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Astronomy in the Big Data Era: Perspectives
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Astronomy in the Big Data Era: Perspectives

A special issue of Data (ISSN 2306-5729). This special issue belongs to the section "Spatial Data Science and Digital Earth".

Deadline for manuscript submissions: closed (1 March 2021) | Viewed by 22467

Special Issue Editors

Prof. Dr. Luka Č. Popović

E-Mail Website
Guest Editor
1. Astronomical Observatory, in Belgrade, Bolgina 7, 11160 Belgrade, Serbia
2. Faculty of Mathematics University of Belgrade, Studentski Trg 16, Belgrade, Serbia
Interests: active galactic nuclei; gravitational lensing; plasma physics; ionosphere
Special Issues, Collections and Topics in MDPI journals
Prof. Dr. Vladimir Sreckovic

E-Mail Website
Guest Editor
The Astrophysics and Ionospheric Laboratory, Institute of Physics Belgrade, University of Belgrade, 11080 Belgrade, Serbia
Interests: space weather studies of upper atmosphere; astrogeoinformatics; astroinformatics; databases; data-mining; natural hazards
Special Issues, Collections and Topics in MDPI journals
Prof. Dr. Milan S. Dimitrijević

E-Mail Website
Guest Editor
Astronomical Observatory, Volgina 7, 11060 Belgrade, Serbia
Interests: stark broadening formalism and calculations; atomic and molecular collisions; stellar spectra; atomic data and databases
Special Issues, Collections and Topics in MDPI journals

Special Issue Information

Dear Colleagues,

Contemporary astronomy is strongly influenced by cosmic missions (e.g., SDSS Gaia) and onboard telescopes and spectrographs are constantly observing and collecting a huge amount of astronomical data (from photometric to spectroscopic data). Additionally, a large number of telescopes located in different places on Earth produce observational data that can be used for astronomical investigations. However, in this era of big data, research into very different astronomical topics also exist.

In this Special Issue, we will present an overview of astronomical research in Serbia and Bulgaria based on selected papers from the XII Serbian–Bulgarian astronomical conference. We are also inviting other researchers to contribute to this issue with the results of their investigations and reviews on different astronomical topics.

Prof. Dr. Luka Č. Popović
Dr. Vladimir A. Sreckovic
Prof. Dr. Milan S. Dimitrijević
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 submissions that pass pre-check are 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.

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Please visit the Instructions for Authors page before submitting a manuscript. The Article Processing Charge (APC) for publication in this open access journal is 1600 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

  • astronomy
  • astrophysics
  • astroinformatics

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Published Papers (7 papers)

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Research

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11 pages, 829 KiB  
Article
No-z Model for Magnetic Fields of Different Astrophysical Objects and Stability of the Solutions
by Evgeny Mikhailov, Daniela Boneva and Maria Pashentseva
Data 2021, 6(1), 4; https://doi.org/10.3390/data6010004 - 10 Jan 2021
Viewed by 2985
Abstract
A wide range of astrophysical objects, such as the Sun, galaxies, stars, planets, accretion discs etc., have large-scale magnetic fields. Their generation is often based on the dynamo mechanism, which is connected with joint action of the alpha-effect and differential rotation. They compete [...] Read more.
A wide range of astrophysical objects, such as the Sun, galaxies, stars, planets, accretion discs etc., have large-scale magnetic fields. Their generation is often based on the dynamo mechanism, which is connected with joint action of the alpha-effect and differential rotation. They compete with the turbulent diffusion. If the dynamo is intensive enough, the magnetic field grows, else it decays. The magnetic field evolution is described by Steenbeck—Krause—Raedler equations, which are quite difficult to be solved. So, for different objects, specific two-dimensional models are used. As for thin discs (this shape corresponds to galaxies and accretion discs), usually, no-z approximation is used. Some of the partial derivatives are changed by the algebraic expressions, and the solenoidality condition is taken into account as well. The field generation is restricted by the equipartition value and saturates if the field becomes comparable with it. From the point of view of mathematical physics, they can be characterized as stable points of the equations. The field can come to these values monotonously or have oscillations. It depends on the type of the stability of these points, whether it is a node or focus. Here, we study the stability of such points and give examples for astrophysical applications. Full article
(This article belongs to the Special Issue Astronomy in the Big Data Era: Perspectives)
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8 pages, 1290 KiB  
Article
Mid-Cycle Observations of CR Boo and Estimation of the System’s Parameters
by Daniela Boneva, Svetlana Boeva, Yanko Nikolov, Zorica Cvetković and Radoslav Zamanov
Data 2020, 5(4), 113; https://doi.org/10.3390/data5040113 - 2 Dec 2020
Cited by 2 | Viewed by 2757
Abstract
We present observations (with NAO Rozhen and AS Vidojevica telescopes) of the AM Canum Venaticorum (AM CVn) binary star CR Bootis (CR Boo) in the UBV bands. The data were obtained in two nights in July 2019, when the V band brightness was [...] Read more.
We present observations (with NAO Rozhen and AS Vidojevica telescopes) of the AM Canum Venaticorum (AM CVn) binary star CR Bootis (CR Boo) in the UBV bands. The data were obtained in two nights in July 2019, when the V band brightness was in the range of 16.1–17.0 mag. In both nights, a variability for a period of 25 ± 1 min and amplitude of about 0.2 magnitudes was visible. These brightness variations are most likely indications of “humps”. During our observational time, they appear for a period similar to the CR Boo orbital period. A possible reason of their origin is the phase rotation of the bright spot, placed in the contact point of the infalling matter and the outer disc edge. We estimated some of the parameters of the binary system, on the base of the observational data. Full article
(This article belongs to the Special Issue Astronomy in the Big Data Era: Perspectives)
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Other

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12 pages, 240 KiB  
Data Descriptor
Stark Width Data for Tb II, Tb III and Tb IV Spectral Lines
by Milan S. Dimitrijević
Data 2021, 6(3), 28; https://doi.org/10.3390/data6030028 - 8 Mar 2021
Viewed by 2000
Abstract
A dataset of Stark widths for Tb II, Tb III and Tb IV is presented. To data obtained before, the results of new calculations for 62 Tb III lines from 5d to 6pj(6,j)o, a transition array, have been added. [...] Read more.
A dataset of Stark widths for Tb II, Tb III and Tb IV is presented. To data obtained before, the results of new calculations for 62 Tb III lines from 5d to 6pj(6,j)o, a transition array, have been added. Calculations have been performed by using the simplified modified semiempirical method for temperatures from 5000 to 80,000 K for an electron density of 1017 cm−3. The results were also used to discuss the regularities within multiplets and a supermultiplet. Full article
(This article belongs to the Special Issue Astronomy in the Big Data Era: Perspectives)
7 pages, 2777 KiB  
Data Descriptor
On the Stark Broadening of Be II Spectral Lines
by Milan S. Dimitrijević, Magdalena Christova and Sylvie Sahal-Bréchot
Data 2020, 5(4), 106; https://doi.org/10.3390/data5040106 - 23 Nov 2020
Viewed by 2505
Abstract
Calculated Stark broadening parameters of singly ionized beryllium spectral lines have been reported. Three spectral series have been studied within semiclassical perturbation theory. The plasma conditions cover temperatures from 2500 to 50,000 K and perturber densities 1011 cm−3 and 1013 [...] Read more.
Calculated Stark broadening parameters of singly ionized beryllium spectral lines have been reported. Three spectral series have been studied within semiclassical perturbation theory. The plasma conditions cover temperatures from 2500 to 50,000 K and perturber densities 1011 cm−3 and 1013 cm−3. The influence of the temperature and the role of the perturbers (electrons, protons and He+ ions) on the Stark width and shift have been discussed. Results could be useful for plasma diagnostics in astrophysics, laboratory, and industrial plasmas. Full article
(This article belongs to the Special Issue Astronomy in the Big Data Era: Perspectives)
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9 pages, 2103 KiB  
Data Descriptor
Stark Broadening of Co II Lines in Stellar Atmospheres
by Zlatko Majlinger, Milan S. Dimitrijević and Vladimir A. Srećković
Data 2020, 5(3), 74; https://doi.org/10.3390/data5030074 - 27 Aug 2020
Cited by 6 | Viewed by 2604
Abstract
Data for Stark full widths at half maximum for 46 Co II multiplets were calculated using a modified semiempirical method. In order to show the applicability and usefulness of this set of data for research into white dwarf and A type star atmospheres, [...] Read more.
Data for Stark full widths at half maximum for 46 Co II multiplets were calculated using a modified semiempirical method. In order to show the applicability and usefulness of this set of data for research into white dwarf and A type star atmospheres, the obtained results were used to investigate the significance of the Stark broadening mechanism for Co II lines in the atmospheres of these objects. We examined the influence of surface gravity (log g), effective temperature and the wavelength of the spectral line on the importance of the inclusion of Stark broadening contribution in the profiles of the considered Co II spectral lines, for plasma conditions in atmospheric layers corresponding to different optical depths. Full article
(This article belongs to the Special Issue Astronomy in the Big Data Era: Perspectives)
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17 pages, 361 KiB  
Data Descriptor
Forty Years of the Applications of Stark Broadening Data Determined with the Modified Semiempirical Method
by Milan S. Dimitrijević
Data 2020, 5(3), 73; https://doi.org/10.3390/data5030073 - 23 Aug 2020
Cited by 22 | Viewed by 3166
Abstract
The aim of this paper is to analyze the various uses of Stark broadening data for non-hydrogenic lines emitted from plasma, obtained with the modified semiempirical method formulated 40 years ago (1980), which are continuously implemented in the STARK-B database. In such a [...] Read more.
The aim of this paper is to analyze the various uses of Stark broadening data for non-hydrogenic lines emitted from plasma, obtained with the modified semiempirical method formulated 40 years ago (1980), which are continuously implemented in the STARK-B database. In such a way one can identify research fields where they are applied and better see the needs of users in order to better plan future work. This is done by analysis of citations of the modified semiempirical method and the corresponding data in international scientific journals, excluding cases when they are used for comparison with other experimental or theoretical Stark broadening data or for development of the theory of Stark broadening. On the basis of our analysis, one can conclude that the principal applications of such data are in astronomy (white dwarfs, A and B stars, and opacity), investigations of laser produced plasmas, laser design and optimization and their applications in industry and technology (ablation, laser melting, deposition, plasma during electrolytic oxidation, laser micro sintering), as well as for the determination of radiative properties of various plasmas, plasma diagnostics, and investigations of regularities and systematic trends of Stark broadening parameters. Full article
(This article belongs to the Special Issue Astronomy in the Big Data Era: Perspectives)
13 pages, 9401 KiB  
Data Descriptor
A Multi-Annotator Survey of Sub-km Craters on Mars
by Alistair Francis, Jonathan Brown, Thomas Cameron, Reuben Crawford Clarke, Romilly Dodd, Jennifer Hurdle, Matthew Neave, Jasmine Nowakowska, Viran Patel, Arianne Puttock, Oliver Redmond, Aaron Ruban, Damien Ruban, Meg Savage, Wiggert Vermeer, Alice Whelan, Panagiotis Sidiropoulos and Jan-Peter Muller
Data 2020, 5(3), 70; https://doi.org/10.3390/data5030070 - 3 Aug 2020
Cited by 7 | Viewed by 4802
Abstract
We present here a dataset of nearly 5000 small craters across roughly 1700 km2 of the Martian surface, in the MC-11 East quadrangle. The dataset covers twelve 2000-by-2000 pixel Context Camera images, each of which is comprehensively labelled by six annotators, whose [...] Read more.
We present here a dataset of nearly 5000 small craters across roughly 1700 km2 of the Martian surface, in the MC-11 East quadrangle. The dataset covers twelve 2000-by-2000 pixel Context Camera images, each of which is comprehensively labelled by six annotators, whose results are combined using agglomerative clustering. Crater size-frequency distributions are centrally important to the estimation of planetary surface ages, in lieu of in-situ sampling. Older surfaces are exposed to meteoritic impactors for longer and, thus, are more densely cratered. However, whilst populations of larger craters are well understood, the processes governing the production and erosion of small (sub-km) craters are more poorly constrained. We argue that, by surveying larger numbers of small craters, the planetary science community can reduce some of the current uncertainties regarding their production and erosion rates. To this end, many have sought to use state-of-the-art object detection techniques utilising Deep Learning, which—although powerful—require very large amounts of labelled training data to perform optimally. This survey gives researchers a large dataset to analyse small crater statistics over MC-11 East, and allows them to better train and validate their crater detection algorithms. The collection of these data also demonstrates a multi-annotator method for the labelling of many small objects, which produces an estimated confidence score for each annotation and annotator. Full article
(This article belongs to the Special Issue Astronomy in the Big Data Era: Perspectives)
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