Yazar "Soydugan, Esin" seçeneğine göre listele

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    A binary star with a ? Scuti component
    (Astronomical Soc Pacific, 2007) Soydugan, Esin; Soydugan, Faruk
    New photometric observations of the Algol type binary system RZ Cassiopeiae were obtained in the B and V filters. The new light curves of the system were analyzed using the Wilson-Devinney code. As expected, the light curves of the system exhibit short-period oscillations due to pulsation of the primary component. The computed light curves have been subtracted from the observed ones to obtain the residual light curves. The frequency analysis was performed on the residual light curves using a computer package called PERIOD 04 (Lenz & Breger 2005). As a result of this analysis, we found that the primary component of RZ Cas shows multi-periodic pulsations.
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    A catalogue of chromospherically active binary stars (third edition)
    (Wiley-Blackwell, 2008) Eker, Z.; Ak, N. Filiz; Bilir, S.; Dogru, D.; Tueysuez, M.; Soydugan, Esin; Bakis, H.
    The catalogue of chromospherically active binaries (CABs) has been revised and updated. With 203 new identifications, the number of CAB stars is increased to 409. The catalogue is available in electronic format where each system has a number of lines (suborders) with a unique order number. The columns contain data of limited numbers of selected cross references, comments to explain peculiarities and the position of the binarity in case it belongs to a multiple system, classical identifications (RS Canum Venaticorum, BY Draconis), brightness and colours, photometric and spectroscopic data, a description of emission features (Ca II H and K, H alpha, ultraviolet, infrared), X-ray luminosity, radio flux, physical quantities and orbital information, where each basic entry is referenced so users can go to the original sources.
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    A catalogue of close binaries located in the ? Scuti region of the Cepheid instability strip
    (Oxford Univ Press, 2006) Soydugan, Esin; Soydugan, Faruk; Demircan, O.; Ibanoglu, C.
    A catalogue of close eclipsing binary systems (detached and semidetached) with at least one of the components located in the delta Scuti region of the Cepheid instability strip is presented. The positions of the stars in the instability strip are determined by their accurate temperatures and luminosities. Observationally detected binaries (20 semidetached, four detached and one unclassified) with oscillating components were included in the catalogue as a separate table. The primaries of the oscillating Algols tend to be located near the blue edge of the instability strip. Using reliable luminosities and temperatures determined by recent photometric and spectroscopic studies, we have found that at least one or two components of 71 detached and 90 semidetached systems are located in the delta Scuti region of the Cepheid instability strip. In addition, 36 detached or semidetached systems discovered by the Hipparcos satellite were also given as a separate list. One of their components is seen in the delta Scuti region, according to their spectral type or B - V colours. They are potential candidate binaries with the delta Scuti-type pulsating components which need further photometric and spectroscopic studies in better precision. This catalogue covers information and literature references for 25 known and 197 candidate binaries with pulsating components.
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    A comprehensive photometric study of the Algol-type eclipsing binary: BG Pegasi
    (Elsevier Science Bv, 2011) Soydugan, Esin; Soydugan, Faruk; Senyuz, T.; Puskullu, C.; Demircan, O.
    This study presents new photometric observations of classical Algol type binary BC Peg with a delta Scuti component The light curve modeling was provided with the physical parameters of the component stars in the BC Peg system for the first time After modeling light curves in B and V filters, the eclipse and proximity effects were removed from the light curve to analyze intrinsic variations caused by the hotter component of the system Frequency analysis of the residuals light represents the multi-mode pulsation of the more massive component of the BC Peg system at periods of 0.039 and 0 047 clays Two frequencies could be associated with non-radial (l = 2) modes The total amplitude of the pulsational variability in the V light curve was found to be about 0 045 mag The long-term orbital period variation of the system was also investigated for the first time The O-C analysis indicates periodic variation superimposed on a downward parabola The secular period variation means that the orbital period of the system is decreasing at a rate of -5 5 seconds per century, probably due to the magnetic activity of the cooler component. The tilted sinusoidal O-C variation may be caused by the gravitational effect of an unseen component around the system (C) 2010 Elsevier B V All rights reserved
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    A spectroscopic study of some Algol systems
    (2005) Soydugan, Faruk; Frasca, A.; Catalano, S.; Ibano?lu, C.; Demircan, O.; Soydugan, Esin
    We present and discuss here new high-resolution (R? 22000) optical spectra of three Algol binaries, namely KO Aql, S Equ and AT Peg, obtained with the echelle spectrograph of Catania Astrophysical Observatory. In this work, we obtained new radial velocity curves for the hotter primary components with a much better precision than the previous data in the literature, mainly coming from old plate spectra. Thanks to the cross-correlation procedure, we were able to obtain, for the first time to our knowledge, radial velocities also for the cool secondary components of KO Aql and S Equ. We have also measured, with a rather good accuracy (2-4 km/s), the rotational velocity of the hotter components of these three systems and found that, with the exception of AT Peg, the primary stars are rotating faster than the synchronization velocity, consistently with a mass transfer scenario. In addition, preliminary results on the mass-transfer effects displayed by the H? and H? extra-absorption/emission components are presented.
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    A spectroscopic study of the Algol-type binaries S Equulei and KO Aquilae: absolute parameters and mass transfer
    (Blackwell Publishing, 2007) Soydugan, Faruk; Frasca, A.; Soydugan, Esin; Catalano, S.; Demircan, O.; Ibanoglu, C.
    We present and analyse high-resolution optical spectra of two Algol binaries, namely S Equ and KO Aql, obtained with the echelle spectrograph at Catania Astrophysical Observatory. New accurate radial velocities (RVs) for the hotter primary components are obtained. Thanks to the cross-correlation procedure, we were able to measure, for the first time to our knowledge, RVs also for the cool secondary components of S Equ and KO Aql. By combining the parameters obtained from the solution of the RV curves with those obtained from the light-curve analysis, reliable absolute parameters of the systems have been derived. The rotational velocity of the hotter components of S Equ and KO Aql has been measured and it is found that the gainers of both systems rotate about 30 per cent faster than synchronously. This is likely due to mass transfer across the Lagrangian L-1 point from the cooler to the hotter component. The lower luminosity of the mass-gaining components of these systems compared to normal main-sequence stars of the same mass can also be an effect of the mass transfer. The H alpha profiles were analysed with the 'synthesis and subtraction' technique and reveal clear evidence of mass transfer and accretion structures. In both systems, especially before the primary eclipses and afterwards, we clearly observed extra absorption lines. From the integrated absorption and the RV variations of these features, we found that the mass accretion is very dense around the impact region of the hotter components. A double-peaked emission in the spectra of S Equ was seen outside the eclipses. One of these peaks is likely originated in a region between the centre of mass and the cooler component, which is occupied by the flowing matter. Furthermore, the H alpha difference spectra of S Equ and KO Aql also display emission features, which should be arising from the magnetic activity of the cooler components.
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    A spectroscopic survey of algol-type binary S Equ
    (Astronomical Soc Pacific, 2007) Soydugan, Faruk; Soydugan, Esin; Frasca, A.
    This study presents the results of the medium-resolution optical spectra of S Equ obtained with the echelle spectrograph of the Catania Astro-physical Observatory. In this work, new radial velocity curves for the components of the system with a precision better than in previous works are obtained using the cross-correlation technique. We have determined the absolute parameters of S Equ combining the orbit and light curve solutions. The preliminary results of the Ha line analysis indicate an extra emission and absorption as a likely result of a mass-transfer process and chromospheric activity of the cooler component.
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    An algol type binary with a ? Scuti component
    (Wiley-V C H Verlag Gmbh, 2006) Soydugan, Esin; Soydugan, Faruk; Ibanoglu, C.; Frasca, A.; Demircan, O.; Akan, M. C.
    We present new BV photometry and spectroscopic observations of RZ Cassiopeiae. The light and radial velocity curves were formed by the new observations which have been analyzed simultaneously by using the Wilson-Dewinney code. The non-synchronous rotational velocity v(1) sin i = 76 +/- 6 km s(-1), deduced for the primary component from the new spectroscopic observations, was also incorporated in the analysis. A time-series analysis of the residual light curves revealed the multi-periodic pulsations of the primary component of RZ Cas. The main peak in the frequency spectrum was observed at about 64.197 c d(-1) in both B and V bands. The pulsational constant was calculated to be 0.0116 days. This value corresponds to high overtones (n similar to 6) of non-radial mode oscillations. We find significant changes in the pulsational amplitude of the primary component from year to year. The peak-to-peak pulsational amplitude of the main frequency displays a decrease from 0.(m)-013 in 2000 to 0.(m)002 in 2001 and thereafter we have found an increase again in the amplitude to 0.(m)01 in the year 2002. We propose the mass transfer from the cool secondary to the pulsating primary as a possible explanation for such remarkable changes in the pulsational behavior of the primary component. (c) 2006 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.
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    Analysis of Exoplanet Light Curves
    (Astronomical Soc Pacific, 2015) Erdem, A.; Budding, E.; Rhodes, M. D.; Puskullu, Q.; Soydugan, Faruk; Soydugan, Esin; Tuysuz, M.
    We have applied the close binary system analysis package WINFITTER to a variety of exoplanet transiting light curves taken both from the NASA Exoplanet Archive and our own groundbased observations. WINFITTER has parameter options for a realistic physical model, including gravity brightening and structural parameters derived from Kopal's applications of the relevant Radau equation, and it includes appropriate tests for determinacy and adequacy of its best fitting parameter sets. We discuss a number of issues related to empirical checking of models for stellar limb darkening, surface maculation, Doppler beaming, microvariability, and transit time variation (TTV) effects. The Radau coefficients used in the light curve modeling, in principle, allow structural models of the component stars to be tested.
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    Angular momentum evolution of Algol binaries
    (Oxford Univ Press, 2006) Ibanoglu, C.; Soydugan, Faruk; Soydugan, Esin; Dervisoglu, A.
    We have compiled the well-determined absolute parameters of Algol-type binaries. The lists contain the parameters of 74 detached and 61 semidetached close binaries. The double-lined eclipsing binaries provide not only the most accurate determinations of stellar mass, radius and temperatures but also distance-independent luminosity for each of their individual components. The distributions of the primary and secondary masses of detached binaries (DBs) are similar, whilst the secondary masses of the semidetached binaries (SDBs) are mostly smaller than 2 M-circle dot with a peak in the M-2-bin (0.21-1.0). The components of the DBs are almost all located in the main-sequence band. On the contrary, the secondary components of the SDBs have larger radii and luminosity with respect to the same mass and the same effective temperature of main-sequence counterparts. They occupy a region of the Hertzsprung-Russell diagram between terminal-age main sequence and giants. Moreover, the total angular momenta and specific angular momenta are larger for the SDBs of orbital periods with P > 5 d than those of the shorter period ones. The specific angular momenta of SDBs with periods longer than 5 d are 65 per cent greater than that of the short period group with the same mass. The DBs and the SDBs with orbital periods longer and shorter than 5 d are separated into three groups in the J/M-5/3 - q diagram. The SDBs with mass ratios greater than 0.3 and P > 5 d have almost the same angular momentum to those of DBs. However, the SDBs with short periods have the smallest angular momentum even though they have the same mass ratios. This result reveals that angular momentum loss (AML) considerably affects the evolution of close binary systems. Recently, Chen, Li & Qian suggested that, in addition to magnetic braking, a circumbinary disc may play an important role in AML from Algol-type binaries. Their calculations indicated that the evolution of Algol-type binaries can be significantly affected by the circumbinary disc. Our results show that the evolution of close binaries begins as a DB and losing angular momentum, first via stellar wind and then magnetic braking plus circumbinary disc the period is shortened and orbit shrinks. Thereafter, the evolution of the system is accelerated and mass transfer rates are enhanced which result in a smaller mass ratios.
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    BINARITY AND PULSATION IN ALGOL-TYPE BINARY SYSTEM SX DRACONIS
    (Iop Publishing Ltd, 2013) Soydugan, Esin; Kacar, Y.
    Photometric observations of SX Dra were carried out to determine the properties of the components and pulsational characteristics of the more massive pulsational component. Physical parameters of the component stars were obtained by modeling B and V light curves using the Wilson-Devinney code. Results indicate that SX Dra is a semi-detached system with the secondary component filling its Roche lobe. The O-C data showed parabolic and sinusoidal variation. Cyclic variation in the O-C diagram could be the result of the possible magnetic activity of the secondary component instead of the third body. The secular increase in the orbital period of the system can be interpreted as being the result of mass transfer from the secondary component to the primary one at a rate of 2.1 x 10(-7) M-circle dot yr(-1). Results of a time-series analysis performed after removing binary effects indicated that the hot component shows delta Scuti light variations with pulsational periods of 63 and 73 minutes. Spherical harmonic degrees (l) were determined to be 3 for the first frequency and 1-2 for the second frequency.
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    Çanakkale Onsekiz Mart Üniversitesi Ar-Ge Strateji Belgesi (Astrofizik)
    (2017) Erdem, Ahmet; Erkan, Naci; Soydugan, Esin; Bulut, İbrahim; Bulut, Ahmet; Demircan, Osman
    Çanakkale Onsekiz Mart Üniversitesi (ÇOMÜ)?de astronomi/astrofizik alanındaki tüm bilimsel çalışmalar 2000 yılından itibaren ÇOMÜ Astrofizik Araştırma Merkezi (ÇAAM) bünyesinde örgütlenmiştir (bkz: http://physics.comu.edu.tr/caam/). Üniversite içinde astronomi, astrofizik ve uzay bilimleriyle profesyonel olarak ilgilenen tüm elemanlar bu merkezin üyesidir. Bu gün ÇAAM kurmuş olduğu Gözlemevi ile Marmara Bölgesi?nin astronomi/astrofizik alanında en etkin çalışan merkez konumundadır. Merkezde ulusal ve uluslararası bağlantılı bilimsel araştırmalar yürütülmekte, eleman yetiştirilmekte ve bölge okulları ve halk için bilimtoplum etkinlikleri hizmeti verilmektedir. ÇAAM?da bilimsel araştırmalar, yıldız astrofiziği, güneş ve güneş sistemi, ötegezegenler, yüksek enerji astrofiziği ve kozmoloji alanlarında yoğunlaşmaktadır. ÇAAM üyeleri son on yılda hakemli dergilerde 200?ün üzerinde makale yayınlamış, bilimsel toplantılarda 300?e yakın bildiri sunmuş, 40 kadar bilimsel araştırma projesi yürütmüş, 10?a yakın bilimsel toplantı düzenlemiş veya düzenlenmesine katkı sunmuş, 8 kitapta yazarlık ve editörlük yapılmış, ve 50 kadar yüksek lisans ve doktora tez çalışması yürütmüştür. Gözlemevinde yapılan gözlemlere dayalı çok sayıda bulgu indekslere giren dergilerde yayınlandı. Gözlemevinde tek veya çift yıldız olarak bilinen 30 kadar yıldızın görünmeyen bileşenleri keşfedildi. Merkez üyeleri tarafından yazılan bir ders kitabı Cambridge Üniversitesi yayınları arasında basıldı. Güncel çift yıldız katalogları oluşturuldu. Çift yıldız yörüngelerinin, aşırı açısal momentum kaybı nedeniyle, gittikçe küçüldüğü ve zaman içinde çift yıldızların tek yıldıza dönüştüğü ilk kez ÇAAM üyeleri tarafından kanıtlandı. Yıldız sismolojisinin, yakınında başka bir yıldız olması halinde, o yıldızın kütle çekimine bağlı olduğu gözlemlerle gösterildi. Ülkemizde ilk kez asteroidlerin fotometrik gözlemlerinden şekillerinin modellenmesi çalışmalarına başlandı. Kuramsal kozmolojide quark gluon plazmasıyla ilgili çok önemli yayınlar yapıldı. Çift yıldızların etrafında görünmeyen başka yıldızların bulunabileceği ve bu istatistiğin oldukça yüksek olduğu kanıtlandı. Çift yıldızların etrafında gezegenler olabileceği bu gözlemevinin birçok yayınında not edildi. ÇOMÜ?nün astrofizik/astronomi alanında gelecek 5 yılda izleyeceği stratejisinde nihai hedefi, Astrofizik Araştırma Merkezi ve Ulupınar Gözlemevi?ni uluslararası kabul edilebilir nitelikte, bilimsel araştırmalar yapan, alanında uzman akademisyen yetiştiren, topluma popüler bilim hizmeti veren, teleskop, detektör, kubbe vb gözlem aletleri ve yazılımları konusunda ar-ge yapan bir mükemmeliyet merkezi haline getirmektir. Bu hedefe ulaşılması için izlenilecek adımlar (stratejik amaçlar): (i) Gözlemevi hizmet binasının yenilenmesi, (ii) 1.22 m ayna çaplı teleskop için modern bir tayfçekerin alınması, kurulması ve çalıştırılması, (iii) İstanbul Üniversitesi Fen Fakültesi Astronomi ve Uzay Bilimleri Bölümü ile ortaklaşa kullanılan 60 cm ayna çaplı teleskobun tam robotik hale getirilmesi, (iv) 40 cm ve 30 cm ayna çaplı teleskopların yarı-robotik hale (uzaktan gözlem yapılabilir hale) getirilmesi, (v) Yenilenmesi planlanan hizmet binasında, kütüphane, mutfak, dinlenme ve çalışma odalarının yanı sıra, ar-ge laboratuvarının kurulması, (vi) Astronomi alanında ar-ge için, örneğin ÇAAM üyelerinin ÇOMÜ TeknoPark bünyesinde kurduğu ASTROIA şirketi vb teknoloji şirketleriyle işbirliklerinin/çalışmaların artırılması, (vii) ÇOMÜ Gözlemevi sitesinde bir gezegenevinin (planetaryum) kurulması ve toplum-bilim hizmetlerinin verilmesi.
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    CCD UBV and Gaia DR3 based analysis of NGC 189, NGC 1758 and NGC 7762 open clusters
    (Elsevier Sci Ltd, 2023) Yontan, Talar; Bilir, Selcuk; Cakmak, Hikmet; Raul, Michel; Banks, Timothy; Soydugan, Esin; Canbay, Remziye
    This paper presents photometric, astrometric, and kinematic analyses of the open clusters NGC 189, NGC 1758 and NGC 7762 based on CCD UBV photometric and Gaia Data Release 3 (DR3) data. According to membership analyses, we identified 32, 57 and 106 most probable member stars with membership probabilities P >= 0:5 in NGC 189, NGC 1758 and NGC 7762, respectively. The color excesses and photometric metallicities of each cluster were determined separately using UBV two-color diagrams. The color excess E(B - V) is 0: 590 +/- 0:023 mag for NGC 189, 0:310 +/- 0:022 mag for NGC 1758 and 0:640 +/- 0:017 mag for NGC 7762. The photometric metallicity [Fe/H] is -0:08 +/- 0:03 dex for both NGC 189 and NGC 1758, and -0:12 +/- 0:02 dex for NGC 7762. Distance moduli and ages of the clusters were obtained by comparing PARSEC isochrones with the color-magnitude diagrams constructed from UBV and Gaia photometric data. During this process, we kept as constant color excess and metallicity for each cluster. The estimated isochrone distance is 1201 +/- 53 pc for NGC 189, 902 +/- 33 pc for NGC 1758 and 911 +/- 31 pc for NGC 7762. These are compatible with the values obtained from trigonometric parallax. Ages of the clusters are 500 +/- 50 Myr, 650 +/- 50 Myr and 2000 +/- 200 Myr for NGC 189, NGC 1758 and NGC 7762, respectively. Galactic orbit integration of the clusters showed that NGC 1758 completely orbits outside the solar circle, while NGC 189 and NGC 7762 enter the solar circle during their orbits. (c) 2023 COSPAR. Published by Elsevier B.V. All rights reserved.
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    Delta scuti bileşenli örten çift sistemlerin zonklama özelliklerinin belirlenmesi
    (2011) Soydugan, Esin; Soydugan, Faruk; Bilir, Selçuk; Bakış, Volkan; Demircan, Osman
    [Abstract Not Available]
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    Determination of Atmospheric Parameters of ? Scuti Stars
    (Amer Inst Physics, 2017) Alicavus, F. Kahraman; Soydugan, Esin; Kubat, J.; Kotkova, L.
    Asteroseismology offers an opportunity for examination and detailed understanding of the internal structure of stars by probing their pulsating modes. To obtain reliable results by asteroseismology, accurate atmospheric parameters and metallicities of pulsating stars are required. Hence, in this study we carried out a spectroscopic survey of 8 single delta Scuti stars in detail. The accurate atmospheric parameters (effective temperature, surface gravity), projected rotational velocities and the metallicities of these stars were derived.
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    Discovery of ? scuti type oscillations in two algol-type binaries: DY Aqr and Bg Peg
    (Hungarian Academy of Sciences (Konkoly Observatory), 2009) Soydugan, Esin; Soydugan, Faruk; Enyuz, T.; Puskullu, Q.; Tuysuz, M.; Bakis, V.; Bilir, S.
    [No abstract available]
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    Discovery of {delta} Scuti type oscillations in two Algol-type binaries: DY Aqr and BG Peg
    (2009) Soydugan, Esin; Soydugan, Faruk; Senyüz, T.; Püsküllü, Ç.; Tüysüz, M.; Bakis, V.; Bilir, S.
    [No abstract available]
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    Eclipsing binary stars with a ? Scuti component
    (Oxford Univ Press, 2017) Alicavus, F. Kahraman; Soydugan, Esin; Smalley, B.; Kubat, J.
    Eclipsing binaries with a delta Sct component are powerful tools to derive the fundamental parameters and probe the internal structure of stars. In this study, spectral analysis of six primary delta Sct components in eclipsing binaries has been performed. Values of T-eff, v sin i, and metallicity for the stars have been derived from medium-resolution spectroscopy. Additionally, a revised list of delta Sct stars in eclipsing binaries is presented. In this list, we have only given the d Sct stars in eclipsing binaries to show the effects of the secondary components and tidallocking on the pulsations of primary delta Sct components. The stellar pulsation, atmospheric and fundamental parameters (e.g. mass, radius) of 92 d Sct stars in eclipsing binaries have been gathered. Comparison of the properties of single and eclipsing binary member delta Sct stars has been made. We find that single d Sct stars pulsate in longer periods and with higher amplitudes than the primary delta Sct components in eclipsing binaries. The v sin i of delta Sct components is found to be significantly lower than that of single delta Sct stars. Relationships between the pulsation periods, amplitudes and stellar parameters in our list have been examined. Significant correlations between the pulsation periods and the orbital periods, Teff, logg, radius, mass ratio, v sin i and the filling factor have been found.
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    Effective Temperatures of Selected Main-Sequence Stars with the Most Accurate Parameters
    (Astronomical Soc Pacific, 2015) Soydugan, Faruk; Eker, Z.; Soydugan, Esin; Bilir, S.; Gokce, E. Y.; Steer, I.; Tuysuz, M.
    In this study we investigate the distributions of the properties of detached double-lined binaries (DBs) in the mass luminosity, mass radius, and mass-effective temperature diagrams. We have improved the classical mass luminosity relation based on the database of DBs by Eker et al. (2014a). Based on the accurate observational data available to us we propose a method for improving the effective temperatures of eclipsing binaries with accurate mass and radius determinations.
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    First photometric study of W UMa-type binary systems: BK Vul and V699 Cep
    (Elsevier, 2024) Adalali, S.; Soydugan, Esin
    In this study, new CCD photometric observations and photometric analysis of BK Vul and V699 Cep systems, which are classified as contact binaries in the literature, are presented. For the V699 Cep, the TESS light curve was also used in the photometric analysis. We determined the basic astrophysical parameters of the BK Vul and V699 Cep systems from photometric analysis using the Wilson-Devinney method. Due to the lack of spectroscopic data for both systems in the literature, these absolute parameters were approximately calculated as to be M 2 = 0.73 M ae , R 1 = 1.39 R ae and R 2 = 1.09 R ae for BK Vul, and M 2 = 0.36 M ae , R 1 = 2.40 R ae and R 2 = 1.33 R ae for V699 Cep after estimating the mass of the primary component. The period decrease rate ( dP/dt ) and cyclic variation period of BK Vul were determined from the O - C analysis as-3.86 x10 -7 day yr -1 and 27 yrs., respectively. The evolutionary status of components of both systems were discussed.