New inclination changing eclipsing binaries in the Magellanic Clouds

Context: Multiple stellar systems are unique laboratories for astrophysics. Analysis of their orbital dynamics may reveal invaluable information about the physical properties of the participating stars. Unfortunately, there are only a few known and well described multiple systems, this is even more so for systems located outside the Milky Way galaxy. A particularly interesting situation occurs when the inner binary in a compact triple system is eclipsing. This is because the stellar interaction, typically resulting in precession of orbital planes, may be observable as a variation of depth of the eclipses on a long timescale. Aims: We aim to present a novel method to determine compact triples using publicly available photometric data from large surveys. Here we apply it to eclipsing binaries (EBs) in Magellanic Clouds from OGLE III database. Methods: We analyzed light curves (LCs) of 26121 LMC and 6138 SMC EBs with the goal to identify those for which the orbital inclination varies in time. Archival LCs of the selected systems, when complemented by our own observations with Danish 1.54m telescope, were thoroughly analyzed using the PHOEBE program. Time dependence of the EB's inclination was described using the theory of orbital-plane precession. By observing the parameter-dependence of the precession rate, we were able to constrain the third companion mass and its orbital period around EB. Results: We identified 58 candidates of new compact triples in Magellanic Clouds. This is the largest published sample of such systems so far. Eight of them were analyzed thoroughly and physical parameters of inner binary were determined together with an estimation of basic characteristics of the third star. These data may provide important clues about stellar formation mechanisms for objects with different metalicity than found in our galactic neighborhood.Comment: Accepted for publication in Astronomy and Astrophysic

Time-dependent spectral-feature variations of stars displaying the B[e] phenomenon III. HD 50138

We analyse spectroscopic observations of the B[e] star HD 50138 (MWC 158, V743 Mon, or IRAS 06491-0654), a member of the FS CMa group, obtained over the last twenty years. Four different epochs are identified in the observational data, where the variability of the spectral features is substantially different. Additionally, two long periods of (3 000 +/- 500) and (5 000 +/- 1000) days are found in the variations of the equivalent widths of the H alpha and [OI] 6300 A lines and radial velocities of the H alpha line violet peak. Modest signatures of a regular period of ~34 days in the radial velocities of the H alpha red peak and H beta central depression are found in the season 2013/2014. The H alpha V/R changes indicate a periodicity of ~50 days. The correlations between individual spectral features significantly restricts the model of the object and suggest that it is most likely a binary system with a highly distorted disc with spiral arms around the primary component. At the same time, no obvious signs of the secondary component has been found in the object's spectrum

Učební úlohy ve výuce fyziky na 2. stupni základní školy: vybrané výsledky CPV videostudie fyziky

Učební úlohy představují soubor specifických požadavků kladených na žákovo učení. Z hlediska didaktiky je klíčovou otázka, jaký potenciál mají učební úlohy pro procesy učení. Předkládané výzkumné sdělení je zaměřeno právě tímto směrem. Na základě systematické analýzy videozáznamů 27 vyučovacích hodin fyziky na 2. stupni základní školy je hledána odpověď na otázky: Kolik učebních úloh je řešeno ve vyučovací hodině a v jakém časovém zastoupení? Kolik času zaujímají fáze zadávání, řešení a kontroly úloh? Kdo je řešitelem úloh? Jaký typ řešení úlohy vyžadují? Výsledky ukazují, že práce s učebními úlohami zaujímá 63 % všech posuzovaných sekvencí, což odpovídá přibližně 6 úlohám za jednu vyučovací hodinu. Dále bylo zjištěno, že nejčastěji řeší úlohy učitel v interakci se žáky, nejvíce úloh vyžaduje slovní řešení a nejméně jsou zastoupeny úlohy řešené experimentálně

DIAMOND DEPOSITION ON WC-Co CUTTING TOOLS AFTER PRE-TREATMENT IN REACTIVE SOLUTIONS

We describe the influence of pre-treatment procedures on the adhesion of diamond films to WC-Co substrates. Annealing of substrates at 600˚C in vacuum and repeated etching in different reactive solutions (Al(OH)2-COOH diluted in acetic acid, Murakami and HCl:HNO3) were studied with respect to their effectiveness in suppressing C diffusion into Co on the WCCo surface. Substrates were coated with polycrystalline diamond films by the dual plasma HF CVD method. Raman spectra confirmed the existence of the diamond phase on all samples. Film surface morphology varied with the pre-treatment method used. Adhesion strength was evaluated using the scratch test

First apsidal motion and light curve analysis of 162 eccentric eclipsing binaries from LMC

We present an extensive study of 162 early-type binary systems located in the LMC galaxy that show apsidal motion and have never been studied before. For the ample systems, we performed light curve and apsidal motion modelling for the first time. These systems have a median orbital period of 2.2 days and typical periods of the apsidal motion were derived to be of the order of decades. We identified two record-breaking systems. The first, OGLE LMC-ECL-22613, shows the shortest known apsidal motion period among systems with main sequence components (6.6 years); it contains a third component with an orbital period of 23 years. The second, OGLE LMC-ECL-17226, is an eccentric system with the shortest known orbital period (0.9879 days) and with quite fast apsidal motion period (11 years). Among the studied systems, 36 new triple-star candidates were identified based on the additional period variations. This represents more than 20% of all studied systems, which is in agreement with the statistics of multiples in our Galaxy. However, the fraction should only be considered as a lower limit of these early-type stars in the LMC because of our method of detection, data coverage, and limited precision of individual times of eclipses.Comment: 24 pages, 18 figures, 5 tables, published in 2020A&A...640A..33

Translanguaging in mainstream education:a sociocultural approach

Due to the monolingual self-understanding of European nation-states, migration-induced multilingualism and the language mixing practices it triggers are not usually acknowledged as resources for learning within mainstream classrooms. The term translanguaging has recently been put forward as both a way of describing the flexible ways in which bilinguals draw upon their multiple languages to enhance their communicative potential and a pedagogical approach in which teachers and pupils use these practices for learning. However, little research has been conducted in how the translanguaging approach can be used in mainstream education to enhance knowledge. This study draws on videographic data recorded in 59 10th grade (15-year-olds) subject-matter classes in 4 secondary schools. Applying sociocultural discourse analysis to peer–peer interaction and therefore considering how learners scaffold one another as they participate in collaborative talk and in the co-construction of knowledge, results describe several functions of translanguaging for ‘exploratory talk’ leading to content-matter learning. Multilingual adolescents in naturalistic settings thus use their multilingualism to cognitively engage with content-based tasks and produce high-order speech acts embedded in complex talk

Surprising variations in the rotation of the chemically peculiar stars CU Virginis and V901 Orionis

CU Vir and V901 Ori belong among these few magnetic chemically peculiar stars whose rotation periods vary on timescales of decades. We aim to study the stability of the periods in CU Vir and V901 Ori using all accessible observational data containing phase information. We collected all available relevant archived observations supplemented with our new measurements of these stars and analysed the period variations of the stars using a novel method that allows for the combination of data of diverse sorts. We found that the shapes of their phase curves were constant, while the periods were changing. Both stars exhibit alternating intervals of rotational braking and acceleration. The rotation period of CU Vir was gradually shortening until the year 1968, when it reached its local minimum of 0.52067198 d. The period then started increasing, reaching its local maximum of 0.5207163 d in the year 2005. Since that time the rotation has begun to accelerate again. We also found much smaller period changes in CU Vir on a timescale of several years. The rotation period of V901 Ori was increasing for the past quarter-century, reaching a maximum of 1.538771 d in the year 2003, when the rotation period began to decrease. A theoretically unexpected alternating variability of rotation periods in these stars would remove the spin-down time paradox and brings a new insight into structure and evolution of magnetic upper-main-sequence stars.Comment: 5 pages, 3 figure

Science with a small two-band UV-photometry mission II: Observations of stars and stellar systems

We outline the impact of a small two-band UV-photometry satellite mission on the field of stellar physics, magnetospheres of stars, binaries, stellar clusters, interstellar matter, and exoplanets. On specific examples of different types of stars and stellar systems, we discuss particular requirements for such satellite missions in terms of specific mission parameters such as bandpass, precision, cadence, and mission duration. We show that such a mission may provide crucial data not only for hot stars that emit most of their light in UV, but also for cool stars, where UV traces their activity. This is important, for instance, for exoplanetary studies, because the level of stellar activity influences habitability. While the main asset of the two-band UV mission rests in time-domain astronomy, an example of open clusters proves that such a mission would be important also for the study of stellar populations. Properties of the interstellar dust are best explored when combining optical and IR information with observations in UV. It is well known that dust absorbs UV radiation efficiently. Consequently, we outline how such a UV mission can be used to detect eclipses of sufficiently hot stars by various dusty objects and study disks, rings, clouds, disintegrating exoplanets or exoasteroids. Furthermore, UV radiation can be used to study the cooling of neutron stars providing information about the extreme states of matter in the interiors of neutron stars and used for mapping heated spots on their surfaces.Comment: Submitted to Space Science Review

Quick Ultra-VIolet Kilonova surveyor (QUVIK)

We present a near-UV space telescope on a ~70kg micro-satellite with a moderately fast repointing capability and a near real-time alert communication system that has been proposed in response to a call for an ambitious Czech national mission. The mission, which has recently been approved for Phase 0, A, and B1 study shall measure the brightness evolution of kilonovae, resulting from mergers of neutron stars in the near-UV band and thus it shall distinguish between different explosion scenarios. Between the observations of transient sources, the satellite shall perform observations of other targets of interest, a large part of which will be chosen in open competition.Comment: SPIE Astronomical Telescopes and Instrumentatio