Abstract The method of astronomy homework organization in order to increase students’ cognitive activity is described in the article, as well as the possibility of individualisation and ...differentiation of homework is shown. Modern methods offer a lot of techniques and innovative forms of teaching methods in order to improve students’ knowledge. These innovations are aimed at applying activity-based and person-centered approaches to learning that will help to intensify students’ training activities therefore it will be engaging and productive. Examples of independent practical tasks of different types and use of information and communication technologies are given. The article gives examples of such kinds of work on astronomy classes as: preparation of a textbook, preparation of supporting notes, practical tasks, solution of astronomical problems and creative tasks.
Abstract The development of students’ key competences and their scientific worldview is one of the significant tasks of secondary education. Understanding of the Universe, its objects, structure and ...research methods is an important part of natural and mathematic worldview. Problem-based learning is a relevant form for develop critical thinking during the study of these topics in the course of astronomy. In the conditions of distant learning this can be realized with the help of interactive online platforms whereas practical tasks can be realized through the use of simulators, mobile and computer applications. This will contribute the development of students’ key competences and practical skills. This research offers to emphasize the Universe study and interactive technology use in order to develop research, information and digital competences as well as competences in natural sciences and technologies.
Abstract Modern mobile technologies have become widespread in our lives. All of us use them every day. The use of mobile phones in education is a topical issue too. This paper presents the ...methodological features of the use of mobile technologies in the astronomy’s class. Modern methods offer a lot of techniques and innovative forms of teaching methods in order to improve students’ knowledge. These innovations are aimed to increase using activity-based and person-centered approaches to learning and also, they will help to intensify students’ training activities therefore. The including mobile technology in education process will be engage and productive. We used mobile technologies for the organization of practical tasks from astronomy, as well as the possibility of individualization of education is shown. The such tasks help to increase students’ cognitive activity. It is presented in the article, as an example for astronomy studying, there is example of mobile phone using for the Moon research.
Abstract This paper introduces the Proceedings of the XV International Conference on Mathematics, Science and Technology Education (ICon-MaSTEd 2023), which took place at the Kryvyi Rih State ...Pedagogical University, Ukraine, from 17 to 19 May 2023. It provides background information and the organizational structure of the conference, as well as the structure of the proceedings. It also acknowledges the many people who contributed to the success of the conference.
Analysis of the radial velocities based on spectra of high (near the
H
α
line) and moderate (4420–4960 Å) resolutions supplemented by the published radial velocities has revealed the binarity of a ...bright member of the young open star cluster χ Per, the star V622 Per. The derived orbital elements of the binary show that the lines of both components are seen in its spectrum, the orbital period is 5.2 days, and the binary is in the phase of active mass exchange. The photometric variability of the star is caused by the ellipsoidal shape of its components. Analysis of the spectroscopic and photometric variabilities has allowed the absolute parameters of the binary’s orbit and its components to be found. V622 Per is shown to be a classical Algol with moderate mass exchange in the binary. Mass transfer occurs from the less massive (
M
1
=
9.1
±
2.7
M
⊙
) but brighter (
log
L
1
=
4.52
±
0.10
L
⊙
) component onto the more massive (
M
2
=
13.0
±
3.5
M
⊙
) and less bright (
log
L
2
=
3.96
±
0.10
L
⊙
) component. Analysis of the spectra has confirmed an appreciable overabundance of CNO-cycle products in the atmosphere of the primary component. Comparison of the positions of the binary’s components on the
T
eff
–log
g
diagram with the age of the cluster χ Per points to a possible delay in the evolution of the primary component due to mass loss by no more than 1–2Myr.
Based on high- and medium-resolution spectra, we analyze the population of Be stars in eight young open star clusters. We have found a clear dependence of the relative content of early-type (B0-B3) ...Be stars on the cluster age. The relative concentration of Be stars of spectral types B0–B3 gradually increases with cluster age, reaching its maximum value of 0.46 in clusters with ages of 12–20 Myr. The almost complete absence of Be stars in older clusters can be easily explained by the fact that B stars leave the main sequence. The few emission objects in clusters with ages of 1–7 Myr are most likely Herbig Be stars. Such a distribution of Be stars in clusters unequivocally points to the evolutionary status of the Be phenomenon. We also briefly consider the causes of this pattern.
Abstract
This paper represents a preface to the Proceedings of the XIV International Conference on Mathematics, Science and Technology Education (ICon-MaSTEd 2022) held at the Kryvyi Rih State ...Pedagogical University, Ukraine, 18-20 May 2022. Background information and the organizational structure of the meeting, proceedings structure, and acknowledgments of the contributions of the many people who made the conference a success are presented.
The populations of B and Be-stars in the young open clusters NGC 7419 and NGC 659 are studied. Lowresolution spectral observations in the region of the Hα line are used to study 34 members of NGC ...7419 and additional spectra in the range λ3700-6200 Å are obtained for 12 stars. During the period of our observations, four previously identified Be-stars manifested an absorption profile for the Hα line. Emission in the Hα line is observed in the spectra of 21 objects. The members of the cluster NGC 7419 are classified as to spectral type. The position of the Be-stars on a two-color IR diagram and a comparison with the position of the objects in other clusters with similar ages cast doubt on the existence of two starformation waves. Moderate resolution spectra were obtained for 22 stars in the cluster NGC 659 over wavelengths of λ4050-5200 Å and for 7 objects in the neighborhood of the Hα line. Emission is observed in both the Hα and Hβ lines for two of the five Be-stars that were studied, while faint emission appears only in the Hα line in one of the stars. The other members of the cluster show no signs of emission in these spectra. T
eff
, log g, and Vsini are estimated for the observed stars. It is found that 5 of the objects are not members of the cluster.
(ProQuest: ... denotes formulae and/or non-USASCII text omitted; see image) Analysis of the radial velocities based on spectra of high (near the H alpha line) and moderate (4420-4960 Å) resolutions ...supplemented by the published radial velocities has revealed the binarity of a bright member of the young open star cluster χ Per, the star V622 Per. The derived orbital elements of the binary show that the lines of both components are seen in its spectrum, the orbital period is 5.2 days, and the binary is in the phase of active mass exchange. The photometric variability of the star is caused by the ellipsoidal shape of its components. Analysis of the spectroscopic and photometric variabilities has allowed the absolute parameters of the binary's orbit and its components to be found. V622 Per is shown to be a classical Algol with moderate mass exchange in the binary. Mass transfer occurs from the less massive (...) but brighter (...) component onto the more massive (...) and less bright (...) component. Analysis of the spectra has confirmed an appreciable overabundance of CNO-cycle products in the atmosphere of the primary component. Comparison of the positions of the binary's components on the T eff-log g diagram with the age of the cluster χ Per points to a possible delay in the evolution of the primary component due to mass loss by no more than 1-2Myr.
This is a study of the population of B and Be stars in the young, relatively poor, diffuse stellar clusters NGC 6871 and NGC 6913. High resolution spectra are used to study the Hα line of eleven ...stars in order to detect emission. Emission profiles were found for three stars in the cluster NGC 6871; one of these is a known WR-star and the Be-star BD +35°3956 demonstrates the transition from the B to the Be phase. Spectra of seven of the B stars revealed no traces of emission in the Hα line. During the time of our observations, the Be star V1322 Cyg in the cluster NGC 6913 had a strong emission Hα line profile with substantial variability in intensity and equivalent width. Moderate resolution spectra of seven stars in the cluster NGC 6871 over wavelengths of 4420-4960 Å and ten stars in the cluster NGC 6913 over wavelengths of 4050-5100 Å are used to classify the series of B and Be stars spectrally and to estimate their
T
eff
and log
g
. It was found that three of the stars are not members of the clusters NGC 6871 or NGC 6913.
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