliorons également l'ajustement AGN de ​​CIGALE des longueurs d'onde UV à IR. Nous utilisons un modèle de tore à deux phases : SKIRTOR. Pour prendre en compte les AGN de ​​type 1 moyennement éteints, nous mettons en œuvre l'extinction des poussières polaires. Nous publions publiquement le code source (nommé "X-CIGALE"). Nous testons X-CIGALE avec des AGN détectés par rayons X dans SDSS, COSMOS et AKARI-NEP. La qualité d'ajustement (indiquée par la réduction de χ 2) est généralement bonne, ce qui indique que X-CIGALE est capable de modéliser le SED observé des rayons X à l'infrarouge. Nous discutons de la constrainabilité et de la dégénérescence des paramètres du modèle lors de l'ajustement d'AKARI-NEP, pour lequel une excellente couverture photométrique en IR moyen est disponible. Nous testons également l'ajustement d'un échantillon de galaxies AKARI-NEP pour lesquelles seules les limites supérieures aux rayons X sont disponibles à partir des observations de Chandra, et nous constatons que la limite supérieure peut effectivement limiter la contribution du SED d'AGN pour certains systèmes. Enfin, à l’aide de X-CIGALE, nous évaluons la capacité d’Athéna à limiter l’activité d’AGN dans de futures études extragalactiques.

Published
2019

5. X-CIGALE: Fitting AGN/galaxy SEDs from X-ray to infrared

Author

Marko Stalevski, F. Duras, Casey Papovich, Médéric Boquien, Guang Yang, Denis Burgarella, Laure Ciesla, W. N. Brandt, V. Buat, Texas A&M University System, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astronomical Observatory Belgrade (AOB), Pennsylvania State University (Penn State), Penn State System, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Burgarella, Denis

Subjects
Infrared, Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), FOS: Physical sciences, Model parameters, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: general, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), quasars:general, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Torus, Astrophysics - Astrophysics of Galaxies, Methods observational, methods: data analysis, Galaxy, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, methods: observational, galaxies: nuclei, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

CIGALE is a powerful multiwavelength spectral energy distribution (SED) fitting code for extragalactic studies. However, the current version of CIGALE is not able to fit X-ray data, which often provide unique insights into AGN intrinsic power. We develop a new X-ray module for CIGALE, allowing it to fit SEDs from the X-ray to infrared (IR). We also improve the AGN fitting of CIGALE from UV-to-IR wavelengths. We implement a modern clumpy two-phase torus model, SKIRTOR. To account for moderately extincted type 1 AGNs, we implement polar-dust extinction. We publicly release the source code (named "X-CIGALE"). We test X-CIGALE with X-ray detected AGNs in SDSS, COSMOS, and AKARI-NEP. The fitting quality (as indicated by reduced χ 2) is good in general, indicating that X-CIGALE is capable of modelling the observed SED from X-ray to IR. We discuss constrainability and degeneracy of model parameters in the fitting of AKARI-NEP, for which excellent mid-IR photometric coverage is available. We also test fitting a sample of AKARI-NEP galaxies for which only X-ray upper limits are available from Chandra observations, and find that the upper limit can effectively constrain the AGN SED contribution for some systems. Finally, using X-CIGALE, we assess the ability of Athena to constrain the AGN activity in future extragalactic studies., CIGALE est un code d'ajustement puissant pour la distribution d'énergie spectrale multi-longueur d'onde (SED) destiné aux études extragalactiques. Cependant, la version actuelle de CIGALE n’est pas en mesure d’adapter les données de rayons X, qui fournissent souvent des informations uniques sur la puissance intrinsèque d’AGN. Nous développons un nouveau module de rayons X pour CIGALE, lui permettant de modéliser les SED des rayons X à l’infrarouge (IR). Nous améliorons également l'ajustement AGN de ​​CIGALE des longueurs d'onde UV à IR. Nous utilisons un modèle de tore à deux phases : SKIRTOR. Pour prendre en compte les AGN de ​​type 1 moyennement éteints, nous mettons en œuvre l'extinction des poussières polaires. Nous publions publiquement le code source (nommé "X-CIGALE"). Nous testons X-CIGALE avec des AGN détectés par rayons X dans SDSS, COSMOS et AKARI-NEP. La qualité d'ajustement (indiquée par la réduction de χ 2) est généralement bonne, ce qui indique que X-CIGALE est capable de modéliser le SED observé des rayons X à l'infrarouge. Nous discutons de la constrainabilité et de la dégénérescence des paramètres du modèle lors de l'ajustement d'AKARI-NEP, pour lequel une excellente couverture photométrique en IR moyen est disponible. Nous testons également l'ajustement d'un échantillon de galaxies AKARI-NEP pour lesquelles seules les limites supérieures aux rayons X sont disponibles à partir des observations de Chandra, et nous constatons que la limite supérieure peut effectivement limiter la contribution du SED d'AGN pour certains systèmes. Enfin, à l’aide de X-CIGALE, nous évaluons la capacité d’Athéna à limiter l’activité d’AGN dans de futures études extragalactiques.

Published
2019
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6. Study of the 777 nm Lines Profile of Atomic Oxygen Using Laser-Induced Plasmas

Author

Favre, Aurélien, Dimitrijevic, Milan, Morel, Vincent, Djurovic, Stevica, Mijatovic, Zoran, Godard, Gilles, Bultel, Arnaud, Complexe de recherche interprofessionnel en aérothermochimie (CORIA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences appliquées Rouen Normandie (INSA Rouen Normandie), Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Institut National des Sciences Appliquées (INSA)-Normandie Université (NU)-Université de Rouen Normandie (UNIROUEN), Normandie Université (NU), Astronomical Observatory Belgrade (AOB), Department of Physics [Novi Sad], University of Novi Sad, and FAVRE, AURELIEN

Subjects
[PHYS]Physics [physics], [PHYS.PHYS.PHYS-ATOM-PH]Physics [physics]/Physics [physics]/Atomic Physics [physics.atom-ph], [SPI.FLUID]Engineering Sciences [physics]/Reactive fluid environment, [SPI.FLUID] Engineering Sciences [physics]/Reactive fluid environment, [PHYS.PHYS.PHYS-ATOM-PH] Physics [physics]/Physics [physics]/Atomic Physics [physics.atom-ph], ComputingMilieux_MISCELLANEOUS, [PHYS] Physics [physics]
Abstract

International audience

Published
2019

7. Differential interferometry of the rapid rotator Regulus

Author

Romain Petrov, M. Hadjara, S. Jankov, Stephane Lagarde, Alain Spang, Pierre Cruzalèbes, Universidad Católica del Norte [Antofagasta], Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherches en Astronomie, Astrophysique, et Géophysique [Algeria], Astronomical Observatory Belgrade (AOB), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, and Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Order (ring theory), FOS: Physical sciences, Astronomy and Astrophysics, Radius, Position angle, Lambda, 01 natural sciences, Spectral line, Flattening, 3. Good health, Computational physics, 010309 optics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectral resolution, Gravity darkening, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS
Abstract

We analyse interferometric data obtained for Regulus with AMBER (Astronomical Multi- BEam combineR) at high spectral resolution ($\lambda/\delta\lambda \approx 12000$) across the Br$\gamma$ spectral line. The study of the photocentre displacement allows us to constrain a large number of stellar parameters -- equatorial radius $R_{\rm eq}$, equatorial velocity $V_{\rm eq}$, inclination $i$, rotation-axis position angle $PA_{\rm rot}$, and flattening -- with an estimation of gravity-darkening coefficient $\beta$ using previously published theoretical results. We use the Simulation Code of Interferometric-observations for ROtators and CirCumstellar Objects (SCIROCCO), a semi-analytical algorithm dedicated to fast rotators. We chose Regulus because it is a very well-known edge-on star, for which an alternative approach is needed to check the previously published results. Our analysis showed that a significant degeneracy of solution is present. By confronting the results obtained by differential interferometry with those obtained by conventional long-base interferometry, we obtain similar results (within the uncertainties), thereby validating our approach, where $V_{eq}$ and $i$ are found separately. From the photocentre displacement, we can independently deduce $PA_{rot}$. We use two minimization methods to restrict observed stellar parameters via a fast rotator model: a non-stochastic method ($\chi^2$ fit) and a stochastic one (Markov Chain Monte Carlo method), in order to check whether the correct global minimum is achieved particularly with respect to the degeneracies of the gravity darkening parameter $\beta$, where we demonstrate, using a quantitative analysis of parameters, that the estimate of $\beta$ is easier for stars with an inclination angle of around $45^\circ$., Comment: 16 pages, 11 figures, MNRAS article

Published
2018
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8. Regulus observed with VLTI/AMBER

Author

Jankov, S., Hadjara, M., Romain Petrov, Cruzalèbes, P., Spang, A., Lagarde, S., Astronomical Observatory Belgrade (AOB), Universidad Católica del Norte [Antofagasta], Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre de Recherches en Astronomie, Astrophysique, et Géophysique [Algeria], Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Astrophysics - Solar and Stellar Astrophysics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS
Abstract

The rapidly rotating primary component of Regulus A system has been observed, for the first time, using the technique of differential interferometry at high spectral resolution. The observations have been performed across the Br$_\gamma$ spectral line with the VLTI/AMBER focal instrument in high spectral resolution mode (R $\approx$ 12000) at $\approx$ 80-130m (projected on the sky) Auxiliary Telescopes triplet baseline configurations. We confirm, within the uncertainties, the results previously obtained using the techniques of classical long-baseline interferometry, although the question of anomalous gravity darkening remains open for the future study.

Published
2018

9. Stark Broadening of Se IV, Sn IV, Sb IV and Te IV Spectral Lines

Author

C. Yubero, Zoran Simić, Joël Rosato, Milan S. Dimitrijević, Roland Stamm, Nenad Milovanović, Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), and Astronomical Observatory Belgrade (AOB)

Subjects
Nuclear and High Energy Physics, Stark broadening, 01 natural sciences, Spectral line, law.invention, Physics::Geophysics, symbols.namesake, law, 0103 physical sciences, atomic data, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, Physics::Atomic Physics, 010306 general physics, line profiles, 010303 astronomy & astrophysics, Line profiles, Atomic data, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], Resolution (electron density), Plasma, Condensed Matter Physics, Laser, Line width, Atomic and Molecular Physics, and Optics, Stark effect, symbols, lcsh:QC770-798, Atomic physics
Abstract

International audience; Stark broadening parameters, line width and shift, are needed for investigations, analysis and modelling of astrophysical, laboratory, laser produced and technological plasmas. Especially in astrophysics, due to constantly increasing resolution of satellite borne spectrographs, and large terrestrial telescopes, data on trace elements, which were previously insignificant, now have increasing importance. Using the modified semiempirical method of Dimitrijević and Konjević, here, Stark widths have been calculated for 2 Se IV, 6 Sn IV, 2 Sb IV and 1 Te IV transitions. Results have been compared with existing theoretical data for Sn IV. Obtained results will be implemented in the STARK-B database, which is also a part of Virtual atomic and molecular data center (VAMDC).

Published
2018
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10. Stark-Zeeman Line Shape Modeling for Magnetic White Dwarf and Tokamak Edge Plasmas: Common Challenges

Author

Yannick Marandet, N. Kieu, M. Koubiti, Joël Rosato, Roland Stamm, Zoran Simić, Milan S. Dimitrijević, I. Hannachi, Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), and Astronomical Observatory Belgrade (AOB)

Subjects
Nuclear and High Energy Physics, Tokamak, Stark broadening, 01 natural sciences, Spectral line, line shapes, 010305 fluids & plasmas, law.invention, symbols.namesake, Zeeman effect, tokamaks, white dwarfs, law, [PHYS.PHYS.PHYS-PLASM-PH]Physics [physics]/Physics [physics]/Plasma Physics [physics.plasm-ph], Physics::Plasma Physics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, Physics::Atomic Physics, 010306 general physics, ComputingMilieux_MISCELLANEOUS, Line (formation), Physics, [PHYS]Physics [physics], [PHYS.PHYS.PHYS-OPTICS]Physics [physics]/Physics [physics]/Optics [physics.optics], [PHYS.PHYS.PHYS-ATOM-PH]Physics [physics]/Physics [physics]/Atomic Physics [physics.atom-ph], White dwarf, Plasma, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Magnetic field, Stark effect, symbols, lcsh:QC770-798, Atomic physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The shape of atomic spectral lines in plasmas contains information on the plasma parameters, and can be used as a diagnostic tool. Under specific conditions, the plasma located at the edge of tokamaks has parameters similar to those in magnetic white dwarf stellar atmospheres, which suggests that the same line shape models can be used. A problem common to tokamak and magnetic white dwarfs concerns the modeling of Stark broadening of hydrogen lines in the presence of an external magnetic field and the related Zeeman effect. In this work, we focus on a selection of issues relevant to Stark broadening in magnetized hydrogen plasmas. Various line shape models are presented and discussed through applications to ideal cases.

Published
2017
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11. Stark broadening of Zr iv spectral lines in the atmospheres of chemically peculiar stars

Author

Zlatko Majlinger, Milan S. Dimitrijević, Zoran Simić, Astronomical Observatory Belgrade (AOB), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), and École normale supérieure - Paris (ENS-PSL)

Subjects
Physics, [PHYS]Physics [physics], atomic data, atomic processes, line: formation, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Spectral line, symbols.namesake, Stars, Stark effect, Space and Planetary Science, 0103 physical sciences, symbols, Physics::Atomic Physics, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Atomic data
Abstract

Stark widths for 18 Zr IV spectral lines have been calculated by using the modified semi-empirical method. The obtained results have been used to investigate the influence of Stark broadening on the spectra of atmospheres of chemically peculiar stars of A spectral type and hydrogen-rich DA and helium-rich DB white dwarfs. Our results have been used also to test possibility to predict new data using some approximate methods developed on the basis on regularities and systematic trends.

Published
2017
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12. Line shapes in turbulent plasmas

Author

Stamm, Roland, Hannachi, Ibtissem, Meireni, Mutia, Capes, Hubert, Godbert-Mouret, Laurence, Koubiti, Mohammed, Rosato, Joël, Marandet, Yannick, Dimitrijević, Milan, Simić, Zoran, Kieu, Ny, Kovačević-Dojcinović, Jelena, Popović, Luka, Dimitrijević, Milan S., Physique des interactions ioniques et moléculaires (PIIM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Astronomical Observatory Belgrade (AOB), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), and École normale supérieure - Paris (ENS Paris)

Subjects
Physics, [PHYS]Physics [physics], Turbulence, Plasma parameters, Langmuir Turbulence, Plasma, 01 natural sciences, Atomic and Molecular Physics, and Optics, 010305 fluids & plasmas, Ion, Computational physics, Dipole, [PHYS.QPHY]Physics [physics]/Quantum Physics [quant-ph], Physics::Plasma Physics, Electric field, Physics::Space Physics, 0103 physical sciences, Microturbulence, Statistical physics, 010306 general physics, ComputingMilieux_MISCELLANEOUS
Abstract

The fluctuations and oscillations observed in turbulent plasmas may affect the line shapes emitted by atoms and ions. We investigate several plasma conditions for which a spectroscopic signature of plasma turbulence can be observed. Starting from the simple model of microturbulence for Doppler profile, we examine how information on turbulent fluctuations is obtained in astrophysics and magnetic fusion plasmas. We recall the potential of a formalism which expresses the measured line shape in function of the probability density function of the fluctuating plasma parameters. New calculations of hydrogen dipole autocorrelation functions and line shapes are presented for plasmas affected by strong Langmuir turbulence and nonlinear wave collapse. We propose a model using a sequence of envelope solitons for the electric field created by the wave packets and felt by the emitters, and show that the line shape may be dominated by the effect of strong Langmuir turbulence.

Published
2017
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13. Stark broadening of B IV spectral lines

Author

Andjelka Kovačević, Sylvie Sahal-Bréchot, Milan S. Dimitrijević, Magdalena Christova, Zoran Simić, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astronomical Observatory Belgrade (AOB), Department of Astronomy, and École normale supérieure - Paris (ENS Paris)

Subjects
Semiclassical physics, chemistry.chemical_element, FOS: Physical sciences, 01 natural sciences, Spectral line, Physics::Geophysics, symbols.namesake, 0103 physical sciences, Physics::Atomic and Molecular Clusters, Physics::Atomic Physics, 010306 general physics, 010303 astronomy & astrophysics, Helium, ComputingMilieux_MISCELLANEOUS, Solar and Stellar Astrophysics (astro-ph.SR), Physics, [PHYS]Physics [physics], White dwarf, Astronomy and Astrophysics, Formalism (philosophy of mathematics), Stark effect, chemistry, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, symbols, Atomic physics, Homogeneous broadening, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hydrogen spectral series
Abstract

Stark broadening parameters for 157 multiplets of helium like boron (B IV) have been calculated using the impact semiclassical perturbation formalism. Obtained results have been used to investigate the regularities within spectral series. An example of the influence of Stark broadening on B IV lines in DO white dwarfs is given., 6 pages, 2 figures

Published
2016
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14. Secular evolution of asteroid families: the role of Ceres

Author

Bojan Novaković, Georgios Tsirvoulis, Clara Maurel, Vladimir Đošović, Stefano Marò, University of Belgrade [Belgrade], Astronomical Observatory Belgrade (AOB), Dipartimento di Matematica [Pisa], University of Pisa - Università di Pisa, and Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), asteroids, 010504 meteorology & atmospheric sciences, transport mechanisms, Dwarf planet, asteroid families, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Secular evolution, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, celestial mechanics, 01 natural sciences, Resonance (particle physics), Celestial mechanics, Secular resonance, Space and Planetary Science, Asteroid, 0103 physical sciences, minor planets, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We consider the role of the dwarf planet Ceres on the secular dynamics of the asteroid main belt. Specifically, we examine the post impact evolution of asteroid families due to the interaction of their members with the linear nodal secular resonance with Ceres. First, we find the location of this resonance and identify which asteroid families are crossed by its path. Next, we summarize our results for three asteroid families, namely (1726) Hoffmeister, (1128) Astrid and (1521) Seinajoki which have irregular distributions of their members in the proper elements space, indicative of the effect of the resonance. We confirm this by performing a set of numerical simulations, showcasing that the perturbing action of Ceres through its linear nodal secular resonance is essential to reproduce the actual shape of the families., Comment: 9 pages, 4 figures; to appear in Proceedings of IAU Symposium 318

Published
2016
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15. On the Stark Broadening of Lu III Spectral Lines

Author

Zoran Simić, Zlatko Majlinger, Milan S. Dimitrijević, Astronomical Observatory Belgrade (AOB), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), and École normale supérieure - Paris (ENS-PSL)

Subjects
Physics, [PHYS]Physics [physics], Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Spectral line, symbols.namesake, Stars, Stark effect, Space and Planetary Science, 0103 physical sciences, Physics::Atomic and Molecular Clusters, symbols, Physics::Atomic Physics, Atomic physics, Stark broadening, atomic data, Lu III: line profiles, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Atomic data
Abstract

The electron-impact widths for 27 Lu III spectral lines have been calculated by using the modified semiempirical method. Calculations have been also performed with the published relativistic Hartree-Fock oscillator strengths and additionally, with the approximate formula of Cowley. With the obtained results, the influence of Stark broadening on Lu III lines was investigated in the spectra of A-type stars. The obtained data will be included in the STARK-B database, which is part of the Virtual Atomic and Molecular Data Center - VAMDC.

Published
2015
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16. Stark Widths of Spectral Lines of Neutral Neon

Author

Andjelka Kovačević, Aleksandar Valjarević, Sylvie Sahal-Bréchot, Milan S. Dimitrijević, Zoran Simić, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astronomical Observatory Belgrade (AOB), Department of Astronomy, Department of Geography, and École normale supérieure - Paris (ENS-PSL)

Subjects
Stark broadening, chemistry.chemical_element, 7. Clean energy, 01 natural sciences, Spectral line, symbols.namesake, Neon, Ionization, 0103 physical sciences, atomic data, Physics::Atomic and Molecular Clusters, Physics::Atomic Physics, 010306 general physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, [PHYS]Physics [physics], Argon, Astronomy and Astrophysics, Stark effect, chemistry, Space and Planetary Science, symbols, Plasma diagnostics, Atomic physics, Homogeneous broadening, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], line profiles [Ne I], Doppler broadening
Abstract

In order to complete Stark broadening data for Ne I spectral lines which are needed for analysis of stellar atmospheres, collisional widths and shifts (the so-called Stark broadening parameters) of 29 isolated spectral lines of neutral neon have been determined within the impact semiclassical perturbation method. Calculations have been performed for the broadening by collisions with electrons, protons and ionized helium for astrophysical applications, and for collisions with ionized neon and argon for laboratory plasma diagnostics. The shifts have been compared with existing experimental values. The obtained data will be included in the STARK-B database, which is a part of the Virtual Atomic and Molecular Data Center - VAMDC.

Published
2015
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17. Stark broadening of Xe viii spectral lines

Author

Andjelka Kovačević, Aleksandar Valjarević, Zoran Simić, Sylvie Sahal-Bréchot, Milan S. Dimitrijević, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astronomical Observatory Belgrade (AOB), Department of Astronomy, Department of Geography, and École normale supérieure - Paris (ENS-PSL)

Subjects
Physics, [PHYS]Physics [physics], atomic processes, Astronomy and Astrophysics, 01 natural sciences, Spectral line, formation [line], symbols.namesake, Stark effect, Space and Planetary Science, 0103 physical sciences, symbols, atomic data, Astrophysics::Solar and Stellar Astrophysics, Atomic physics, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Atomic data, Doppler broadening
Abstract

Stark broadening parameters have been calculated for 60 spectral lines of Xe VIII, for broadening by electron, proton, and He III impacts. For calculations, the semiclassical perturbation approach in the impact approximation has been used. The widths and shifts are provided for temperatures from 20 000 K to 500 000 K and for an electron density of 10(17) cm(-3). Obtained results have been used to study the influence of Stark broadening on spectral lines in DO white dwarf atmospheres and it has been found that exist broad layers where this broadening mechanism is dominant in comparison with thermal Doppler broadening.

Published
2015
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18. Asteroid secular dynamics: Ceres’ fingerprint identified

Author

Zoran Knežević, Bojan Novaković, Clara Maurel, Georgios Tsirvoulis, University of Belgrade [Belgrade], Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), and Astronomical Observatory Belgrade (AOB)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Physics, Dwarf planet, Dynamics (mechanics), [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, celestial mechanics, Asteroid family, Celestial mechanics, Secular resonance, Space and Planetary Science, Asteroid, minor planets asteroids: individual (Ceres), Asteroid belt, Direct consequence, minor planets asteroids: general, Astrophysics - Earth and Planetary Astrophysics
Abstract

Here we report on the significant role of a so far overlooked dynamical aspect, namely a secular resonance between the dwarf planet Ceres and other asteroids. We demonstrate that this type of secular resonance can be the dominant dynamical factor in certain regions of the main asteroid belt. Specifically, we performed a dynamical analysis of the asteroids belonging to the (1726) Hoffmeister family. To identify which dynamical mechanisms are actually at work in this part of the main asteroid belt, i.e. to isolate the main perturber(s), we study the evolution of this family in time. The study is accomplished using numerical integrations of test particles performed within different dynamical models. The obtained results reveal that the post-impact evolution of the Hoffmeister asteroid family is a direct consequence of the nodal secular resonance with Ceres. This leads us to the conclusion that similar effects must exist in other parts of the asteroid belt. In this respect, the obtained results shed light on an important and entirely new aspect of the long-term dynamics of small bodies. Ceres' fingerprint in asteroid dynamics, expressed through the discovered secular resonance effect, completely changes our understanding of the way in which perturbations by Ceres-like objects affect the orbits of nearby bodies., Comment: Accepted for publication in the ApJL

Published
2015
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19. Stark Broadening in Compact Stars: Xe VI Lines

Author

Sylvie Sahal-Bréchot, Milan S. Dimitrijević, Andjelka Kovačević, Zoran Simić, Aleksandar Valjarević, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astronomical Observatory Belgrade (AOB), Department of Astronomy, Department of Geography, and École normale supérieure - Paris (ENS Paris)

Subjects
Stark broadening, Semiclassical physics, Xe VI, Astrophysics, 01 natural sciences, Spectral line, 010309 optics, symbols.namesake, 0103 physical sciences, atomic data, Astrophysics::Solar and Stellar Astrophysics, Physics::Atomic Physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, white dwarfs, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], White dwarf, Astronomy and Astrophysics, Stars, Stark effect, Space and Planetary Science, symbols, Astrophysics::Earth and Planetary Astrophysics, Atomic physics, Homogeneous broadening, Atomic data
Abstract

International audience; We will consider Stark broadening of non hydrogenic spectral lines in the impact approximation in compact stars: pre-white dwarf and white dwarf atmospheres. In order to show an example, Stark broadening parameters have been calculated, using the impact semiclassical perturbation approach for four Xe VI spectral lines. Obtained results have been used to demonstrate the influence of Stark broadening in DA and DB white dwarf atmospheres.

Published
2015
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20. Stark broadening of B IV lines for astrophysical and laboratory plasma research

Author

Sylvie Sahal-Bréchot, Magdalena Christova, Zoran Simić, Andjelka Kovačević, Milan S. Dimitrijević, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Astronomical Observatory Belgrade (AOB), Department of Astronomy, and École normale supérieure - Paris (ENS-PSL)

Subjects
Physics, [PHYS]Physics [physics], Atmospheric Science, Atomic Physics (physics.atom-ph), FOS: Physical sciences, Aerospace Engineering, Perturbation (astronomy), Astronomy and Astrophysics, Plasma, Physics - Atomic Physics, Formalism (philosophy of mathematics), symbols.namesake, Geophysics, Stark effect, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, symbols, General Earth and Planetary Sciences, Atomic physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hydrogen spectral series, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, Atomic data
Abstract

Stark broadening parameters for 36 multiplets of B IV have been calculated using the semi-classical perturbation formalism. Obtained results have been used to investigate the regularities within spectral series and temperature dependence., 8 pages, 6 figures, 1 table, in press in Advances in Space Research

Published
2014
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21. Virtual Atomic and Molecular Data Center

Author

Dubernet, M. L., Vincent Boudon, Culhane, J. L., Dimitrijevic, M. S., Fazliev, A. Z., Joblin, C., Kupka, F., Leto, G., Pierre Le Sidaner, Loboda, P. A., Mason, H. E., Mason, N. J., Mendoza, C., Mulas, G., Millar, T. J., Nuñez, L. A., Perevalov, V. I., Piskunov, N., Ralchenko, Y., Rixon, G., Rothman, L. S., Roueff, E., Ryabchikova, T. A., Ryabtsev, A., Sahal-Brechot, S., Bernard Schmitt, Schlemmer, S., Tennyson, J., Tyuterev, Vladimir G., Walton, N. A., Valentine Wakelam, Zeippen, C. J., Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique ( LPMAA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Interdisciplinaire Carnot de Bourgogne ( LICB ), Université de Bourgogne ( UB ) -Centre National de la Recherche Scientifique ( CNRS ), Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Astronomical Observatory Belgrade, V.E. Zuev Institute of Atmospheric Optics ( IAO ), Siberian Branch of the Russian Academy of Sciences ( SB RAS ), Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France, Centre Etud Spatiale Rayonnements Toulouse, University Vienna, Fac Math, Osserv Astrofis Catania, Ist Nazl Astrofis, Observatoire de Paris - Site de Meudon ( OBSPM ), Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS ), All-Russian Scientific Research Institute of Technical Physics RFNTC VNIITF, Centre for Mathematical Science, Dept Appl Math & Theoret Phys Cambridge, Centre for Mathematical Science, Open university Faculty of Sciences, Universidad de Los Andes Venezuela, CeCalCULA, Corp Parque Tecnol Merida, Ctr Calculo Cient, Universidad de Los Andes Venezuela, Instituto Venezolano Investigaciones Cientificas, Ctr Fis, Caracas, Instituto Venezolano Investigaciones Cientificas, Osservatorio Astronomico di Cagliari, Ist Nazl Astrofis, Osservatorio Astronomico di Cagliari, Queen's UniversityBelfast, Sch Math & Phys, Universidad Industrial de Santander [Bucaramanga] ( UIS ), AMOR 2010, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ), Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique (LPMAA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interdisciplinaire Carnot de Bourgogne (ICB), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Astronomical Observatory Belgrade (AOB), V.E. Zuev Institute of Atmospheric Optics (IAO), Siberian Branch of the Russian Academy of Sciences (SB RAS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Universidad de Los Andes [Mérida, Venezuela] (ULA), INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), Queen's University [Belfast] (QUB), Universidad Industrial de Santander [Bucaramanga] (UIS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Francois, Francoise, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Interdisciplinaire Carnot de Bourgogne (LICB), Universidad de Los Andes [Venezuela] (ULA), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

(special issue HighRus2009). VAMDC; International audience

Published
2010

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