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Kalomeni, Belinda
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04.05. Department of Pyhsics
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Publication Collaboration
| Affiliation Name | Count |
|---|---|
| Ege University | 31 |
| Izmir Institute of Technology | 19 |
| KU Leuven | 9 |
| Astronomy and Space | 8 |
| University of Cambridge | 7 |
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Data obtained from OpenAlex
Scholarly Output
19
Articles
13
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19456/7736
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0
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0
WoS Citation Count
621
Scopus Citation Count
622
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0
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0
WoS Citations per Publication
32.68
Scopus Citations per Publication
32.74
Open Access Source
19
Supervised Theses
0
| Journal | Count |
|---|---|
| Astrophysical Journal | 3 |
| Astronomy and Astrophysics | 3 |
| Astronomical Journal | 2 |
| Proceedings of the International Astronomical Union | 2 |
| AIP Conference Proceedings | 2 |
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19 results
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Now showing 1 - 10 of 19
Conference Object Citation - WoS: 1Long-Term Monitoring of Polars(Cambridge University Press, 2011) Kalomeni, Belinda; Kalomeni, Belinda; 04.05. Department of Pyhsics; 04. Faculty of Science; 01. Izmir Institute of TechnologyWe present long-term observations of magnetic cataclysmic variables AM Her, AN UMa, AR UMa, DP Leo, and V1309 Ori obtained with the ROTSEIIId telescope. All data have been analysed and preliminary results indicate periods of 170 days, 217 days, and 180 days for AM Her, AN UMa, and AR UMa, respectively. © International Astronomical Union 2012.Article Citation - WoS: 13Citation - Scopus: 8Marginally Low Mass Ratio Close Binary System V1191 Cyg(Elsevier Ltd., 2012) Ulaş, B.; Kalomeni, Belinda; Keskin, Varol; Köse, O.; Yakut, Kadri; 04.05. Department of Pyhsics; 04. Faculty of Science; 01. Izmir Institute of TechnologyIn this study, we present photometric and spectroscopic variations of the extremely small mass ratio (q ≃ 0.1) late-type contact binary system V1191 Cyg. The parameters for the hot and cooler companions have been determined as Mh = 0.13 (1) M⊙, Mc = 1.29 (8) M ⊙, Rh = 0.52 (15) R⊙, Rc = 1.31 (18) R⊙, Lh = 0.46 (25) L⊙, Lc = 2.71 (80) L⊙, the separation of the components is a = 2.20 (8) R⊙ and the distance of the system is estimated as 278 (31) pc. Analyses of the times of minima indicates a period increase of dPdt=1.3(1)×10-6days/yr that reveals a very high mass transfer rate of dMdt=2.0(4)×10-7M⊙/yr from the less massive component to the more massive one. New observations show that the depths of the minima of the light curve have been interchanged. © 2011 Elsevier B.V. All rights reserved.Article Citation - WoS: 12Citation - Scopus: 12Short and Long Time-Scale Variability in Magnetic Cataclysmic Variables: Long-Term Monitoring of Polars(Oxford University Press, 2012) Kalomeni, Belinda; Kalomeni, Belinda; 04.05. Department of Pyhsics; 04. Faculty of Science; 01. Izmir Institute of TechnologyWe present long-term observations of the magnetic cataclysmic variables AM Her, AN UMa, AR UMa, DP Leo and V1309 Ori. Analyses of both short- and long-period light variations are presented. For the first time, as far as we know, long-period variations of AN UMa and AR UMa have been studied and multiple frequencies obtained. Fourier analysis indicates 170-, 218- and 180-d variations for AM Her, AN UMa and AR UMa, respectively. These periodicities may be due to modulation of the mass-transfer rate resulting from magnetic cycles in the secondary stars. In addition, we collect the physical parameters of polars from the literature and estimate their mass-transfer rates and orbital period variation and give a rough estimation of the donor magnetic fields.Conference Object Citation - WoS: 3Citation - Scopus: 3Photometric Multi-Site Campaign on Massive B Stars in the Open Cluster Chi Persei (ngc 884)(IOP Publishing, 2008) Saesen, S.; Kalomeni, Belinda; Pigulski, A.; Carrier, F.; De Ridder, J.; Aerts, C.; Handler, G.; Drummond, R.; Kalomeni, Belinda; 04.05. Department of Pyhsics; 04. Faculty of Science; 01. Izmir Institute of TechnologyIn 2005 a photometric observation campaign started on the open cluster chi Persei, involving 13 telescopes spread over the whole northern hemisphere. After two years we gathered almost 1200 hours of data. We present here preliminary results on the variability search, especially from the 60-cm telescope in Bialkow (Poland), which show seven confirmed beta Cephei stars, four candidate B-type pulsators and other interesting variable stars.Conference Object Evolution of Binaries Towards Hmxbs and Lmxbs(American Institute of Physics, 2011) Kalomeni, Belinda; Kalomeni, Belinda; 04.05. Department of Pyhsics; 04. Faculty of Science; 01. Izmir Institute of TechnologyIn this study we investigate the evolution of binary systems towards low mass x-ray binaries and high mass x-ray binaries using Eggleton's binary star evolution code. © 2011 American Institute of Physics.Article Citation - WoS: 38Citation - Scopus: 37Close Binary and Other Variable Stars in the Solar-Age Galactic Open Cluster M67(EDP Sciences, 2009) Yakut, Kadri; Kalomeni, Belinda; Kalomeni, Belinda; Van Winckel, H.; Wealkens, C.; De Cat, P.; Bauwens, E.; Vuckovic, M.; Saesen, S.; Le Guillou, L.; Parmaksızoğlu, M.; Uluç, K.; Khamitov, I.; Raskin, G.; Aerts, C.; 04.05. Department of Pyhsics; 04. Faculty of Science; 01. Izmir Institute of TechnologyWe present multi-colour time-series CCD photometry of the solar-age galactic open cluster M67 (NGC 2682). About 3600 frames spread over 28 nights were obtained with the 1.5 m Russian-Turkish and 1.2 m Mercator telescopes. High-precision observations of the close binary stars AH Cnc, EV Cnc, ES Cnc, the δ Scuti type systems EX Cnc and EW Cnc, and some long-period variables belonging to M67 are presented. Three full multi-colour light curves of the overcontact binary AH Cnc were obtained during three observing seasons. Likewise we gathered three light curves of EV Cnc, an EB-type binary, and two light curves of ES Cnc, a blue straggler binary. Parts of the light change of long-term variables S1024, S1040, S1045, S1063, S1242, and S1264 are obtained. Period variation analysis of AH Cnc, EV Cnc, and ES Cnc were done using all times of mid-eclipse available in the literature and those obtained in this study. In addition, we analyzed multi-colour light curves of the close binaries and also determined new frequencies for the δ Scuti systems. The physical parameters of the close binary stars were determined with simultaneous solutions of multicolour light and radial velocity curves. Finally we determined the distance of M67 as 857(33) pc via binary star parameters, which is consistent with an independent method from earlier studies.Article Citation - WoS: 91Citation - Scopus: 88The Anticorrelated Nature of the Primary and Secondary Eclipse Timing Variations for the Kepler Contact Binaries(IOP Publishing Ltd., 2013) Tran, K.; Kalomeni, Belinda; Rappaport, S.; Borkovits, T.; Csizmadia, Sz.; Kalomeni, Belinda; 04.05. Department of Pyhsics; 04. Faculty of Science; 01. Izmir Institute of TechnologyWe report a study of the eclipse timing variations in contact binary systems, using long-cadence lightcurves from the Kepler archive. As a first step, observed minus calculated (O-C) curves were produced for both the primary and secondary eclipses of some 2000 Kepler binaries. We find ∼390 short-period binaries with O-C curves that exhibit (1) random walk-like variations or quasi-periodicities, with typical amplitudes of ±200-300 s, and (2) anticorrelations between the primary and secondary eclipse timing variations. We present a detailed analysis and results for 32 of these binaries with orbital periods in the range of 0.35 ± 0.05 days. The anticorrelations observed in their O-C curves cannot be explained by a model involving mass transfer, which, among other things, requires implausibly high rates of ∼0.01 MȮ yr-1. We show that the anticorrelated behavior, the amplitude of the O-C delays, and the overall random walk-like behavior can be explained by the presence of a starspot that is continuously visible around the orbit and slowly changes its longitude on timescales of weeks to months. The quasi-periods of ∼50-200 days observed in the O-C curves suggest values for k, the coefficient of the latitude dependence of the stellar differential rotation, of ∼0.003-0.013.Article Citation - WoS: 6Citation - Scopus: 6Variation of the Light and Period of the Magnetic Cataclysmic Variable Am Her(IOP Publishing, 2008) Kalomeni, Belinda; Kalomeni, Belinda; Yakut, Kadri; 04.05. Department of Pyhsics; 04. Faculty of Science; 01. Izmir Institute of TechnologyGround-based, long-term optic variability of AM Her, covering the period between 2003-2008, has been conducted to study the features seen in both low and high states of the system. Low-state analysis shows the presence of short-term, low-amplitude light variations of about 0.02-0.03 mag with a mean power time between 16 s and 226 s. Brightness variations on the order of 0.7-2 mag, which could be due to the stellar activity of the component in the system, are also detected. A total of 30 years' times of minimum light given in the literature are combined with nine times of minima obtained in this study. We represented the (observed-calculated) diagram by a parabolic curve and also by two broken lines. Under the assumption of a parabolic variation, we estimate an increase in period, dP/dt = 7.5(1.2) x 10(-9) days yr(-1), with a mass transfer rate of. M = 8(2) x 10(-9) M(circle dot) yr(-1), in agreement with the previous findings by a different method.Article Citation - WoS: 3Citation - Scopus: 3Close Binary System Go Cyg(Elsevier Ltd., 2012) Ulaş, Burak; Kalomeni, Belinda; Keskin, Varol; Köse, O.; Yakut, Kadri; 04.05. Department of Pyhsics; 04. Faculty of Science; 01. Izmir Institute of TechnologyIn this study, we present long term photometric variations of the close binary system GO Cyg. Modelling of the system shows that the primary is filling Roche lobe and the secondary of the system is almost filling its Roche lobe. The physical parameters of the system are M1 = 3.0 ± 0.2M ⊙, M2 = 1.3 ± 0.1M⊙, R 1 = 2.50 ± 0.12R⊙, R2 = 1.75 ± 0.09R⊙, L1 = 64 ± 9L ⊙, L2 = 4.9 ± 0.7L⊙, and a = 5.5 ± 0.3R⊙. Our results show that GO Cyg is the most massive system near contact binary (NCB). Analysis of times of the minima shows a sinusoidal variation with a period of 92.3 ± 0.5 yr due to a third body whose mass is less than 2.3M⊙. Finally a period variation rate of -1.4 × 10-9 d/yr has been determined using all available light curves.Article Citation - WoS: 37Citation - Scopus: 36Absolute Properties of the Binary System Bb Pegasi(IOP Publishing, 2007) Kalomeni, Belinda; Kalomeni, Belinda; Keskin, Varol; Değirmenci, Ömer Lütfi; Ulaş, Burak; Köse, Oğuzhan; 04.05. Department of Pyhsics; 04. Faculty of Science; 01. Izmir Institute of TechnologyWe present ground-based photometry of the low-temperature contact binary BB Peg. We collected all the times of mid-eclipse available in the literature and combined them with those obtained in this study. Analyses of the data indicate a period increase of (3.0 ± 0.1) × 10-8 days yr -1. This period increase of BB Peg can be interpreted in terms of the mass transfer 2.4 × 10-8 M⊙ yr-1 from the less massive to the more massive component. The physical parameters have been determined as Mc = 1.42M⊙, Mh = 0.53 M⊙, Rc = 1.29 R⊙, Rh, = 0.83 R⊙, Lc = 1.86 L⊙, and L h = 0.94 L⊙ through simultaneous solutions of light and of the radial velocity curves. The orbital parameters of the third body, which orbits the contact system in an eccentric orbit, were obtained from the period variation analysis. The system is compared to the similar binaries in the Hertzsprung-Russell and mass-radius diagrams.