The first multisite photometric campaign devoted to the rapidly oscillating mass-accreting (primary) component of Algol-type eclipsing binary system AS Eri has confirmed presence rapid pulsations with frequency 59.03116 d-1, and revealed second third oscillation modes frequencies 62.5631 d-1 61.6743 respectively. These are related 5-6 overtone oscillations among shortest periods excited in non-magnetic MS A-F stars. nearly equator-on visibility binaries help narrow range possible mode...

We searched for circumbinary planets orbiting NY Vir in historical eclipse times including our long-term CCD data.Sixty-eight of minimum light with accuracies better than 10 s were used the ephemeris computations.The best fit to those timings indicated that orbital period has varied due a combination two sinusoids periods P 3 =8.2yr and 4 =27.0 yr semi-amplitudes K =6.9s =27.3 s, respectively.The periodic variations most likely arise from pair light-time effects presence third fourth bodies...

In this study, we address the question of whether can properly determine differential emission measures (DEMs) using Solar Orbiter/Extreme Ultraviolet Imager (EUI)/Full Sun (FSI) and AI-generated extreme UV (EUV) data. The FSI observes only two full-disk EUV channels (174 304 Å), which is insufficient for accurately determining DEMs lead to significant uncertainties. To solve problem, trained tested deep learning models based on Pix2PixCC Dynamics Observatory (SDO)/Atmospheric Imaging...

In this study, we determine the differential emission measures (DEMs) using Solar Orbiter/Extreme Ultraviolet Imager (EUI)/Full Sun (FSI) and AI-generated EUV data. The FSI observes only two full-disk extreme UV (EUV) channels (174 304 Å), which poses a limitation for accurately determining DEMs. We address problem deep learning models based on Pix2PixCC, trained Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) dataset. These successfully generate five-channel (94, 131,...

The purpose of this study is to conduct a customized program for the elderly with mild cognitive impairment and mild-severe physical functional who use day care facilities among long-term verify their effectiveness. To end, 16 people in experimental group control were studied using two located Gwangjin-gu, Seoul. conducted by cognitive-physical activity that provides support from 3rd grade insurance elderly, it composed reflecting real awareness training, stimulation activities, exercise...

We present the results of a three-continent multisite photometric campaign carried out on Algol-type eclipsing binary system RZ Cas, in which primary component has recently been discovered to be δ Sct-type pulsator. The observations include, for first time, complete simultaneous Strömgren uvby light curves together with few Crawford Hβ data collected around orbital phase quadrature. new confirm pulsational behaviour component. A detailed analysis, based these observations, is presented both...

New CCD photometric observations of the eclipsing system AR Boo were obtained from February 2006 to April 2008. The star's properties are derived detailed studies period variability and all available light curves. We find that over about 56 years orbital has varied due a combination an upward parabola sinusoid rather than in monotonic fashion. Mass transfer less massive primary more secondary component is likely responsible for at least significant part secular change. cyclical variation...

We present new photometric data of the transiting planet HAT-P-12b observed in 2011. Our three transit curves are modelled using JKTEBOP code and adopting quadratic limb-darkening law. Including our measurements, 18 times spanning about 4.2 yr were used to determine improved ephemeris with a epoch 2,454,187.85560$\pm$0.00011 BJD an orbital period 3.21305961$\pm$0.00000035 d. The physical properties star-planet system computed empirical calibrations from eclipsing binary stars stellar...

We present the results of a systematic search for pulsating components in Algol-type eclipsing binary systems. A total number 14 binaries with A–F spectral type primary were observed 22 nights. confirmed small-amplitude oscillating features recently detected pulsator TW Dra, which has period 0.053 day and semi-amplitude about 5 mmag B-passband. discovered new two RX Hya AB Per. The component is dominant 0.052 7 mmag. Per also 0.196 10 suggest that these pulsators are members newly introduced...

We present four new transits of the planetary system TrES-3 observed between 2009 May and 2010 June. Among these, third transit by itself indicates possible evidence for brightness disturbance, which might be result planet blocking a cool starspot on stellar surface. A total 109 times, including our measurements, were used to determine improved ephemeris with epoch 2454185.910944$\pm$0.000072 HJED an orbital period 1.30618700$\pm$0.00000015 d. analyzed light curves using JKTEBOP code...

The Kepler light curve of KIC 4739791 exhibits partial eclipses, the inverse O'Connell effect, and multiperiodic pulsations. Including a starspot on either binary components, light-curve synthesis indicates that is in detached or semi-detached configuration with both short orbital period low mass ratio. Multiple frequency analyses were performed residuals after subtracting binarity effects from original data. We detected 14 frequencies: 6 low-frequency region (0.1−2.3 days−1) 8...

We present CCD photometric results of the eclipsing binary Y Cam, whose primary component has been known to be a δ Scuti type pulsator. Observations were performed for 16 nights, including two minima, from November 2000 May 2001. After correction light variations caused by phenomenon, we investigated its pulsating features in detail. derived four pulsation frequencies 15.0473 c/d, 18.2852 14.8203 c/d and 17.7348 using all data except phase. The first frequency turned out constant over 40...

New CCD photometry over four successive years from 2005 is presented for the eclipsing binary GW Cep, together with reasonable explanations light and period variations. All historical curves, obtained a 30 yr interval, display striking changes, are best modeled by simultaneous existence of cool spot hot on more massive component star. The facts that system magnetically active has consistently existed inner hemisphere star indicate two spots formed (1) magnetic dynamo-related activity (2)...

We present new multicolor charge-coupled device (CCD) photometry for the short-period close binary V432 Per, made on six nights between 2006 February and December. A period study of system, based all published newly observed times minimum light, reveals that orbital has varied as a beat effect due to combination secular increase sinusoidal variation, with 35.3 yr semi-amplitude 0.0104 d. The continuous can be interpreted mass transfer from less massive secondary star more primary component...

New CCD photometry is presented for the hot overcontact binary DK Cyg together with reasonable explanations light and period variations. Historical velocity curves from 1962 to 2012 were simultaneously analyzed Wilson–Devinney (W–D) synthesis code. The brightness disturbances satisfactorily modeled by applying a magnetic cool spot on primary star. Based 261 times of minimum that include 116 new timings span more than 87 years, study reveals orbital has varied due periodic oscillation...

We have obtained CCD photometric observations of the near‐contact binary AX Dra during two observing seasons from 2001 March through May and 2003 April May. From these measurements, seasonal light curves for were compiled, a total 13 new timings minimum calculated. An analysis resulting O - C diagram reveals evidence periodic change with semiamplitude 0.0061 days period 56.1 yr, but this conclusion depends entirely on photographic plate estimates around 1960. Our display conventional...

We present the results of new CCD photometry for contact binary BX Peg, made during three successive months beginning on September 2008. As do historical light curves, our observations display an O'Connell effect and November data by themselves indicate clear evidence very short-time brightness disturbance. For these variations, model spots are applied separately to two set Group I (Sep.--Oct.) II (Nov.). The former is described a single cool spot secondary photosphere latter two-spot with...

NSVS 02502726 has been known as a double-lined, detached eclipsing binary that consists of two low-mass stars. We obtained $BVRI$ photometric follow-up observations in 2009 and 2011 to measure improved physical properties the star. Each set light curves, including 2008 data given by \cCakirli et al., was simultaneously analyzed with previously published radial-velocity curves using Wilson-Devinney code. The conspicuous seasonal variations system are satisfactorily modelled two-spot model one...

We present multi-passband CCD photometry of 20 ROTSE-I δ Scuti type pulsating stars and 1 RR Lyrae star to re-classify their variable types using the comparison amplitudes between V I passbands. For re-classification, we used a criterion that have larger amplitude differences passbands than eclipsing binaries because brightness changes are mainly due temperature variations. As result, only six were re-confirmed as variables thirteen turned out be W UMa binaries. The other two identified one...

New CCD photometry of seven successive years from 2010 is presented for the HW Vir-type eclipsing binary 2M 1533+3759. Using $VI$ light curves together with radial-velocity data given by For et al. (2010), we determined absolute parameters each component to be $M_1$ = 0.442$\pm$0.012 M$_\odot$, $M_2$ 0.124$\pm$0.005 $R_1$ 0.172$\pm$0.002 R$_\odot$, $R_2$ 0.157$\pm$0.002 $L_1$ 19.4$\pm$1.4 L$_\odot$, and $L_2$ 0.002$\pm$0.002 L$_\odot$. These indicate that 1533+3759 a detached system...

Abstract We present observational results of four eclipsing binary stars, Y Cam, RZ Cas, AS Eri and RU UMi, which were reported to have δ Scuti type pulsating components.

1998년 12월부터 1999년 5월까지 총 10일간 W UMa형 접촉쌍성 AH Cnc를 소백산천문대의 61cm 망원경과 PM512 CCD 카메라, 그리고 BVI 필터를 사용하여 측광을 수행하였다. 새롭게 얻은 광도곡선을 Wilson-Devinney 쌍성모델의 Mode 3(접촉형)으로 분석해서 측광해를 구하고 Roche 모형을 얻었다. 지금까지 발표된 모든 극심시각들과 이번 관측자료를 (O-C)도를 영년주기 증가율와 질량이동률을 계산하였다. photometric observations of a UMa type contact binary Cnc were performed for ten nights from December 1998 to May 1999 using camera and filters attached the 61㎝ reflector at Sobaeksan Optical Astronomy Observatory. New light curves analyzed with 3...

2000년 11월부터 2001년 5월까지 총 16일간 맥동 식쌍성 Y Carn을 소백산천문대의 61cm 망원경에 부착된 단일 V 필터로 CCD 측광을 수행하였다. 새롭게 얻은 광도곡선과 Broglia & Marin(1974)의 BV 광도곡선을 Wilson-Devinney 방법의 Mode 2(분리형)와 5(준분리형)으로 분석하였다. 분석 결과는 다음과 같다. 1) 광도곡선 분석만으로는 분리헝과 준분리형의 Roche 모형 중 어느 것이 Cam의 진실한 모형인가를 가려낼 수가 없다. 2) B광도곡선에는 삼체의 광도가 약 2%, V광도곡선에는 3% 존재한다. 3) 주성에서 발생하는 맥동에 의한 밝기 변화는 해에 거의 영향을 주지 않으나, 맥동을 고려하였을 경우 분리형 모델이 준분리형 모델보다 약간 더 관측치를 잘 맞춘다. 4) 분리형과 각각에 대해 절대물리량을 계산하였다. We performed photometric observations of the eclipsing binary...