• Journal of Astronomy and Space Sciences
• /
• 제33권3호
• /
• pp.185-196
• /
• 2016

New multiband BVRI light curves of NSVS 1461538 were obtained as a byproduct during the photometric observations of our program star PV Cas for three years from 2011 to 2013. The light curves indicate characteristics of a typical W-subtype W UMa eclipsing system, displaying a flat bottom at primary eclipse and the O'Connell effect, rather than those of an Algol/b Lyrae eclipsing variable classified by the northern sky variability survey (NSVS). A total of 35 times of minimum lights were determined from our observations (20 timings) and the SuperWASP measurements (15 ones). A period study with all the timings shows that the orbital period may vary in a sinusoidal manner with a period of about 5.6 yr and a small semi-amplitude of about 0.008 day. The cyclical period variation can be interpreted as a light-time effect due to a tertiary body with a minimum mass of 0.71 M_⊙. Simultaneous analysis of the multiband light curves using the 2003 version of the Wilson-Devinney binary model shows that NSVS 1461538 is a genuine W-subtype W UMa contact binary with the hotter primary component being less massive and the system shows a low mass ratio of q(m_c/m_h)=3.51, a high orbital inclination of 88.7°, a moderate fill-out factor of 30 %, and a temperature difference of ΔT=412 K. The O'Connell effect can be similarly explained by cool spots on either the hotter primary star or the cool secondary star. A small third-light corresponding to about 5 % and 2 % of the total systemic light in the B and V bandpasses, respectively, supports the third-body hypothesis proposed by the period study. Preliminary absolute dimensions of the system were derived and used to look into its evolutionary status with other W UMa binaries in the mass-radius and mass-luminosity diagrams. A possible evolution scenario of the system was also discussed in the context of the mass vs mass ratio diagram.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
• /
• 한국우주과학회 2000년도 한국우주과학회보 제9권2호
• /
• pp.87-87
• /
• 2000

• 한국우주과학회:학술대회논문집(한국우주과학회보)
• /
• 한국우주과학회 1997년도 한국우주과학회보 제6권2호
• /
• pp.17.2-17
• /
• 1997

No Abstract.See Full-text

• 천문학회지
• /
• 제8권1호
• /
• pp.15-23
• /
• 1975

A new technique of photographic observations is developed for the determination of time of minimum light of eclipsing binary. An instrumental system to accomplish the observation is described. With this instrument the atmospheric extinction coefficients in Seoul are observed, and four times of minimum light for Algol and W UMa are determined.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
• /
• 한국우주과학회 2001년도 한국우주과학회보 제10권1호
• /
• pp.21-21
• /
• 2001

No Abstract, See Full Text

• East Asian mathematical journal
• /
• 제25권2호
• /
• pp.119-126
• /
• 2009

In this paper slightly fuzzy continuous mappings is introduced and some interesting properties and characterizations of slightly fuzzy continuous mappings are discussed.

• Journal of Astronomy and Space Sciences
• /
• 제15권2호
• /
• pp.335-340
• /
• 1998

IUE 저 분산 관측자료를 가지고 W-UMa 형 별인 44i Boo의 자외선 광도곡선을 완성하였다. 채층과 전이영역으로부터 나오는 방출선의 변화를 알아보기 위해서 CI, CII, CIV, SiIV, Hell 선의 방출선 세기를 계산하였다. CIV 방출 선이 가장 강한 방출을 보였으며, CII, Hell, CI, SiV의 순서로 방출선의 세기가 관측되었음이 확인되었다. 또한 방출선의 세기가 주기적으로 변하고 있음을 확인하였고, 모든 방출 선들이 위상 0.2와 0.8부근에서 상대적으로 강한 방출 선을 보인다. 이는 44i Boo의 표면에서 채층 및 전이영역의 활동성으로 인해 자외선 방출이 불 균일하게 나오고 있음을 나타내는 것이라고 해석할 수 있다. 채층 활동의 변화로 인해 관측시간이 서로 다를 때 자외선 방출선의 변광 형태도 달라지고 있음을 확인하였다.

• Journal of Astronomy and Space Sciences
• /
• 제20권4호
• /
• pp.249-260
• /
• 2003

1998년 12월부터 1999년 5월까지 총 10일간 W UMa형 접촉쌍성 AH Cnc를 소백산천문대의 61cm 망원경과 PM512 CCD 카메라, 그리고 BVI 필터를 사용하여 CCD 측광을 수행하였다. 새롭게 얻은 BVI 광도곡선을 Wilson-Devinney 쌍성모델의 Mode 3(접촉형)으로 분석해서 측광해를 구하고 Roche 모형을 얻었다. 지금까지 발표된 모든 극심시각들과 이번 관측자료를 사용하여 얻은 (O-C)도를 분석해서 영년주기 증가율와 질량이동률을 계산하였다.

• Bulletin of the Korean Chemical Society
• /
• 제31권12호
• /
• pp.3579-3582
• /
• 2010

We studied the reaction of tri-methylaluminum (TMA) on hydroxyl (OH)-terminated Si (001) surfaces for the initial growth of aluminum oxide thin-films using density functional theory. TMA was adsorbed on the oxygen atom of OH due to the oxygen atom’s lone pair electrons. The adsorbed TMA reacted with the hydrogen atom of OH to produce a di-methylaluminum group (DMA) and methane with an energy barrier of 0.50 eV. Low energy barriers in the range of 0 - 0.11 eV were required for DMA migration to the inter-dimer, intra-dimer, and inter-row sites on the surface. A unimethylaluminum group (UMA) was generated at each site with low energy barriers in the range of 0.21 - 0.25 eV. Among the three sites, the inter-dimer site was the most probable for UMA formation.

• 천문학회보
• /
• 제44권1호
• /
• pp.83.4-83.4
• /
• 2019

We present multi-color, high-cadence photometric study of a distant SU UMa-type dwarf nova KSP-OT-201611a discovered by the Korea Microlensing Telescope Network (KMTNet) Supernova Program (KSP). From October 2016 to May 2017, two outbursts with an interval of approximately 90 days were detected in the BV I-bands. The shapes and amplitudes of the outbursts reveal the nature of KSP-OT-201611a to be a SU UMa-type dwarf nova of outside-in origin with a superhump and an inferred orbital period of 1.69 h. The two observed bursts show a distinctively different color evolutions during the bursts due most likely to the viscosity different in accretion disk between them. The observed quiescent magnitudes and properties of the source during the outbursts indicate that it is at a large distance (~7.3 kpc) and height (~1.7 kpc) from the Galactic disk, possibly belonging to the group of poorly-studied Population II dwarf novae. The continuous monitoring of this source may offer a rare opportunity to study a PopII dwarf nova.