Search

In this study, it was aimed to reveal the relationship between high school students’ music listening habits and their attitudes towards intangible cultural heritage elements. The research sample consists of 353 students studying at Isparta Süleyman Demirel Science High School. Research data were collected with a structured questionnaire. In the first part of the structured questionnaire consisting of three parts, there are questions to determine gender and grade, in the second part there are questions to determine the music listening habits of the students, and in the last part there is the Intangible Cultural Heritage Attitude Scale, the validity and reliability study of which was conducted by Gürel and Çetin (2019). The analyses within the scope of construct validity of the measurement tool were made and evaluated to be appropriate. In addition, as a result of the reliability analysis applied to the entire scale, Cronbach’s Alpha result was calculated as .871. Independent samples t-test and one-factor analysis of variance (ANOVA) were used to analyse the data obtained from the research. According to the results of the analyses, when the music listening habits of high school students and their attitudes towards intangible cultural heritage elements were examined, it was determined that there was no significant relationship according to gender, grade level, music listening tool, frequency of allocating special time for music listening and Turkish lyrics of music. In addition, it was determined that there was a significant difference between the type of music students listened to and their attitudes towards intangible cultural heritage elements.

For solar-like oscillators, the asteroseismic relations connect the stellar mean density and surface gravity to observable properties of the oscillations. Since the space missions CoRoT and Kepler, the asteroseismic relations have been massively employed out of their theoretical domain of validity, that is the main-sequence solar-type stars, in particular for red giant stars. However, despite a surprisingly good performance of the asteroseismic relation with red giant stars, they are biased and attempts to parametrize the departure of the relations for evolved stars have been the subject of many recent efforts. In this study, we propose a new parametrization of the asteroseismic relations for red giants of radii up to ${\sim } 50\, \mathrm{R}_\odot$, based on a calibration performed with Gaia parallax data. We find that the asteroseismic scaling relations depend on metallicity and effective temperature. For this solution, we obtain a parallax offset of about −0.026 ± 0.001 mas, and radius ranges from 3.8 to 53.2 R⊙. Most stars have masses that range from 0.9 to 1.7 M⊙, with the star count peaking around 1.2 M⊙. We also use data of the eclipsing binaries with solar-like oscillating components for calibration and discuss the diagnostic potential of the mass–metallicity diagram for our understanding of the evolution of red giants and the chemodynamics of the Galactic disc. Using this diagram, we identify stars that lost and gained mass and estimate the minimum change in mass.

Milli Eğitim Bakanlığının 2023 vizyonunda vurgulanan 21. Yüzyıl becerilerinin eğitim programlarında yer alması hususundan hareketle 21. yüzyıl becerilerinin Müzik Dersi Öğretim Programı’nda ne derecede yer bulduğunun ortaya koyulması önem arz etmektedir. Bu araştırma ile 2018 yılında yenilenmiş olan Müzik Dersi Öğretim Programı’ndaki (İlkokul-Ortaokul) kazanımların, 21. Yüzyıl becerilerine uygunluğunun incelenmesi amaçlanmıştır. Araştırma nitel araştırma yöntemleri doğrultusunda oluşturulmuştur. Çalışmada kullanılan veriler doküman incelemesi yapılarak elde edilmiştir. Araştırmada Müzik Dersi Öğretim Programı’nda yer alan kazanımların tamamı içerik analizine tabi tutulmuştur. İçerik analizi yapılırken kazanımların P21’in çerçevesinde yer alan ana beceriler ve bu ana becerilerin içesinde yer alan alt becerilere uygunluğu dikkate alınmıştır. Bu bağlamda tüm sınıflar düzeyinde toplam 179 kazanım, Müzik Dersi Öğretim Programındaki öğrenme alanları ekseninde alt temalara ayrılmıştır ve incelenmiştir. Araştırma sonucunda müzik dersi öğretim programında yer alan kazanımların 21. Yüzyıl becerilerini yeterli düzeyde yansıtmadığı ve becerilerin kazanımlara dağılımında her hangi bir dengenin gözetilmediği belirlenmiştir.

Asteroseismology of bright stars has become increasingly important as a method to determine the fundamental properties (in particular ages) of stars. The Kepler Space Telescope initiated a revolution by detecting oscillations in more than 500 main-sequence and subgiant stars. However, most Kepler stars are faint and therefore have limited constraints from independent methods such as long-baseline interferometry. Here we present the discovery of solar-like oscillations in alpha Men A, a naked-eye (V = 5.1) G7 dwarf in TESS's southern continuous viewing zone. Using a combination of astrometry, spectroscopy, and asteroseismology, we precisely characterize the solar analog alpha Men A (T-eff = 5569 +/- 62 K, R-star = 0.960 +/- 0.016 R-circle dot, M-star = 0.964 +/- 0.045 M-circle dot). To characterize the fully convective M dwarf companion, we derive empirical relations to estimate mass, radius, and temperature given the absolute Gaia magnitude and metallicity, yielding M-star = 0.169 +/- 0.006 M (circle dot), R-star = 0.19 +/- 0.01 R-circle dot, and T-eff = 3054 +/- 44 K. Our asteroseismic age of 6.2 +/- 1.4 (stat) +/- 0.6 (sys) Gyr for the primary places alpha Men B within a small population of M dwarfs with precisely measured ages. We combined multiple ground-based spectroscopy surveys to reveal an activity cycle of P = 13.1 +/- 1.1 yr for alpha Men A, a period similar to that observed in the Sun. We used different gyrochronology models with the asteroseismic age to estimate a rotation period of similar to 30 days for the primary. Alpha Men A is now the closest (d = 10 pc) solar analog with a precise asteroseismic age from space-based photometry, making it a prime target for next-generation direct-imaging missions searching for true Earth analogs., National Science Foundation under the Graduate Research Fellowship Program [DGE 1842402]; Alfred P. Sloan Foundation; National Aeronautics and Space Administration [80NSSC18K1585, 80NSSC19K0379]; National Science Foundation [AST-1717000]; NASA FINESST award [80NSSC19K1424]; MICINN project [PRPPID2019-108709GBI00]; Independent Research Fund Denmark [7027-00096B]; Carlsberg Foundation [CF19-0649, CF17-0760]; Australian Research Council [DP210103119]; UK Science and Technology Facilities Council (STFC) [ST/R0023297/1]; PLATO CNES grant; GOLF CNES grant; Danish National Research Foundation [DNRF106]; Spanish Ministry of Science and Innovation; Ramon y Cajal fellowship [RYC-201517697]; NASA [80NSSC20K0458, 80NSSC20K0515]; XSEDE [TG-AST090107]; NSF [ACI-1663696, AST1716436, PHY-1748958]; NASA Exoplanet Exploration Program; [PID2019-107187GB-I00], We acknowledge the traditional owners of the land on which the Anglo-Australian Telescope stands, the Gamilaraay people, and pay our respects to elders past, present, and emerging. The authors would like to thank the staff at the Gemini South Observatory for follow-up observations. A.C. acknowledges support from the National Science Foundation under the Graduate Research Fellowship Program (DGE 1842402). D.H. acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC18K1585, 80NSSC19K0379), and the National Science Foundation (AST-1717000). T.A.B. acknowledges support from a NASA FINESST award (80NSSC19K1424). A.S. is partially supported by MICINN project PRPPID2019-108709GBI00. V.S.A. acknowledges support from the Independent Research Fund Denmark (research grant 7027-00096B) and the Carlsberg Foundation (grant agreement CF19-0649). T.R.B. acknowledges support from the Australian Research Council (DP210103119). W.H.B., W.J.C., and M.B.N. thank the UK Science and Technology Facilities Council (STFC) for support under grant ST/R0023297/1. R.A.G. acknowledges the support of the PLATO and GOLF CNES grants. M.S.L. is supported by the Carlsberg Foundation (grant agreement No. CF17-0760). Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (grant DNRF106). S.M. acknowledges support from the Spanish Ministry of Science and Innovation with Ramon y Cajal fellowship No. RYC-201517697 and from grant No. PID2019-107187GB-I00. T.S.M. acknowledges support from NASA grant 80NSSC20K0458. Computational time at the Texas Advanced Computing Center was provided through XSEDE allocation TG-AST090107. R.H. D.T. acknowledges support from NSF grants ACI-1663696, AST1716436, and PHY-1748958 and NASA grant 80NSSC20K0515. Some of the observations in the paper made use of the highresolution imaging instrument Zorro obtained under Gemini LLP proposal No. GN/S-2021A-LP-105. Zorro was funded by the NASA Exoplanet Exploration Program and built at the NASA AMES Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium).Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

Celik Orhan, Zeynep/0000-0002-9424-2339; KAYHAN, Cenk/0000-0001-9198-2289, WOS: 000496926900003, Planets and planet candidates are subjected to great investigation in recent years. in this study, we analyse 20 planet and planet-candidate host stars at different evolutionary phases. We construct stellar interiormodels of the host stars with the MESA e.volution code and obtain their fundamental parameters under influence of observational asteroseismic and non-asteroseismic constraints. Model mass range of the host stars is 0.74-1.55 M-circle dot. the mean value of the so-called large separation between oscillation frequencies and its variation about the minima shows the diagnostic potential of asteroseismic properties. Comparison of variations of model and observed large separations versus the oscillation frequencies leads to inference of fundamental parameters of the host stars. Using these parameters, we revise orbital and fundamental parameters of 34 planets and four planet candidates. According to our findings, radius range of the planets is 0.35-16.50 R-circle plus. the maximum difference between the transit and revised radii occurs for Kepler-444b-f is about 25 per cent.

Müzik eğitiminde ders işleme sürecinin verimli ve etkili olmasında öğretmenin çalgı kullanımı önem taşımaktadır. Öğretmenler bu süreçte eğitimini aldıkları çalgıların yanı sıra görev yaptıkları okul, bölge ve sosyo-kültürel koşullar doğrultusunda çeşitli çalgılardan faydalanmaktadırlar. Son yıllarda Türkiye’de bir öğretmen çalgısı olarak Ukulele nin kullanımı yaygınlaşmaktadır. Bu çalışma ile Ukulele nin yapısal özellikleri ve müzik eğitiminde kullanılabilirliğine ilişkin özelliklerinin belirlenmesi amaçlanmıştır. Alan yazın taraması ile ulaşılabilen kaynaklar temel alınarak Ukulele nin hem yapısal olarak hem de müzik eğitimi sürecindeki rolü incelenmiştir.

Asteroseismology using space-based telescopes is vital to our understanding of stellar structure and evolution. {\textit{CoRoT}}, {\textit{Kepler}}, and {\textit{TESS}} space telescopes have detected large numbers of solar-like oscillating evolved stars. %(kaynaklar, Kallinger, vb ). Solar-like oscillation frequencies have an important role in the determination of fundamental stellar parameters; in the literature, the relations between the two is established by the so-called scaling relations. % These scaling relations are in better agreement with mass and radius of main-sequence stars with large separation ($\Delta\nu$) and frequency of maximum amplitude (${\nu_{\rm max}}$). In this study, we analyse data obtained from the observation of 15 evolved solar-like oscillating stars using the {\textit{Kepler}} and ground-based %\textit{CoRoT} telescopes. The main purpose of the study is to determine very precisely the fundamental parameters of evolved stars by constructing interior models using asteroseismic parameters. We also fit the reference frequencies of models to the observational reference frequencies caused by the He {\scriptsize II} ionization zone. The 15 evolved stars are found to have masses and radii within ranges of $0.79$-$1.47$ $M_{\rm sun}$ and $1.60$-$3.15$ $R_{\rm sun}$, respectively. Their model ages range from $2.19$ to $12.75$ Gyr. %Using a number of methods based on conventional and modified scaling relations and evolutionary models constructed with using the {\small {MESA}} code, we determine stellar radii, masses and ages. It is revealed that fitting reference frequencies typically increase the accuracy of asteroseismic radius, mass, and age. The typical uncertainties of mass and radius are $\sim$ 3-6 and $\sim$ 1-2 per cent, respectively. Accordingly, the differences between the model and literature ages are generally only a few Gyr.

The Transiting Exoplanet Survey Satellite (TESS) is recording short-cadence, high duty-cycle timeseries across most of the sky, which presents the opportunity to detect and study oscillations in interesting stars, in particular planet hosts. We have detected and analysed solar-like oscillations in the bright G4 subgiant HD 38529, which hosts an inner, roughly Jupiter-mass planet on a 14.3d orbit and an outer, low-mass brown dwarf on a 2136 d orbit. We combine results frommultiple stellarmodelling teams to produce robust asteroseismic estimates of the star's properties, including its mass M = 1.48 +/- 0.04 M-circle dot, radius R = 2.68 +/- 0.03 R-circle dot, and age t = 3.07 +/- 0.39 Gyr. Our results confirm that HD 38529 has a mass near the higher end of the range that can be found in the literature and also demonstrate that precise stellar properties can be measured given shorter timeseries than produced by CoRoT, Kepler, or K2., UK Science and Technology Facilities Council (STFC)UK Research & Innovation (UKRI)Science & Technology Facilities Council (STFC) [ST/R0023297/1]; Danish National Research FoundationDanmarks Grundforskningsfond [DNRF106]; grant FPI-SO from the Spanish Ministry of Economy and Competitiveness (MINECO) [SEV-2015-0548-17-2, BES-2017-082610]; Spanish Ministry with the Ramon y Cajal fellowship [RYC-2015-17697]; NASANational Aeronautics & Space Administration (NASA) [NNX17AF27G, NNX16AI09G, 80NSSC19K0374]; TESS GI Program under NASA [80NSSC18K1585, 80NSSC19K0385]; Carlsberg FoundationCarlsberg Foundation [CF19-0649]; Independent Research Fund Denmark [7027-00096B]; Alexander von Humboldt Foundation at the Max-Planck-Institut fur Astrophysik; national funds through Fundacao para a Ciencia e Tecnologia (FCT); FCT/MCTES through national funds (PIDDAC) [UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/30389/2017]; Fundo Europeu de Desenvolvimento Regional (FEDER) through COMPETE2020: Programa Operacional Competitividade e Internacionalizacao [POCI01-0145-FEDER-030389]; European Union's Horizon 2020 research and innovation programme under the H2020 Marie Sklodowska-Curie Actions grant [792848]; Scientific and Technological Research Council of TurkeyTurkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK) [TUBITAK:118F352]; NASA Explorer ProgramNational Aeronautics & Space Administration (NASA); PLATO-CNES grant, WHB, WJC, and MBN thank the UK Science and Technology Facilities Council (STFC) for support under grant ST/R0023297/1. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant DNRF106). LGC thanks the support from grant FPI-SO from the Spanish Ministry of Economy and Competitiveness (MINECO; research project SEV-2015-0548-17-2 and predoctoral contract BES-2017-082610). SM acknowledges support from the Spanish Ministry with the Ramon y Cajal fellowship number RYC-2015-17697. ARGS acknowledges the support from NASA under grant NNX17AF27G. RAG acknowledges the support of the PLATO-CNES grant. DLB acknowledges support from the TESS GI Program under NASA awards 80NSSC18K1585 and 80NSSC19K0385. JRM acknowledges support from the Carlsberg Foundation (grant CF19-0649). VSA acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B). BN acknowledges postdoctoral funding from the Alexander von Humboldt Foundation taken at the Max-Planck-Institut fur Astrophysik. MSC and MD are supported in the form of work contracts funded by national funds through Fundacao para a Ciencia e Tecnologia (FCT). MSC and MD acknowledge support by FCT/MCTES through national funds (PIDDAC) by grants UIDB/04434/2020, UIDP/04434/2020, and PTDC/FIS-AST/30389/2017 and by Fundo Europeu de Desenvolvimento Regional (FEDER) through COMPETE2020: Programa Operacional Competitividade e Internacionalizacao by grant POCI01-0145-FEDER-030389. TC acknowledges support from the European Union's Horizon 2020 research and innovation programme under the H2020 Marie Sklodowska-Curie Actions grant 792848 (PULSATION). SB acknowledges NASA grants NNX16AI09G and 80NSSC19K0374. ZCO, MY, and SO acknowledge the Scientific and Technological Research Council of Turkey (TUBITAK:118F352) This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by the NASA Explorer Program. Calculations in this paper had used the University of Birmingham's BlueBEAR High-Performance Computing service.1

Most previous efforts to calibrate how rotation and magnetic activity depend on stellar age and mass have relied on observations of clusters, where isochrones from stellar evolution models are used to determine the properties of the ensemble. Asteroseismology employs similar models to measure the properties of an individual star by matching its normal modes of oscillation, yielding the stellar age and mass with high precision. We use 27 days of photometry from the Transiting Exoplanet Survey Satellite to characterize solar-like oscillations in the G8 subgiant of the 94 Aqr triple system. the resulting stellar properties, when combined with a reanalysis of 35 yr of activity measurements from the Mount Wilson HK project, allow us to probe the evolution of rotation and magnetic activity in the system. the asteroseismic age of the subgiant agrees with a stellar isochrone fit, but the rotation period is much shorter than expected from standard models of angular momentum evolution. We conclude that weakened magnetic braking may be needed to reproduce the stellar properties, and that evolved subgiants in the hydrogen shell-burning phase can reinvigorate large-scale dynamo action and briefly sustain magnetic activity cycles before ascending the red giant branch., NSFNational Science Foundation (NSF) [AST-1812634]; NASANational Aeronautics & Space Administration (NASA) [NNX17AF27G, NNX16AB97G, 80NSSC20K0458, 80NSSC19K0374]; Visiting Fellowship at the Max Planck Institute for Solar System Research; NASA through the TESS Guest Investigator Program [80NSSC18K1584, 80NSSC18K1585, 80NSSC19K0379]; NASA through the Living With A Star Program [NNX16AB76G]; TESS GI Program [80NSSC18K1585, 80NSSC19K0385]; UK Space Agency; Danish National Research FoundationDanmarks Grundforskningsfond [DNRF106]; NCAR Advanced Study Program Postdoctoral FellowshipNational Science Foundation (NSF)NSF - Directorate for Geosciences (GEO); National Science FoundationNational Science Foundation (NSF); CNES PLATO grant; German Aerospace Center (Deutsches Zentrum fur Luft- und Raumfahrt) under PLATO Data Center [50OO1501]; European Research Council (ERC)European Research Council (ERC) [715947]; Programme de Physique Stellaire et Planetaire; Australian Research CouncilAustralian Research Council; Spanish Ministry of Economy and Competitiveness (MINECO) [SEV-2015-0548-17-2, BES-2017-082610]; State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU); European Social Fund via the Lithuanian Science Council (LMTLT)Research Council of Lithuania (LMTLT) [09.3.3-LMT-K-712-01-0103]; ESA PRODEX program; Spanish Ministry with the Ramon y Cajal fellowship [RYC-2015-17697]; Scientific and Technological Research Council of TurkeyTurkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK) [TuBTAK:118F352], T.S.M. acknowledges support from NSF grant AST-1812634, NASA grants NNX16AB97G and 80NSSC20K0458, and a Visiting Fellowship at the Max Planck Institute for Solar System Research. Computational time at the Texas Advanced Computing Center was provided through XSEDE allocation TG-AST090107. J.v.S. acknowledges support from NASA through the TESS Guest Investigator Program (80NSSC18K1584). S.B. acknowledges NASA grant 80NSSC19K0374. D.B. acknowledges support from NASA through the Living With A Star Program (NNX16AB76G) and from the TESS GI Program under awards 80NSSC18K1585 and 80NSSC19K0385. W.J.C., W.H.B. and M.B.N. acknowledge support from the UK Space Agency. Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation (grant agreement No.: DNRF106). R.E. was supported by the NCAR Advanced Study Program Postdoctoral Fellowship. the National Center for Atmospheric Research is sponsored by the National Science Foundation. R.A.G. and B.M. acknowledge support from the CNES PLATO grant. P.G. acknowledges funding from the German Aerospace Center (Deutsches Zentrum fur Luft- und Raumfahrt) under PLATO Data Center grant 50OO1501. D.H. acknowledges support from NASA through the TESS Guest Investigator Program (80NSSC18K1585, 80NSSC19K0379). T.R. acknowledges support from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 715947). T.A. acknowledges support from the Programme de Physique Stellaire et Planetaire. T.R.B. acknowledges support from the Australian Research Council. L.G.C. acknowledges support from grant FPI-SO from the Spanish Ministry of Economy and Competitiveness (MINECO) (research project SEV-2015-0548-17-2 and predoctoral contract BES-2017-082610). A.J. Acknowledges support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU). H.K. acknowledges support from the European Social Fund via the Lithuanian Science Council (LMTLT) grant No. 09.3.3-LMT-K-712-01-0103. M.N.L. acknowledges support from the ESA PRODEX program. S.M. acknowledges support from the Spanish Ministry with the Ramon y Cajal fellowship number RYC-2015-17697. Z.C.O., S.o. and M.Y. acknowledge support from the Scientific and Technological Research Council of Turkey (TuBTAK:118F352). A.R.G.S. acknowledges support from NASA grant NNX17AF27G. This work benefited from discussions within the international team "The Solar and Stellar Wind Connection: Heating processes and angular momentum loss" at the International Space Science Institute (ISSI).

Orhan, Zeynep Celik/0000-0002-9424-2339; Serenelli, Aldo/0000-0001-6359-2769; Monteiro, Mario J. P. F. G./0000-0003-0513-8116; Huber, Daniel/0000-0001-8832-4488; Adibekyan, Vardan/0000-0002-0601-6199; Reffert, Sabine/0000-0002-0460-8289; Stock, Stephan/0000-0002-1166-9338; Stassun, Keivan/0000-0002-3481-9052; Cunha, Margarida/0000-0001-8237-7343; Kuszlewicz, James/0000-0002-3322-5279; Lund, Mikkel Norup/0000-0001-9214-5642; Mathur, Savita/0000-0002-0129-0316; Nielsen, Martin Bo/0000-0001-9169-2599; Mosser, Benoit/0000-0002-7547-1208; Pereira, Filipe/0000-0002-2157-7146; Lucas, Miles/0000-0001-6341-310X; miglio, andrea/0000-0001-5998-8533; Ball, Warrick/0000-0002-4773-1017; Basu, Sarbani/0000-0002-6163-3472; Veras, Dimitri/0000-0001-8014-6162; Handberg, Rasmus/0000-0001-8725-4502; Christensen-Dalsgaard, Jorgen/0000-0001-5137-0966; Delgado Mena, Elisa/0000-0003-4434-2195, WOS: 000498546800001, The Transiting Exoplanet Survey Satellite (TESS) is performing a near all-sky survey for planets that transit bright stars. in addition, its excellent photometric precision enables asteroseismology of solar-type and red-giant stars, which exhibit convection-driven, solar-like oscillations. Simulations predict that TESS will detect solar-like oscillations in nearly 100 stars already known to host planets. in this paper, we present an asteroseismic analysis of the known red-giant host stars HD;212771 and HD;203949, both systems having a long-period planet detected through radial velocities. These are the first detections of oscillations in previously known exoplanet-host stars by TESS, further showcasing the mission?s potential to conduct asteroseismology of red-giant stars. We estimate the fundamental properties of both stars through a grid-based modeling approach that uses global asteroseismic parameters as input. We discuss the evolutionary state of HD;203949 in depth and note the large discrepancy between its asteroseismic mass (M-* = 1.23 0.15 MM* = 1.00 0.16 M if in the clump) and the mass quoted in the discovery paper (M-* = 2.1 0.1 M), implying a change >30% in the planet?s mass. Assuming HD;203949 to be in the clump, we investigate the planet?s past orbital evolution and discuss how it could have avoided engulfment at the tip of the red-giant branch. Finally, HD;212771 was observed by K2 during its Campaign 3, thus allowing for a preliminary comparison of the asteroseismic performances of TESS and K2. We estimate the ratio of the observed oscillation amplitudes for this star to be, NASA Explorer ProgramNational Aeronautics & Space Administration (NASA); ESA PRODEXEuropean Space Agency [PEA 4000119301]; Stellar Astrophysics Centre (SAC) - Danish National Research Foundation [DNRF106]; European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grantEuropean Union (EU) [792848, 664931]; FCT/MCTESPortuguese Foundation for Science and Technology [UID/FIS/04434/2019]; FCTPortuguese Foundation for Science and Technology [PTDC/FIS-AST/30389/2017, PTDC/FIS-AST/28953/2017, PTDC/FIS-AST/32113/2017, CEECIND/02619/2017, IF/00650/2015/CP1273/CT0001, IF/00028/2014/CP1215/CT0002]; FEDER through COMPETE2020 [POCI-01-0145-FEDER-030389, POCI-01-0145-FEDER-028953, POCI-01-0145-FEDER-032113]; National Science Foundation under the Kavli Institute for Theoretical Physics program "Better Stars, Better Planets" [NSF PHY-1748958]; European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant [338251]; ESA PRODEX programme; CNES through the PLATO grants; Spanish GovernmentSpanish Government [ESP2017-82674-R]; Generalitat de CatalunyaGeneralitat de Catalunya [2017-SGR-1131]; STFC via an Ernest Rutherford Fellowship [ST/P003850/1]; NSFNational Science Foundation (NSF) [AST-1514676]; NASANational Aeronautics & Space Administration (NASA) [NNX16AI09G]; Spanish Ministry through the Ramon y Cajal fellowship [RYC-2015-17697]; NYUAD Institute [G1502]; DFGGerman Research Foundation (DFG) [SPP 1992, RE 2694/5-1]; Scientific and Technological Research Council of TurkeyTurkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK) [TUBITAK:118F352]; National Aeronautics and Space Administration through the TESS Guest Investigator Program [80NSSC18K1585, 80NSSC19K0379]; European Social Fund via the Lithuanian Science Council [09.3.3-LMT-K-712-01-0103], This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. Funding for the TESS Asteroseismic Science Operations Center at Aarhus University is provided by ESA PRODEX (PEA 4000119301) and Stellar Astrophysics Centre (SAC), funded by the Danish National Research Foundation (Grant agreement No.: DNRF106). the project leading to this publication has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No..792848 (PULSATION). This work was supported by FCT/MCTES through national funds (UID/FIS/04434/2019). This work was supported by FCT through national funds (PTDC/FIS-AST/30389/2017, PTDC/FIS-AST/28953/2017, and PTDC/FIS-AST/32113/2017) and by FEDER through COMPETE2020 (POCI-01-0145-FEDER-030389, POCI-01-0145-FEDER-028953, and POCI-01-0145-FEDER-032113). This research was supported in part by the National Science Foundation under grant No.NSF PHY-1748958 through the Kavli Institute for Theoretical Physics program "Better Stars, Better Planets". the research leading to the presented results has received funding from the European Research Council under the European Community's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No..338251 (StellarAges). E.C.is funded by the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No..664931. M.N.L.acknowledges support from the ESA PRODEX programme. B.M.and R.A.G. acknowledge the support received from CNES through the PLATO grants. A. S.is partially supported by grants ESP2017-82674-R (Spanish Government) and 2017-SGR-1131 (Generalitat de Catalunya). D.V.gratefully acknowledges the support of the STFC via an Ernest Rutherford Fellowship (grant ST/P003850/1). V. A.and S.G.S. acknowledge support from FCT through Investigador FCT contracts No..IF/00650/2015/CP1273/CT0001 and No..IF/00028/2014/CP1215/CT0002, respectively. S. B. acknowledges NSF grant AST-1514676 and NASA grant NNX16AI09G. S.M..acknowledges support from the Spanish Ministry through the Ramon y Cajal fellowship No. RYC-2015-17697. M.B.N..acknowledges support from NYUAD Institute grant G1502. S.R..acknowledges support from the DFG priority program SPP 1992 "Exploring the Diversity of Extrasolar Planets (RE 2694/5-1)". M.Y., Z.C.O., and S. O. acknowledge the Scientific and Technological Research Council of Turkey (TUBITAK:118F352). D.H. acknowledges support by the National Aeronautics and Space Administration (80NSSC18K1585, 80NSSC19K0379) awarded through the TESS Guest Investigator Program. M.S.C. is supported in the form of a work contract funded by FCT (CEECIND/02619/2017). H.K. acknowledges support from the European Social Fund via the Lithuanian Science Council grant No. 09.3.3-LMT-K-712-01-0103.

Tez çalışmamızda Bulgar edebiyatının Türkiye'de yer alma süreci tarihsel çerçevede neden ve sonuçlarıyla incelenmiştir. Geçmişten günümüze çevrilen kitapların sayısının Türkiye ve Bulgaristan'daki toplumsal ve kültürel tablolardan etkilendiği görülmüştür. Bu sebeple, çeviri süreci, bahsi geçen olayların yarattığı etkiye göre on ya da yirmi yılı kapsayan dönemler halinde ele alınmıştır. Çalışmanın birinci bölümünde Türkiye'deki çeviri faaliyetlerinin seyrine göz atılmış, çevirinin Türkiye'deki etkisi tartışılmıştır. İkinci bölümde Bulgar edebiyatının Türkiye'de ilgi uyandıran özellikleri belirtilerek, ülkemizde yer alma süreci ve ilk çevirilere değinilmiştir. Üçüncü bölümden itibaren çalışmanın ana konusunu oluşturan her iki ülkedeki tarihsel seyrin çeviriye etkisi, karşılaştırmalı olarak her bölümde ele alınmış, çeviri kitap verileri analiz edilmiş ve ulaşılan bulgunun neden ve sonuçları üzerinde durulmuştur. Bölüm başlıkları kronolojik bir çerçevede sunulmuştur. Elde edilen veriler, yıl, tür, yazar ya da çevirmen tercihi açısından bulunduğu dönemin etkisi dikkate alınarak sınıflandırılmış ve değerlendirilmiştir. Ayrıca, yapılan çevirilerin Türk okuyucusunda nasıl bir etki yarattığı tartışılmıştır. Çalışmanın sonuç kısmında, ulaşılan bulgular değerlendirilmiş ve Bulgarcadan çeviri faaliyetlerinin seyri konusunda önerilerde bulunulmuştur. In this study, the process of Bulgarian Literature's taking place in Turkey has been analyzed via its causes and results through a historical perspective. It has been observed that the number of the translated books from the past to present are affected from the communal and cultural cases in Turkey and Bulgaria. For this reason, the translation process has been handled in ten or twenty year periods according to the effects created by the mentioned cases. In the first part of the study, the process of the translation activities in Turkey has been investigated and the effects of the translation in Turkey have been discussed. The characteristics of the Bulgarian literature that are of interest in Turkey have been defined and the process of Bulgarian literature's taking place in our country and the first translations have been investigated in the second chapter. From the third chapter, the effects of the historical course in two countries to the translation process, which is the main subject of this study, have been handled in a comparative way, the translated books datas have been analyzed and the reasons and the results of the obtained data have been emphasized in each chapter. The headlines of each part have been presented in a chronological frame. The obtained data has been categorized and evaluated in terms of year, genre, writer or the translators' choice. Furthermore, the effects of the tarnslations on Turkish readers have been discussed. At the conclusion part of this study, the obtained data has been evaluated and some suggestions on the course on translations from Bulgarian have been given. 177

Recently, our understanding of the origin of W UMa-type contact binaries has become clearer. Initial masses of their components were successfully estimated by Y{\i}ld{\i}z and Do\u{g}an using a new method mainly based on observational properties of overluminous secondary components. In this paper, we continue to discuss the results and make computations for age and orbital evolution of these binaries. It is shown that the secondary mass, according to its luminosity, also successfully predicts the observed radius. While the current mass of the primary component is determined by initial masses, the current secondary mass is also a function of initial angular momentum. We develop methods to compute the age of A- and W-subtype W UMa-type contact binaries {in terms of} initial masses and mass according to the luminosity of the secondaries. Comparisons of our results with the mean ages from kinematic properties of these binaries and data pertaining to contact binaries in open and globular clusters, have increased our confidence on this method. The mean ages of both A- and W-subtype contact binaries are found as 4.4 and 4.6 Gyr, respectively. From kinematic studies, these ages are given as 4.5 and 4.4 Gyr, respectively. We also compute orbital properties of A-subtype contact binaries at the time of the first overflow. Initial angular momentum of these binaries is computed by comparing them with the well-known detached binaries. The angular momentum loss rate derived in the present study for the detached phase is in very good agreement with the semi-empirical rates available in the literature. In addition to the limitations on the initial masses of W UMa-type contact binaries, it is shown that the initial period of these binaries is less than about 4.45 d., Comment: 11 pages and 10 figures. MNRAS 2013

Bu araştırmanın amacı ilkokul 3. sınıf müzik dersi kazanımlarının gerçekleştirilmesinde kullanılan şarkı dağarcığına ilişkin mevcut durumu belirlemek, yeni bir şarkı dağarcığı oluşturarak bu şarkı dağarcığının öğrenme-öğretme sürecindeki etkililiğini anlamak ve öğretimin niteliğini geliştirmeye katkı sunmaktır. Araştırma nitel araştırma desenlerinden eylem araştırması şeklinde tasarlanmıştır. Araştırmanın uygulaması 2013-2014 öğretim yılı Bahar Döneminde Isparta İli Merkez İlçesinde bulunan Öğretmenler İlkokulu 3/C sınıfındaki 30 öğrenci ve sınıf öğretmeninin katılımı ile gerçekleştirilmiştir. Eylem planını; araştırmacının kazanımlara göre bestelediği şarkılar, ders planları ve şarkıların kayıtları oluşturmaktadır. Araştırma çerçevesinde eylem planı 27.03.2014 - 21.05.2014 tarihleri arasındaki toplam 8 haftada ve müzik derslerinde uygulanmıştır.Araştırma verileri doküman incelemesi, kişisel bilgi formları, yarı yapılandırılmış görüşmeler, öğrenci, öğretmen ve araştırmacı günlükleri, video ve ses kayıtları ve derecelenmiş puanlama anahtarından oluşan veri toplama araçları kullanılarak elde edilmiştir. Yarı yapılandırılmış görüşmelerin ses kaydı ve uygulama derslerinin video kayıtlarının çözümlemesinde bilgisayar destekli nitel veri analiz programı olan `QSR-Nvivo 10` kullanılmıştır. Nitel verilerin analizi betimsel analiz ve içerik analizi ile gerçekleştirilmiş ve elde edilen bulgular araştırma soruları doğrultusunda yorumlanmıştır. Araştırmada sonuç olarak, İlkokul 3. Sınıf Müzik Dersi Öğretmen Kılavuz Kitabı'nın incelenmesi sonucunda Müzik Dersi Öğretim Programı'nda önerilen 5E Öğrenme Modeli'ne ilişkin örnek uygulamalar ile öğrenme-öğretme süreci içerisinde yer verilen etkinlik ve kavramlara ilişkin yeterince açıklama ve örnek uygulamaya yer verilmediği belirlenmiştir. Bununla birlikte, öğrenme-öğretme sürecinde kullanılan şarkıların kazanımlarla örtüştüğü, kitabın değerlendirme alanının ise sınırlı olduğu tespit edilmiştir. Uygulamadan önceki müzik derslerinde sadece şarkı söyleme etkinliklerine yer verildiği, uygulamalarda ders kazanımlarına odaklanılmadığı, öğrencilerin şarkıları hatırladıkları ancak müzik dersi kazanımlarına ulaşamadıkları belirlenmiştir. Uygulama süreci ve sonrasında, derslerin eylem planları doğrultusunda yürütüldüğü, öğretmenin ders kazanımı farkındalığının arttığı, öğrencilerin bu süreçte kazanımlara göre hazırlanan şarkı dağarcığı ile müzik derslerinde verilmek istenen ders kazanımlarına ulaşabildiği görülmüştür. Ayrıca, uygulama sürecinde öğrencilerin şarkı kayıtları ile söyleme, dinleme, çalma ve birliktelik becerilerinin geliştiği, besteleme ve seslendirme alanlarına karşı farkındalık kazandığı tespit edilmiştir.Anahtar Sözcükler: Eylem araştırması, sınıf öğretmeni, 5E modeli, ilkokulda müzik eğitimi, kazanımlar, şarkılar. The purpose of this research is to determine the current situation regarding the song repertoire used in the realizationed of the achievements of the primary school 3rd grade music lessons. It is designed to understand the effectiveness of this repertoire in the learning-teaching process by creating a new song repertoire, and to contribute to improving the quality of teaching. As the study entailed the solution of the problem, it was designed as qualitative action research. The research was carried out with the participation of 30 students and the classroom teacher of 3/C class in Teachers Primary School in the central district of Isparta Province in the spring term of the 2013-2014 academic year. The action plan contained the songs that the researcher composed according to the achievements, the lesson plans and the records of the songs. The action plan was practised in music lessons for a total of 8 weeks between March 27, 2014 and May 21, 2014.Research data were obtained by using data collection tools including document review, personal information forms, semi-structured interviews, the diaries of student, teacher and researcher, video and audio recordings, and graded scoring key. `QSR-Nvivo 10`, a computer-aided qualitative data analysis program, was used to analyze of the audio recording of semi-structured interviews and the video recordings of application lessons. The analysis of qualitative data was actualisationed by descriptive analysis and content analysis, and the findings were interpreted hrough research questions. As a result of examining the Primary School 3rd Grade Music Lesson Teacher's Guide Book, it has been determined that sample exercises related to 5E learning model recommended in Music Lesson Curriculum and sufficient explanation and sample exercises about activities and concepts included in learning-teaching process are not included. It was also determined that the songs used in the learning-teaching process overlap with the outcomes and that the evaluation area of the book is limited. It was determined that music lessons before the practice included only singing activities in the lessons and that students did not focus on lesson acquisition at the implementation, and that the students remembered the songs but did not reach the goals of the music lesson. During the implementation process and afterwards, it is seen that the lessons are carried out in accordance with the action plans and that the teacher has increased awareness of course acquisition and that the students can reach the desired goals to be given in music lessons with song repertoire prepared according to their achievements. At the same time, during the implementation process, it was determined that the students' skills of singing with recordings of songs, listening, playing and collaborating with their peers were developed and that students gained awareness of composition and performing fields. Key words: Action research, classroom teachers, 5E model, music education in primary school, outcomes, songs. 343

WOS: 000288702600007, Binary systems, in particular eclipsing binaries, are essential sources of knowledge of the fundamental properties of stars. The ages of binaries, members of open clusters, are constrained by their own fundamental properties and by those of the hosting cluster. The ages of eleven open clusters are here found by constructing models for the components of twelve eclipsing binaries. The difference between the ages we find and the ages of the clusters derived from isochrone fitting is up to 40%. For the binary system V497 Cep in NGC 7160, the difference is about 100%. Binary systems whose primary component is about to complete its main-sequence lifetime, such as V453 Cyg and V906 Sco, are the most suitable systems for age determination. Using model results for these stars, we derive an expression for sensitive and uncomplicated relative age determination of binary systems (age divided by the main-sequence lifetime of the primary star). The expression is given as a logarithm of radii ratio divided by a logarithm of mass ratio. Two advantages of this expression are that: (i) it is nearly independent of the assumed chemical composition of the models because of the appearance of the ratio of radii; and (ii) the ratios of radii and masses are observationally much more precise than their absolute values. We also derive another expression using luminosities rather than radii and compare results., Scientific and Technological Research Council of Turkey (TUBITAK)Turkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK), This work is supported by the Scientific and Technological Research Council of Turkey (TUBITAK).

Putting their chemically peculiarities aside, Ap and Am stars have many common properties. The discriminating property between them could be the rotation of their interiors beneath their slowly rotating surface. In the PV Cas (HD 240208) binary system whose light curve shows Ap-like variation, the agreement between the theoretical and observed apsidal advance rate is satisfied only with differentially rotating models of the component stars in which rapid rotation is extended almost to the surface. Thus, it seems that there is a steep rotation rate gradient near the surface of the Ap stars. The conclusion we reach in the analysis of PV Cas system leads us to introduce the effective mass as a new conceptual tool in stellar astrophysics: $M_{\rm eff}= M_\star (1-\bar{\Lambda})^{1.75}$ , where $M_\star$ and $\bar{\Lambda}$ are mass of the star and average of ratio of centrifugal to the gravitational acceleration throughout the model, respectively. We find that the effective mass of PV Cas A whose true mass is $2.82\pm 0.05\,M_\odot$ is $2.6\,M_\odot$ for both solar and metal rich compositions. To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Grids of stellar evolution are required in many fields of astronomy/astrophysics, such as planet hosting stars, binaries, clusters, chemically peculiar stars, etc. In this study, a grid of stellar evolution models with updated ingredients and recently determined solar abundances is presented. The solar values for the initial abundances of hydrogen, heavy elements and mixing-length parameter are 0.0172, 0.7024 and 1.98, respectively. The mass step is small enough (0.01 M-circle dot) that interpolation for a given star mass is not required. The range of stellar mass is 0.74 to 10.00 M-circle dot. We present results in different forms of tables for easy and general application. The second stellar harmonic, required for analysis of apsidal motion of eclipsing binaries, is also listed. We also construct rotating models to determine the effect of rotation on stellar structure and derive fitting formulae for luminosity, radius and the second harmonic as a function of rotational parameter. We also compute and list colors and bolometric corrections of models required for transformation between theoretical and observational results. The results are tested for the Sun, the Hyades cluster, the slowly rotating chemically peculiar Am stars and eclipsing binaries with apsidal motion. The theoretical and observational results along isochrones are in good agreement. The grids are also applicable to rotating stars provided that equatorial velocity is given.

WOS: 000344141500013, Recently the number of main-sequence and subgiant stars exhibiting solar-like oscillations that are resolved into individual mode frequencies has increased dramatically. While only a few such data sets were available for detailed modeling just a decade ago, the Kepler mission has produced suitable observations for hundreds of new targets. This rapid expansion in observational capacity has been accompanied by a shift in analysis and modeling strategies to yield uniform sets of derived stellar properties more quickly and easily. We use previously published asteroseismic and spectroscopic data sets to provide a uniform analysis of 42 solar-type Kepler targets from the Asteroseismic Modeling Portal. We find that fitting the individual frequencies typically doubles the precision of the asteroseismic radius, mass, and age compared to grid-based modeling of the global oscillation properties, and improves the precision of the radius and mass by about a factor of three over empirical scaling relations. We demonstrate the utility of the derived properties with several applications., NASANational Aeronautics & Space Administration (NASA) [NNX13AC44G, NNX13AE91G]; White Dwarf Research Corporation through the Pale Blue Dot project; Danish National Research FoundationDanmarks Grundforskningsfond [DNRF106]; European Research CouncilEuropean Research Council (ERC) [267864]; Scientific and Technological Research Council of TurkeyTurkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK) [TUBITAK:112T989]; European Commission grant for the SPACEINN project [FP7-SPACE-2012-312844]; NSF Astronomy and Astrophysics postdoctoral fellowshipNational Science Foundation (NSF) [AST 09-02004]; NSFNational Science Foundation (NSF) [PHY 08-21899, PHY 11-25915]; Investigador FCT contract - FCT/MCTES (Portugal); POPH/FSE (EC)European Commission Joint Research CentreEuropean Social Fund (ESF); Hungarian OTKAOrszagos Tudomanyos Kutatasi Alapprogramok (OTKA) [K83790, KTIA URKUT_10-1-2011-0019]; Lendulet Young Researchers Programme of the Hungarian Academy of Sciences; Janos Bolyai Research Scholarship of the Hungarian Academy of SciencesHungarian Academy of Sciences; City of Szombathely [S-11-1027]; European Community Seventh Framework Programme (FP7) [269194 (IRSES/ASK)]; CNES grant at CEA-Saclay; NIUS programme of HBCSE (TIFR); MICINN grant [AYA2011-24704]; ESF EUROCORES Program EuroGENESIS (MICINN) [EUI2009-04170]; Australian Research CouncilAustralian Research Council; Science and Technology Facilities CouncilScience & Technology Facilities Council (STFC) [ST/J001163/1], We would like to thank Victor Silva Aguirre for helpful discussions. This work was supported in part by NASA grants NNX13AC44G and NNX13AE91G, and by White Dwarf Research Corporation through the Pale Blue Dot project (http://whitedwarf.org/palebluedot/). Computational time on Kraken at the National Institute of Computational Sciences was provided through XSEDE allocation TG-AST090107. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (grant DNRF106). We acknowledge the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement No.: 267864), the Scientific and Technological Research Council of Turkey (TUBITAK:112T989), and a European Commission grant for the SPACEINN project (FP7-SPACE-2012-312844). B.P.B. was supported in part by NSF Astronomy and Astrophysics postdoctoral fellowship AST 09-02004. C.M.S.O. is supported by NSF grant PHY 08-21899 and K.I.T.P. is supported by NSF grant PHY 11-25915. M.S.C. is supported by an Investigador FCT contract funded by FCT/MCTES (Portugal) and POPH/FSE (EC). A.D. has been supported by the Hungarian OTKA grants K83790, KTIA URKUT_10-1-2011-0019 grant, the Lendulet-2009 Young Researchers Programme of the Hungarian Academy of Sciences, the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences and the City of Szombathely under agreement No. S-11-1027. A.D. and R.A.G. acknowledge the support of the European Community Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 269194 (IRSES/ASK). R.A.G. and D. Salabert acknowledge the support of the CNES grant at CEA-Saclay. A.M. acknowledges support from the NIUS programme of HBCSE (TIFR). A.S. is supported by the MICINN grant AYA2011-24704 and by the ESF EUROCORES Program EuroGENESIS (MICINN grant EUI2009-04170). D. Stello is supported by the Australian Research Council.

WOS: 000346963300084, It is already stated in the previous studies that the radius of the giant planets is affected by stellar irradiation. The confirmed relation between radius and incident flux depends on planetary mass intervals. In this study, we show that there is a single relation between radius and irradiated energy per gram per second (l(-)), for all mass intervals. There is an extra increase in radius of planets if l(-) is higher than 1100 times energy received by the Earth (l(circle plus)). This is likely due to dissociation of molecules. The tidal interaction as a heating mechanism is also considered and found that its maximum effect on the inflation of planets is about 15 per cent. We also compute age and heavy element abundances from the properties of host stars, given in the TEPCat catalogue (Southworth 2011). The metallicity given in the literature is as [Fe/H]. However, the most abundant element is oxygen, and there is a reverse relation between the observed abundances [Fe/H] and [O/Fe]. Therefore, we first compute [O/H] from [Fe/H] by using observed abundances, and then find heavy element abundance from [O/H]. We also develop a new method for age determination. Using the ages we find, we analyse variation of both radius and mass of the planets with respect to time, and estimate the initial mass of the planets from the relation we derive for the first time. According to our results, the highly irradiated gas giants lose 5 per cent of their mass in every 1 Gyr., Scientific and Technological Research Council of TurkeyTurkiye Bilimsel ve Teknolojik Arastirma Kurumu (TUBITAK) [TUBITAK: 112T989], The anonymous referee is acknowledged for suggestions which improved the presentation of the manuscript. This work is supported by the Scientific and Technological Research Council of Turkey (TUBITAK: 112T989).

WOS: 000319260500041, W UMa type binaries have two defining characteristics. These are (i) the effective temperatures of both components are very similar, and (ii) the secondary (currently less massive) component is overluminous for its current mass. We consider the latter to be an indication of its mass before the mass transfer event. For these stars, we define a mass difference (delta M) between the mass determined from its luminosity and the present mass determined from fitting the binary orbit. We compare the observed values of the mass difference to stellar models with mass-loss. The range of initial secondary masses that we find for observed W UMa type binaries is 1.3-2.6 M-circle dot. We discover that the A- and the W-subtype contact binaries have different ranges of initial secondary masses. Binary systems with an initial mass higher than 1.8 +/- 0.1 M-circle dot become A-subtype while systems with initial masses lower than this become W-subtype. Only 6 per cent of systems violate this behaviour. We also obtain the initial masses of the primaries using the following constraint for the reciprocal of the initial mass ratio: 0 < 1/q(i) < 1. The range of initial masses we find for the primaries is 0.2-1.5 M-circle dot, except for two systems. Finally in comparing our models to observed systems, we find evidence that the mass transfer process is not conservative. We find that only 34 per cent of the mass from the secondary is transferred to the primary. The remainder is lost from the system.

WOS: 000301297500010, The evolved solar-type stars 16 Cyg A and B have long been studied as solar analogs, yielding a glimpse into the future of our own Sun. The orbital period of the binary system is too long to provide meaningful dynamical constraints on the stellar properties, but asteroseismology can help because the stars are among the brightest in the Kepler field. We present an analysis of three months of nearly uninterrupted photometry of 16 Cyg A and B from the Kepler space telescope. We extract a total of 46 and 41 oscillation frequencies for the two components, respectively, including a clear detection of octupole (l = 3) modes in both stars. We derive the properties of each star independently using the Asteroseismic Modeling Portal, fitting the individual oscillation frequencies and other observational constraints simultaneously. We evaluate the systematic uncertainties from an ensemble of results generated by a variety of stellar evolution codes and fitting methods. The optimal models derived by fitting each component individually yield a common age (t = 6.8 +/- 0.4 Gyr) and initial composition (Z(i) = 0.024 +/- 0.002, Y-i = 0.25 +/- 0.01) within the uncertainties, as expected for the components of a binary system, bolstering our confidence in the reliability of asteroseismic techniques. The longer data sets that will ultimately become available will allow future studies of differential rotation, convection zone depths, and long-term changes due to stellar activity cycles., NASA's Science Mission Directorate; NASANational Aeronautics & Space Administration (NASA) [NNX09AE59G]; National Science FoundationNational Science Foundation (NSF) [NSF PHY05-51164]; Science and Technology Facilities CouncilScience & Technology Facilities Council (STFC) [ST/J001163/1], Funding for this Discovery mission is provided by NASA's Science Mission Directorate. This work was supported in part by NASA grant NNX09AE59G. Computational time on Kraken at the National Institute of Computational Sciences was provided through NSF TeraGrid allocation TG-AST090107. We acknowledge the KITP staff at UCSB for their warm hospitality during the research program "Asteroseismology in the Space Age." This research was supported in part by the National Science Foundation under Grant No. NSF PHY05-51164. The authors thank Jeff Hall, Todd Henry, Dave Soderblom, and Russel White for helpful discussions, as well as the entire Kepler team, without whom these results would not be possible. We also thank all funding councils and agencies that have supported the activities of the Kepler Asteroseismic Science Consortium Working Group 1, including the Pale Blue Dot Project hosted by White Dwarf Research Corporation (http://whitedwarf.org/palebluedot/).

WOS: 000287194100010, We present initial results on some of the properties of open clusters NGC 6791 and NGC 6819 derived from asteroseismic data obtained by NASA's Kepler mission. In addition to estimating the mass, radius, and log g of stars on the red giant branch (RGB) of these clusters, we estimate the distance to the clusters and their ages. Our model-independent estimate of the distance modulus of NGC 6791 is (m - M)(0) = 13.11 +/- 0.06. We find (m - M)(0) = 11.85 +/- 0.05 for NGC 6819. The average mass of stars on the RGB of NGC 6791 is 1.20 +/- 0.01 M-circle dot, while that of NGC 6819 is 1.68 +/- 0.03 M-circle dot. It should be noted that we do not have data that cover the entire RGB and the actual mass will be somewhat lower. We have determined model-dependent estimates of ages of these clusters. We find ages between 6.8 and 8.6 Gyr for NGC 6791, however, most sets of models give ages around 7 Gyr. We obtain ages between 2 and 2.4 Gyr for NGC 6819., NASA's Science Mission Directorate; Science and Technology Facilities CouncilScience & Technology Facilities Council (STFC) [ST/F002041/1], Funding for the Kepler mission is provided by NASA's Science Mission Directorate. The authors wish to thank the entire Kepler team, without whom these results would not be possible. We also thank all funding councils and agencies that have supported the activities of Working Group 2 of the Kepler Asteroseismic Science Consortium.

Calculation of equation of state in stellar interiors becomes difficult as contained gas deviates from perfect gas. We present a method for the calculation of electron pressure in terms of density and temperature in the presence of degeneracy. The method is applicable forT

Bu araştırma, Resmi ve Özel Kurumlara Bağlı Çocuk Koroları profilini belirlemek amacıyla yapılmıştır.Araştırmada; gerekli nitel verileri toplamak için kaynak tarama, alt problemlere ilişkin verileri toplamak için ise bu korolarda eğitim almakta olan çocukların anne ve babalarına anket uygulanmıştır. Ayrıca, çocuk korolarının olanaklarını ve şeflerin profilini belirlemek için görüşme yöntemi uygulanmıştır. Anket uygulamaları frekans (f) ve yüzde (%) değerlerinden oluşan tablolarla ortaya konulmuştur, görüşme verileri ise betimsel analiz yöntemi kullanılarak şekillerle sergilenmiştir.Araştırmanın örneklemi, T.C Kültür ve Turizm Bakanlığı Devlet Çoksesli Çocuk Korosu*(Türkiye Çocukları ve Melodi ), TRT Ankara Çocuk Korosu*( Üretim ve Hazırlık), TPKD Çocuk Korosu, SCA Müzik Vakfı JM Çocuk Korosu, Hacettepe Çocuk Korosu ve Başkent Üniversitesi Çocuk Korosu ve bu korolarda eğitim alan çocukların ailelerinden seçilerek oluşturulmuştur.Sonuç olarak, anne- baba profili çoğunlukla orta yaş grubunda, bir üniversite mezunu, ekonomik olarak orta düzeyde ve müzikle amatör olarak ilgilenen bireyler olarak belirlenmiştir. Bu korolarda eğitim alan çocukların çoğunluğunu kızların oluşturduğu 7-14 yaş aralığında olan çocuklar olduğu, bu eğitimin çocuklar tarafından severek yapıldığı için uzun zaman sürdürüldüğü, çocukların çoğunlukla spor, resim, dans, tiyatro gibi çeşitli sosyal etkinliklerde de yer aldığı belirlenmiştir. Bu koroların olanaklarının genel olarak çalışma mekânı olarak elverişli olduğu, çoğunlukla yardımcı şef ve piyano eşlikçileri ile birlikte çalıştıkları, koronun giderlerinin genellikle kurum ve aile tarafından karşılandığı ve yılda en az bir defa konser verdikleri belirlenmiştir. Bu korolarda görev yapan koro şeflerinin ise üniversitelerin müzikle ilgili bölüm ve anabilim dallarından mezun oldukları ve çoğunlukla lisansüstü eğitimi aldıkları ayrıca çocuk korolarında uzun yıllardır görev yaptıkları belirlenmiştir. This research aims to determine the general profile of child choirs that are related to official and private authorities.In the research; a literature review was done to collect the needed qualitative data, as to collect data that are related to the sub-problems, a survey was applied to children?s parents who are taking charge in these choirs. In addition, to determine the profiles of child choirs and their conductors an interview method was applied. Surveys were performed in the form of tables consisting of frequency (f) and percentage (%), as for interview data, by using descriptive analysis they were displayed in the form of shapes.A sample of the research was set by separating out from Turkish of Republic Ministry of Culture and Tourism State Polyphonic Child Choir*(Turkish Children and Melody), TRT Ankara Child Choir*(Production and Preparation), TPKD (The Turkish Polyphonic Choir Association) Child Choir, SCA (Sevda Cenap And) Music Foundation JM Child Choir, Hacettepe Child Choir, Başkent University Child Choir and parents of children that are taking in charge of these choirs.As a result, the profile of mother-father was determined that the persons are mostly middle-aged, are graduated from a university, have middle-income and are interested in music as dabble. It is determined that the most of the children who are taking charge in these choirs are girls and their ages are between 7 and 14, the taking charge in these choirs has a long time because of to be liked by the children, the most of the children also participate various social activities such as sports, drawing, dancing and drama. It was also determined that the opportunities of the choirs generally are sufficient as a workplace, the choirs mostly work with an assistant conductor and piano accompanist, the expenses of the choir usually have met by the authority and families, the choir has given least a concert in a year. It was determined that the conductors, who work in the choirs, are graduated from universities? departments relevant to music and they have mostly master degree and also they have worked in children choirs over many years. 77

252nd Symposium of the International-Astronomical-Union -- APR 06-11, 2008 -- Sanya, PEOPLES R CHINA, WOS: 000263138600033, Mixing length parameter of the mixing length theory is a free parameter and used to calibrate radii of late-type stars. From the Hyades cluster and the alpha Centauri system, we find that the parameter depends on the stellar mass and some other properties of stars. Considering some other systems, we describe how the parameter depends on stellar parameters., Int Astron Union, Natl Nat Sci Fdn China, Chinese Acad Sci, Natl Astron Observatories

The small separation (delta nu 01, delta nu 02 and delta nu 13) between the oscillations with low degree l is dependent primarily on the sound speed profile within the stellar core, where nuclear evolution occurs. The detection of such oscillations for a star offers a very good opportunity to determine the stage of its nuclear evolution, and hence its age. In this context, we investigate the Sun and alpha Cen A and B. For alpha Cen A and B, each of the small separations delta nu 01, delta nu 02 and delta nu 13 gives a different age. Therefore, in our fitting process, we also employ the second difference, defined as nu n2 - 2 nu n1 + nu n0, which is 2 delta nu 01- delta nu 02. In addition to this, we also use frequency ratio (nu n0/ nu n2). For the Sun, these expressions areequivalent and give an age of about 4.9-5.0 Gyr. For alpha Cen A and B, however, the small separation and the second difference give very different ages. This conflict may be solved by the detection of oscillation frequencies that can be measured much more precisely than the current frequencies. When we fit the models to the observations, we find (i) Z 0=0.020, t=3.50 Gyr and M B=1.006 Msun from the small separations delta nu 01, delta nu 02 and delta nu 13 of alpha Cen B; and (ii) a variety of solutions from the non-seismic constraints and delta nu 02 of alpha Cen A and B, in which the masses of alpha Cen A and B are slightly modified and the age of the system is about 5.2-5.3 Gyr. For Z=0.025, the closest masses we find to the observed masses are M B=0.922 Msun and M A=1.115 Msun.The differences between these masses and the corresponding observed masses are about 0.01 Msun., Comment: 9 Pages and 9 Figures

The $\alpha$ Cen binary system is a well-known stellar system with very accurate observational constraints to structure of its component stars. In addition to the classical non-seismic constraints, there are also seismic constraints for the interior models of $\alpha$ Cen A and B. These two types of constraint give very different values for the age of the system. While we obtain 8.9 Gyr for the age of the system from the non-seismic constraints, the seismic constraints imply that the age is about 5.6-5.9 Gyr. There may be observational or theoretical reasons for this discrepancy, which can be found by careful consideration of similar stars. The $\alpha$ Cen binary system, with its solar type components, is also suitable for testing the stellar mass dependence of the mixing-length parameter for convection derived from the binaries of Hyades. The values of the mixing-length parameter for $\alpha$ Cen A and B are 2.10 and 1.90 for the non-seismic constraints. If we prioritize to the seismic constraints, we obtain 1.64 and 1.91 for $\alpha$ Cen A and B, respectively. By taking into account of these two contrasting cases for stellar mass dependence of the mixing-length parameter, we derive two expressions for its time dependence, which are also compatible with the mass dependence of the mixing-length parameter derived from the Hyades stars. For assessment, these expressions should be tested in other stellar systems and clusters., Comment: 8 pages, 6 figures, to be published in MNRAS

WOS: 000237812700040, We present our findings based on a detailed analysis of the binaries of the Hyades, in which the masses of the components are well known. We fit the models of the components of a binary system to observations so as to give the observed total V and B-V of that system and the observed slope of the main sequence in the corresponding parts. According to our findings, there is a very definite relationship between the mixing-length parameter and the stellar mass. The fitting formula for this relationship can be given as alpha = 9.19 (M/M-circle dot-0.74)(0.053)-6.65, which is valid for stellar masses greater than 0.77 M-circle dot. While no strict information is gathered for the chemical composition of the cluster, as a result of degeneracy in the colour-magnitude diagram, by adopting Z = 0.033 and using models for the components of 70 Tau and theta(2) Tau we find the hydrogen abundance to be X = 0.676 and the age to be 670 Myr. If we assume that Z = 0.024, then X = 0.718 and the age is 720 Myr. Our findings concerning the mixing-length parameter are valid for both sets of the solution. For both components of the active binary system V818 Tau, the differences between radii of the models with Z = 0.024 and the observed radii are only about 4 per cent. More generally, the effective temperatures of the models of low-mass stars in the binary systems studied are in good agreement with those determined by spectroscopic methods.

WOS: 000232659500024, In this study, we show that only models with differential rotation, as opposed to non-rotation or solid-body rotation for the components of PV Cas, are in satisfactory agreement with the observations ( including constraints on the apsidal advance rate and the synchronous rotation of the components in addition to their luminosities and radii). Internal rotation profiles found for solar and metal-rich chemical compositions are similar to each other in that only a small part of the outermost regions is rotating very slowly ( v(eq) similar to 65 km s(-1)) and the rest is rotating very rapidly. Confirmation of Ap-like variations in the light curve of the system leads us to search for a connection between this type ( and similar types) of internal rotation and chemically peculiar stars. The temperature difference between the blue sides of the main sequence for the normal and for the magnetic Ap stars may arise from such a connection, since we find a similar difference between the models with this kind of rotation and the non-rotating models of somewhat lower mass.

WOS: 000185534000033, In this study we propose to explain the discrepancy between classical models and the observational data of early type stars in eclipsing binaries by the existence of a rapidly rotating core in the primary, rather than by invoking a low metal abundance. Our claim is based on the analysis of the double lined eclipsing binary EK Cep, on which a strong constraint is put by its apsidal motion. We constructed models both with and without rotation for the components of the system. If the stars do not rotate, then, considering ( i) that both components have the same chemical composition and age, and (ii) that the primary star is exactly at the zero-age main-sequence point, we derive X = 0.614 and Z = 0.04 for respectively the hydrogen and heavy element abundances, with a mixing-length parameter alpha = 1.30, somewhat lower than that calibrated on the Sun. These values satisfy all the observational constraints at the single age of 26 Myr, except the luminosity and radius of the primary, and they are also in good agreement with the observed chemical evolution in the solar neighborhood. Since the observed luminosity and radius of EK Cep A are less than those predicted by a non-rotating model, we deduce that this star must have a rapidly rotating core, while its envelope is synchronized with the orbital motion due to tidal interaction. To achieve perfect agreement between the rotating model of this star and the observations, the requirement is that the central region rotates about 65 times faster than the synchronized envelope, which contains 48% of the star's total mass. We describe the effect of such differential rotation on the location of the star in the HR diagram, and compare it with that of rotation caused by contraction alone. We confirm also that such rapid rotation may account for the spread which is observed in the isochrones of open clusters.

Helioseismic results put very important constraints on structure of the solar models, which can not be reachable by another way. These constraints lead toward what we should do to obtain a solar model in good agreement with the Sun. In this connection, diffusion of chemical elements took its indispensable part in the standard solar models. In this study, we obtained models without diffusion, with diffusion of H only and with diffusion of H and heavy elements. Influence of so-called T—effect in equation of state is also discussed. Since heavy element abundance is not known very accurately, models with various initial heavy element abundance (Z) are also obtained to deduce which Z is appropriate. Relative sound speed difference between the Sun and model with diffusion of H and heavy elements and with Z = 0.02 is not larger than 0.2%.

Eclipsing binary system DI Her has an apsidal motion and its observed apsidal advance seems to be less than even the relativistic advance. Therefore many debates are centered about DI Her, which may also be extended to more or less similar systems showing such a discrepancy between the theory and the observations. Computed value of the apsidal motion rate from the eclipse timings of DI Her, up to now, is very small and about one fourth of the relativistic advance. In this work we show that such a small observed rate is due to use of visual and photographic data having low precision, and due to disregarding the large orbital eccentricity of the system. As a result, we found that the observed apsidal advance is still less than the relativistic advance, but is larger than the previous results by a factor of about two.