Special Issue "Spectral Line Shapes in Astrophysics and Related Topics"

A special issue of Atoms (ISSN 2218-2004).

Deadline for manuscript submissions: closed (1 September 2017)

Special Issue Editors

Guest Editor
Dr. Milan S. Dimitrijević

Astronomical Observatory, Belgrade, Serbia
Website | E-Mail
Interests: stark broadening; line profiles; stellar spectra; atomic and ionic collisions with formation of quasimolecules; atomic processes in white dwarfs and solar type stars; astroinformatics; databases; history and philosophy of science
Guest Editor
Prof. Dr. Luka Č. Popović

Astronomical Observatory, Belgrade, Serbia
Website | E-Mail
Interests: astrophysical spectra; spectra of active galactic nuclei; line profiles; stark broadening; astroinformatics; databases

Special Issue Information

Dear Colleagues,

Spectral lines, their widths, and shapes, are powerful tools for emitting/absorbing gas diagnostics in different astrophysical objects (from the Solar system to the most distant objects in the Universe—quasars). The emission/absorption lines of astrophysical objects are produced over a wide range of distances from an observer and under a wide range of physical and kinematical conditions. Therefore, in astrophysical objects, the lines from X-ray (Fe K) to the radio (radio recombination line) have been observed. On the other hand, the experimental and theoretical investigations of laboratory plasma have been applied in spectroscopic astrophysical research, especially in atomic data needed for line shape calculations. Data on spectral lines and their profiles are also important for diagnostics, analysis and modelling of fusion plasma, laser produced plasma, lasers design and development and various plasmas in industry and technology like light sources based on plasmas or welding and piercing of metals by laser produced plasma. This Special Issue of Atoms will highlight the need for continuing research on the spectral line shapes and will review present investigation in astrophysics where spectral line shapes have been used as a tool to investigate physical and kinematical properties of celestial objects. Moreover, there will be a number of studies of spectral line shapes in laboratory plasma, fusion plasma, laser-produced plasma, and about atomic data needed for the calculation of spectral line properties. 

Dr. Milan S. Dimitrijević
Prof. Luka Č. Popović
Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All papers will be peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Atoms is an international peer-reviewed open access quarterly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. The Article Processing Charge (APC) for publication in this open access journal is 350 CHF (Swiss Francs). Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  •  spectra
  • line profiles
  • stellar spectra
  • AGN spectra
  • interstellar spectra
  • laboratory plasma
  • fusion plasma
  • lasers
  • plasma in industry
  • stars
  • extragalactic objects

Published Papers (19 papers)

View options order results:
result details:
Displaying articles 1-19
Export citation of selected articles as:

Research

Jump to: Other

Open AccessFeature PaperArticle Nonlinear Spectroscopy of Alkali Atoms in Cold Medium of Astrophysical Relevance
Atoms 2017, 5(4), 50; doi:10.3390/atoms5040050
Received: 31 August 2017 / Revised: 21 November 2017 / Accepted: 2 December 2017 / Published: 6 December 2017
PDF Full-text (877 KB) | HTML Full-text | XML Full-text
Abstract
The time-dependent population dynamics of hyperfine (HF) sublevels of n2p3/2 atomic states upon laser excitation in a cold medium of alkali atoms is examined. We demonstrate some peculiarities of the absorption HF multiplet formation in D2-line resulting
[...] Read more.
The time-dependent population dynamics of hyperfine (HF) sublevels of n 2 p 3 / 2 atomic states upon laser excitation in a cold medium of alkali atoms is examined. We demonstrate some peculiarities of the absorption HF multiplet formation in D2-line resulting from a long interaction time (∼200 μ s) interaction between light and Na ( n = 3 ) and Cs ( n = 6 ) atoms in a cold and slow sub-thermal ( T 1 K) beam. We analytically describe a number of D2-line-shape effects that are of interest in spectroscopic studies of cold dusty white dwarfs: broadening by optical pumping, intensity redistribution within components of D2-line HF multiplet for partially closed transitions and asymmetry of absorption lines induced by AC Stark shifts for cyclic transitions. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Regularities and Systematic Trends on Zr IV Stark Widths
Atoms 2017, 5(4), 49; doi:10.3390/atoms5040049
Received: 10 September 2017 / Revised: 14 October 2017 / Accepted: 23 November 2017 / Published: 1 December 2017
PDF Full-text (220 KB) | HTML Full-text | XML Full-text
Abstract
Regularities and systematic trends among the Stark widths of 18 Zr IV spectral lines obtained by modified semiempirical approach have been discussed. Also we compared those calculated Stark broadening parameters with estimates according to Cowley, Purić et al. and Purić and Šćepanović and
[...] Read more.
Regularities and systematic trends among the Stark widths of 18 Zr IV spectral lines obtained by modified semiempirical approach have been discussed. Also we compared those calculated Stark broadening parameters with estimates according to Cowley, Purić et al. and Purić and Šćepanović and checked the possibility to find some new estimates. It is demonstrated as well that the formula of Cowley (1971) overestimates Stark widths, obtained by using modified semiempirical method, with the increase of angular orbital momentum quantum number due to its neglection. It is also found that the results obtained by using formula for simple estimates of Purić et al. (1991) are in agreement with the modified semiempirical results within the estimated error bars of both methods, while the estimates using formula of Purić and Šćepanović (1999) are in strong disagreement which increases with the increase of angular orbital momentum quantum number. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Open AccessFeature PaperArticle Rosetta Mission: Electron Scattering Cross Sections—Data Needs and Coverage in BEAMDB Database
Atoms 2017, 5(4), 46; doi:10.3390/atoms5040046
Received: 21 September 2017 / Revised: 13 November 2017 / Accepted: 14 November 2017 / Published: 17 November 2017
PDF Full-text (5446 KB) | HTML Full-text | XML Full-text
Abstract
The emission of [O I] lines in the coma of Comet 67P/Churyumov-Gerasimenko during the Rosetta mission have been explained by electron impact dissociation of water rather than the process of photodissociation. This is the direct evidence for the role of electron induced processing
[...] Read more.
The emission of [O I] lines in the coma of Comet 67P/Churyumov-Gerasimenko during the Rosetta mission have been explained by electron impact dissociation of water rather than the process of photodissociation. This is the direct evidence for the role of electron induced processing has been seen on such a body. Analysis of other emission features is handicapped by a lack of detailed knowledge of electron impact cross sections which highlights the need for a broad range of electron scattering data from the molecular systems detected on the comet. In this paper, we present an overview of the needs for electron scattering data relevant for the understanding of observations in coma, the tenuous atmosphere and on the surface of 67P/Churyumov-Gerasimenko during the Rosetta mission. The relevant observations for elucidating the role of electrons come from optical spectra, particle analysis using the ion and electron sensors and mass spectrometry measurements. To model these processes electron impact data should be collated and reviewed in an electron scattering database and an example is given in the BEAMD, which is a part of a larger consortium of Virtual Atomic and Molecular Data Centre—VAMDC. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Active Galactic Nuclei Search
Atoms 2017, 5(4), 45; doi:10.3390/atoms5040045
Received: 10 September 2017 / Revised: 6 November 2017 / Accepted: 7 November 2017 / Published: 10 November 2017
PDF Full-text (2388 KB) | HTML Full-text | XML Full-text
Abstract
We present the first results of medium-band photometric observations on the 1m Schmidt Telescope of Byurakan Astrophysical Observatory (Armenia). The object sample was created in the SA68 field. The medium-band filter set (13 filters with FWHM = 250 Å + 5 broadband SDSS
[...] Read more.
We present the first results of medium-band photometric observations on the 1m Schmidt Telescope of Byurakan Astrophysical Observatory (Armenia). The object sample was created in the SA68 field. The medium-band filter set (13 filters with FWHM = 250 Å + 5 broadband SDSS filters) allowed us to create low-resolution spectra of each object in the SA68 field. We compared them with the template spectra to select AGNs and to determine their photometric redshifts. Our sample consists of 330 objects with 0.5–5.1 redshift range and complete up to 23.0 AB magnitude. The comparison of our sample with SDSS DR10 and BOSS + MMT QSO showed that sufficiently more objects in the 3.2–5.1 redshift range were found. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle A New Analysis of Stark and Zeeman Effects on Hydrogen Lines in Magnetized DA White Dwarfs
Atoms 2017, 5(4), 44; doi:10.3390/atoms5040044
Received: 8 September 2017 / Revised: 13 October 2017 / Accepted: 1 November 2017 / Published: 6 November 2017
PDF Full-text (917 KB) | HTML Full-text | XML Full-text
Abstract
White dwarfs with magnetic field strengths larger than 10 T are understood to represent more than 10% of the total population of white dwarfs. The presence of such strong magnetic fields is clearly indicated by the Zeeman triplet structure visible on absorption lines.
[...] Read more.
White dwarfs with magnetic field strengths larger than 10 T are understood to represent more than 10% of the total population of white dwarfs. The presence of such strong magnetic fields is clearly indicated by the Zeeman triplet structure visible on absorption lines. In this work, we discuss the line broadening mechanisms and focus on the sensitivity of hydrogen lines on the magnetic field. We perform new calculations in conditions relevant to magnetized DA stellar atmospheres using models inspired from magnetic fusion plasma spectroscopy. A white dwarf spectrum from the Sloan Digital Sky Survey (SDSS) database is analyzed. An effective temperature is provided by an adjustment of the background radiation with a Planck function, and the magnetic field is inferred from absorption lines presenting a Zeeman triplet structure. An order-of-magnitude estimate for the electron density is also performed from Stark broadening analysis. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Models of Emission-Line Profiles and Spectral Energy Distributions to Characterize the Multi-Frequency Properties of Active Galactic Nuclei
Atoms 2017, 5(4), 43; doi:10.3390/atoms5040043
Received: 10 September 2017 / Revised: 22 October 2017 / Accepted: 23 October 2017 / Published: 6 November 2017
PDF Full-text (567 KB) | HTML Full-text | XML Full-text
Abstract
The spectra of active galactic nuclei (AGNs) are often characterized by a wealth of emission lines with different profiles and intensity ratios that lead to a complicated classification. Their electromagnetic radiation spans more than 10 orders of magnitude in frequency. In spite of
[...] Read more.
The spectra of active galactic nuclei (AGNs) are often characterized by a wealth of emission lines with different profiles and intensity ratios that lead to a complicated classification. Their electromagnetic radiation spans more than 10 orders of magnitude in frequency. In spite of the differences between various classes, the origin of their activity is attributed to a combination of emitting components, surrounding an accreting supermassive black hole (SMBH), in the unified model. Currently, the execution of sky surveys, with instruments operating at various frequencies, provides the possibility to detect and to investigate the properties of AGNs on very large statistical samples. As a result of the spectroscopic surveys that allow the investigation of many objects, we have the opportunity to place new constraints on the nature and evolution of AGNs. In this contribution, we present the results obtained by working on multi-frequency data, and we discuss their relations with the available optical spectra. We compare our findings with the AGN unified model predictions, and we present a revised technique to select AGNs of different types from other line-emitting objects. We discuss the multi-frequency properties in terms of the innermost structures of the sources. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle The Screening Characteristics of the Dense Astrophysical Plasmas: The Three-Component Systems
Atoms 2017, 5(4), 42; doi:10.3390/atoms5040042
Received: 31 August 2017 / Revised: 14 October 2017 / Accepted: 19 October 2017 / Published: 2 November 2017
PDF Full-text (493 KB) | HTML Full-text | XML Full-text
Abstract
As the object of investigation, astrophysical fully ionized electron-ion plasma is chosen with positively charged ions of two different kinds, including the plasmas of higher non-ideality. The direct aim of this work is to develop, within the problem of finding the mean potential
[...] Read more.
As the object of investigation, astrophysical fully ionized electron-ion plasma is chosen with positively charged ions of two different kinds, including the plasmas of higher non-ideality. The direct aim of this work is to develop, within the problem of finding the mean potential energy of the charged particle for such plasma, a new model, self-consistent method of describing the electrostatic screening. Within the presented method, such extremely significant phenomena as the electron-ion and ion-ion correlations are included in the used model. We wish to draw attention to the fact that the developed method is suitable for astrophysical applications. Here we keep in mind that in outer shells of stars, the physical conditions change from those that correspond to the rare, practically ideal plasma, to those that correspond to extremely dense non-ideal plasma. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Using the Pairs of Lines Broadened by Collisions with Neutral and Charged Particles for Gas Temperature Determination of Argon Non-Thermal Plasmas at Atmospheric Pressure
Atoms 2017, 5(4), 41; doi:10.3390/atoms5040041
Received: 1 September 2017 / Revised: 16 October 2017 / Accepted: 17 October 2017 / Published: 23 October 2017
PDF Full-text (1035 KB) | HTML Full-text | XML Full-text
Abstract
The spectroscopic method for gas temperature determination in argon non-thermal plasmas sustained at atmospheric pressure proposed recently by Spectrochimica Acta Part B 129 14 (2017)—based on collisional broadening measurements of selected pairs of argon atomic lines, has been applied to other pairs of
[...] Read more.
The spectroscopic method for gas temperature determination in argon non-thermal plasmas sustained at atmospheric pressure proposed recently by Spectrochimica Acta Part B 129 14 (2017)—based on collisional broadening measurements of selected pairs of argon atomic lines, has been applied to other pairs of argon atomic lines, and the discrepancies found in some of these results have been analyzed. For validation purposes, the values of the gas temperature obtained using the different pairs of lines have been compared with the rotational temperatures derived from the OH ro-vibrational bands, using the Boltzmann-plot technique. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Detailed Investigation of the Electric Discharge Plasma between Copper Electrodes Immersed into Water
Atoms 2017, 5(4), 40; doi:10.3390/atoms5040040
Received: 11 September 2017 / Revised: 15 October 2017 / Accepted: 16 October 2017 / Published: 23 October 2017
PDF Full-text (4023 KB) | HTML Full-text | XML Full-text
Abstract
A phenomenological picture of pulsed electrical discharge in water is produced by combining electrical, spectroscopic, and imaging methods. The discharge is generated by applying ~350 μs long 100 to 220 V pulses (values of current from 400 to 1000 A, respectively) between the
[...] Read more.
A phenomenological picture of pulsed electrical discharge in water is produced by combining electrical, spectroscopic, and imaging methods. The discharge is generated by applying ~350 μs long 100 to 220 V pulses (values of current from 400 to 1000 A, respectively) between the point-to-point copper electrodes submerged into the non-purified tap water. Plasma channel and gas bubble occur between the tips of the electrodes, which are initially in contact with each other. The study includes detailed experimental investigation of plasma parameters of such discharge using the correlation between time-resolved high-speed imaging, electrical characteristics, and optical emission spectroscopic data. Radial distributions of the electron density of plasma is estimated from the analysis of profiles and widths of registered Hα and Hβ hydrogen lines, and Cu I 515.3 nm line, exposed to the Stark mechanism of spectral lines’ broadening. Estimations of the electrodes’ erosion rate and bubbles’ size depending on the electrical input parameters of the circuit are presented. Experimental results of this work may be valuable for the advancement of modeling and the theoretical understanding of the pulse electric discharges in water. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Stark-Zeeman Line Shape Modeling for Magnetic White Dwarf and Tokamak Edge Plasmas: Common Challenges
Atoms 2017, 5(4), 36; doi:10.3390/atoms5040036
Received: 23 August 2017 / Revised: 21 September 2017 / Accepted: 29 September 2017 / Published: 4 October 2017
Cited by 1 | PDF Full-text (2320 KB) | HTML Full-text | XML Full-text
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
[...] Read more.
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. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Line Shape Modeling for the Diagnostic of the Electron Density in a Corona Discharge
Atoms 2017, 5(4), 35; doi:10.3390/atoms5040035
Received: 31 August 2017 / Revised: 23 September 2017 / Accepted: 24 September 2017 / Published: 28 September 2017
PDF Full-text (456 KB) | HTML Full-text | XML Full-text
Abstract
We present an analysis of spectra observed in a corona discharge designed for the study of dielectrics in electrical engineering. The medium is a gas of helium and the discharge was performed at the vicinity of a tip electrode under high voltage. The
[...] Read more.
We present an analysis of spectra observed in a corona discharge designed for the study of dielectrics in electrical engineering. The medium is a gas of helium and the discharge was performed at the vicinity of a tip electrode under high voltage. The shape of helium lines is dominated by the Stark broadening due to the plasma microfield. Using a computer simulation method, we examine the sensitivity of the He 492 nm line shape to the electron density. Our results indicate the possibility of a density diagnostic based on passive spectroscopy. The influence of collisional broadening due to interactions between the emitters and neutrals is discussed. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Effect of Turbulence on Line Shapes in Astrophysical and Fusion Plasmas
Atoms 2017, 5(4), 34; doi:10.3390/atoms5040034
Received: 30 August 2017 / Revised: 15 September 2017 / Accepted: 18 September 2017 / Published: 25 September 2017
PDF Full-text (8034 KB) | HTML Full-text | XML Full-text
Abstract
We look at the effect of wave collapse turbulence on a hydrogen line shape in plasma. An atom immersed in plasma affected by strong Langmuir turbulence may be perturbed by a sequence of wave packets with a maximum electric field magnitude that is
[...] Read more.
We look at the effect of wave collapse turbulence on a hydrogen line shape in plasma. An atom immersed in plasma affected by strong Langmuir turbulence may be perturbed by a sequence of wave packets with a maximum electric field magnitude that is larger than the Holtsmark field. For such conditions, we propose to calculate the shape of the hydrogen Lyman α Lyman β and Balmer α lines with a numerical integration of the Schrödinger equation coupled to a simulation of a sequence of electric fields modeling the effects of the Langmuir wave. We present and discuss several line profiles of Lyman and Balmer lines. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Quasar Black Hole Mass Estimates from High-Ionization Lines: Breaking a Taboo?
Atoms 2017, 5(3), 33; doi:10.3390/atoms5030033
Received: 31 August 2017 / Revised: 12 September 2017 / Accepted: 14 September 2017 / Published: 20 September 2017
Cited by 1 | PDF Full-text (1210 KB) | HTML Full-text | XML Full-text
Abstract
Can high ionization lines such as CIVλ1549 provide useful virial broadening estimators for computing the mass of the supermassive black holes that power the quasar phenomenon? The question has been dismissed by several workers as a rhetorical one because blue-shifted, non-virial
[...] Read more.
Can high ionization lines such as CIV λ 1549 provide useful virial broadening estimators for computing the mass of the supermassive black holes that power the quasar phenomenon? The question has been dismissed by several workers as a rhetorical one because blue-shifted, non-virial emission associated with gas outflows is often prominent in CIV λ 1549 line profiles. In this contribution, we first summarize the evidence suggesting that the FWHM of low-ionization lines like H β and MgII λ 2800 provide reliable virial broadening estimators over a broad range of luminosity. We confirm that the line widths of CIV λ 1549 is not immediately offering a virial broadening estimator equivalent to the width of low-ionization lines. However, capitalizing on the results of Coatman et al. (2016) and Sulentic et al. (2017), we suggest a correction to FWHM CIV λ 1549 for Eddington ratio and luminosity effects that, however, remains cumbersome to apply in practice. Intermediate ionization lines (IP ∼ 20–30 eV; AlIII λ 1860 and SiIII] λ 1892) may provide a better virial broadening estimator for high redshift quasars, but larger samples are needed to assess their reliability. Ultimately, they may be associated with the broad-line region radius estimated from the photoionization method introduced by Negrete et al. (2013) to obtain black hole mass estimates independent from scaling laws. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Stark Broadening from Impact Theory to Simulations
Atoms 2017, 5(3), 32; doi:10.3390/atoms5030032
Received: 31 August 2017 / Accepted: 11 September 2017 / Published: 20 September 2017
PDF Full-text (2918 KB) | HTML Full-text | XML Full-text
Abstract
Impact approximation is widely used for calculating Stark broadening in a plasma. We review its main features and different types of models that make use of it. We discuss recent developments, in particular a quantum approach used for both the emitter and the
[...] Read more.
Impact approximation is widely used for calculating Stark broadening in a plasma. We review its main features and different types of models that make use of it. We discuss recent developments, in particular a quantum approach used for both the emitter and the perturbers. Numerical simulations are a useful tool for gaining insight into the mechanisms at play in impact-broadening conditions. Our simple model allows the integration of the Schrödinger equation for an emitter submitted to a fluctuating electric field. We show how we can approach the impact results, and how we can investigate conditions beyond the impact approximation. The simple concepts developed in impact and simulation approaches enable the analysis of complex problems such as the effect of plasma rogue waves on hydrogen spectra. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Radiative and Collisional Molecular Data and Virtual Laboratory Astrophysics
Atoms 2017, 5(3), 31; doi:10.3390/atoms5030031
Received: 4 September 2017 / Revised: 12 September 2017 / Accepted: 13 September 2017 / Published: 19 September 2017
PDF Full-text (597 KB) | HTML Full-text | XML Full-text
Abstract
Spectroscopy has been crucial for our understanding of physical and chemical phenomena. The interpretation of interstellar line spectra with radiative transfer calculations usually requires two kinds of molecular input data: spectroscopic data (such as energy levels, statistical weights, transition probabilities, etc.) and collision
[...] Read more.
Spectroscopy has been crucial for our understanding of physical and chemical phenomena. The interpretation of interstellar line spectra with radiative transfer calculations usually requires two kinds of molecular input data: spectroscopic data (such as energy levels, statistical weights, transition probabilities, etc.) and collision data. This contribution describes how such data are collected, stored, and which limitations exist. Also, here we summarize challenges of atomic/molecular databases and point out our experiences, problems, etc., which we are faced with. We present overview of future developments and needs in the areas of radiative transfer and molecular data. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Open AccessFeature PaperArticle Stark Widths of Na IV Spectral Lines
Atoms 2017, 5(3), 29; doi:10.3390/atoms5030029
Received: 16 August 2017 / Revised: 8 September 2017 / Accepted: 14 September 2017 / Published: 18 September 2017
PDF Full-text (733 KB) | HTML Full-text | XML Full-text
Abstract
Sodium is a very important element for the research and analysis of astrophysical, laboratory, and technological plasmas, but neither theoretical nor experimental data on Stark broadening of Na IV spectral lines are present in the literature. Using the modified semiempirical method of Dimitrijević
[...] Read more.
Sodium is a very important element for the research and analysis of astrophysical, laboratory, and technological plasmas, but neither theoretical nor experimental data on Stark broadening of Na IV spectral lines are present in the literature. Using the modified semiempirical method of Dimitrijević and Konjević, here Stark widths have been calculated for nine Na IV transitions. Na IV belongs to the oxygen isoelectronic sequence, and we have calculated Stark widths belonging to singlets, triplets, and quintuplets, as well as with different parent terms. This is used to discuss similarities within one transition array with different multiplicities and parent terms. Additionally, calculated widths will be implemented in the STARK-B database (http://stark-b.obspm.fr) which is also a part of the Virtual Atomic and Molecular Data Center (VAMDC—http://www.vamdc.org/). Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Open AccessFeature PaperArticle Semiclassical Stark Broadening Parameters of Ar VII Spectral Lines
Atoms 2017, 5(3), 27; doi:10.3390/atoms5030027
Received: 16 August 2017 / Revised: 1 September 2017 / Accepted: 6 September 2017 / Published: 8 September 2017
PDF Full-text (228 KB) | HTML Full-text | XML Full-text
Abstract
Using the semi-classical perturbation approach in the impact approximation, full width at half maximum and shift have been determined for eight spectral lines of Ar VII, for broadening by electron-, proton-, and He III-impacts. The results are provided for temperatures from 20,000 K
[...] Read more.
Using the semi-classical perturbation approach in the impact approximation, full width at half maximum and shift have been determined for eight spectral lines of Ar VII, for broadening by electron-, proton-, and He III-impacts. The results are provided for temperatures from 20,000 K to 500,000 K, and for an electron density of 10 18 cm 3 . The obtained results will be included in the STARK-B database, which is also in the virtual atomic and molecular data center (VAMDC). Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Open AccessFeature PaperArticle Stark Widths of Ar II Spectral Lines in the Atmospheres of Subdwarf B Stars
Atoms 2017, 5(3), 26; doi:10.3390/atoms5030026
Received: 29 August 2017 / Accepted: 4 September 2017 / Published: 7 September 2017
PDF Full-text (357 KB) | HTML Full-text | XML Full-text
Abstract
Stark broadening parameters are of interest for many problems in astrophysics and laboratory plasmas investigation. Ar II spectral lines are observed in many kinds of stellar atmospheres such as the atmospheres of B-Type stars and subdwarf B stars. In this work, we present
[...] Read more.
Stark broadening parameters are of interest for many problems in astrophysics and laboratory plasmas investigation. Ar II spectral lines are observed in many kinds of stellar atmospheres such as the atmospheres of B-Type stars and subdwarf B stars. In this work, we present theoretical Stark widths for Ar II spectral lines. We use the impact semiclassical perturbation approach. Our results are compared with the available experimental values. Finally, the importance of the Stark broadening mechanism is studied in atmospheric conditions of subdwarf B stars. Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Other

Jump to: Research

Open AccessFeature PaperProject Report Photometric and Polarimetric Interpretation of Blazar AO 0235+164 Behaviour
Atoms 2017, 5(4), 39; doi:10.3390/atoms5040039
Received: 7 September 2017 / Revised: 30 September 2017 / Accepted: 3 October 2017 / Published: 19 October 2017
PDF Full-text (2901 KB) | HTML Full-text | XML Full-text
Abstract
Among the great number of controversial issues, the most topical one both for theoretical and observational astrophysics presently is a problem of active galactic nuclei investigation. To explain the behaviour of blazar AO 0235+164, which has been under observation at the LX200 telescope
[...] Read more.
Among the great number of controversial issues, the most topical one both for theoretical and observational astrophysics presently is a problem of active galactic nuclei investigation. To explain the behaviour of blazar AO 0235+164, which has been under observation at the LX200 telescope (SPbSU) since 2002, the method of analyzing developed by V.A. Hagen-Thorn and S.G. Marchenko was applied. It is based on the assumption that in the case of observational data lying on the straight line in the absolute Stokes parameters space { I , Q , U } (for polarimetry) and the fluxes space { F 1 , . . F n } (for photometry), relative Stokes parameters and relative flux ratios stay unchanged , and consequently, only one source is corresponding to the variability of general value of flux. In this paper, the photometric and polarimetric interpretation of blazar behaviour is presented. Furthermore, the flux and flux–flux diagrams are obtained for three periods of object monitoring: 2006–2007 and 2008–2009 (outbursts) and 2009–2016 (decline with 2015 outburst). Full article
(This article belongs to the Special Issue Spectral Line Shapes in Astrophysics and Related Topics)
Figures

Figure 1

Back to Top