• Journal of Astronomy and Space Sciences
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• 제23권3호
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• pp.177-188
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• 2006

소백산 천문대의 61cm 망원경과 2K CCD 카메라로 2003년 1월 6일부터 24일까지 5일간 WUMa형 접촉쌍성 V523 Cas를 측광판측하여 총 920개의 관측점(${\Delta}B$: 230점, ${\Delta}V$. 230점, ${\Delta}R$: 230점, ${\Delta}I$: 230점)을 얻었다. 우리의 관측점으로부터 9개의 새로운 극심시각(주극심: 5개, 부극심: 4개)을 산출하였다. 2004년도 Wilson-Devinney(WD) 쌍성 모형으로 우리가 얻은 새로운 BVRI 광도곡선과 Rucinski et al.(2003)의 시선속도 곡선을 결합하여 분석함으로서 V523 Cas의 제 물리요소를 새롭게 산출하였다. 광도곡선에 나타난 작은 비대칭을 온도가 높은 주성의 광구 표면에 차거운 흑점과 반성에 뜨거운 흑점을 가정하여 설명하였다.

• Journal of Astronomy and Space Sciences
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• 제8권1호
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• pp.73-83
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• 1991

조기형 근접쌍성 AQ Cas를 1982년부터 1989년까지 (총 91일 밤) 연세대학교 천문대 일산 관측소에서 관측하여 UBV 광도곡선을 완성하였다. U의 광도곡선으로부터 두 별사이에 물질이동으로 인하여 위상 0.55와 0.90근처에서 광도가 어두워지는 현상을 확인하였다. 우리의 관측점으로 4개의 식심시각을 결정하였고, 수집한 식심 시각을 가지고 새로운 광도요소를 얻었다. 또한, BV 광도곡선을 가지고 Wilson-Devinney 계산법으로 측광 궤도요소들을 구하였다.

• 천문학회지
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• 제39권2호
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• pp.41-50
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• 2006

We present the results of new multi-color CCD photometry for the contact binary XZ Leo, together with reasonable explanations for the period and light variations. Six new times of minimum light have been determined. A period study with all available timings confirms Qian's (2001) finding that the O-C residuals have varied secularly according to $dP/dt\;=\;+8.20{\times}10^{-8}\;d\;yr^{-l}$. This trend could be interpreted as a conservative mass transfer from the less massive cool secondary to the more massive hot primary in the system with a mass flow rate of about $5.37{\times}10^{-8}\;M_{\odot}\;yr^{-l}$. By simultaneous analysis of our light curves and the previously published radial-velocity data, a consistent set of light and velocity parameters for XZ Leo is obtained. The small differences between the observed and theoretical light curves are modelled by a blue third light and by a hot spot near the neck of the primary component. Our period study does not support the tertiary light but the hot region which may be formed by gas streams from the cool secondary. The solution indicates that XZ Leo is a deep contact binary with the values of q=0.343, $i=78^{\circ}.8$, ${\Delta}(T_1-T_2)=126\;K$, and f=33.6 %, differing much from those of Niarchos et al. (1994). Absolute parameters of XZ Leo are determined as follows: $M_1=1.84\;M_{\odot},\;M_2=0.63\;M_{\odot},\;R_1=1.75\;R_{\odot},\;R_2=1.10\;R_{\odot},\;L_1=7.19\;L_{\odot},\;and\;L_2=2.66\;L_{\odot}$.

• 천문학회보
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• 제41권1호
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• pp.41.3-42
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• 2016

New CCD photometric observations of GX Aur have been made between 2004 and 2015. Our light curves are the first ever compiled and display the variable O'Connell effect. The light variations are satisfactorily modeled by including time-varying cool-spots on the component stars. Our light curve synthesis indicates that the eclipsing pair is an A-type contact binary with parameters of i = 81.1 deg, ${\Delta}T=36K$, q = 0.950 and f = 46%. Including our 25 timing measurements, a total of 83 times of minimum light spanning about 66 yr were used for a period study. It was found that the orbital period of GX Aur has varied due to two periodic oscillations superposed on an upward-opening parabolic variation. The long-term period increase rate is deduced as $+9.636{\times}10^{-10}d\;yr^{-1}$, which can be produced as a mass transfer from the secondary star to the primary at a rate of $3.136{\times}10^{-6}M_{\odot}\;yr^{-1}$, among the largest rates for contact systems. The periods and semi-amplitudes of the two periodic variations are about $P_3=8.7yr$ and $P_4=21.2yr$, and $K_3=0.011d$ and $K_4=0.017d$, respectively. The most reasonable explanation for both cycles is a pair of light-travel-time effects driven by the possible existence of an unseen third and fourth components with projected masses of $M_3=0.91M_{\odot}$ and $M_4=1.09M_{\odot}$ in eccentric orbits of $e_3=0.13$ and $e_4=0.73$. Because no third light was detected in the light curve synthesis, each circumbinary object could be a compact star or a binary itself.

• Journal of the Optical Society of Korea
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• 제1권1호
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• pp.26-35
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• 1997

Rigorous coupled-wave analysis (RCWA) with a simplified eigenvalue problem is used to investigate the an-tireflective property of one-dimensional surface-relief gratings such as binary gratings, triangular gratings and gratings with triangle-like surface profiles. The convergence of RCWA is investigated by varying the number of layers and the number of space-harmonics used in the computation. For unpolarized light normally incident on a medium of refractive index 1.64 from vaccum, a triangle-like grating shows the reflectivity of $1.6 {\times} 10^{-4}$ in contrast to a minimum reflectivity of $3.8 {\times} 10^{-3}$ for a binary grating. We also study the dependence of reflectivity on the wavelength, and on the angle of incidence for a groove shape and depth which result in minimum reflectivity.

• 농업과학연구
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• 제40권4호
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• pp.395-403
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• 2013

Plant factory has drawn attention in many countries in the world due to capability of environmental control not only for better yield and quality, but also for increase in functional and medicinal components of the products. In this paper, an experimental plant factory was constructed for various tests under different environmental conditions, and the operations were evaluated. A production room was constructed with adiabatic materials with dimensions of $6,900{\times}3,000{\times}2,500$ mm ($L{\times}W{\times}H$). Four sets of $2,890{\times}600{\times}2,320$ mm ($L{\times}W{\times}H$) production frame unit, each with 9 light-installed beds and an aeroponic fertigation system, resulting in 36 beds, were prepared. Accuracy and response were evaluated for each environmental control component with and without crops. Air temperature, humidity, $CO_2$ concentration, light intensity, frequency, and duty ratio, fertigation rate and scheduling were controllable from a main control computer through wireless communication devices. When the plant factory was operated without crop condition, the response times were 8 minutes for change in temperature from 20 to $15^{\circ}C$ and 20 minutes from 15 to $20^{\circ}C$; 7 minutes for change in humidity from 40 to 65%; and 4 minutes for change in $CO_2$ concentration from 450 to 1000 ppm. When operated for 24 hours with crop cultivation; average, maximum, and minimum values of temperatures were 20.06, 20.8, and $18.8^{\circ}C$; humidity were 66.72, 69.37, and 63.73%; $CO_2$ concentrations were 1017, 1168, and 911 ppm, respectively. Photosynthetic Photon Flux Density was increased as the distance from the light source decreased, but variability was greater at shorter distances. Results of the study would provide useful information for efficient application of the plant factory and to investigate the optimum environment for crop growth through various experiments.

• 천문학회지
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• 제39권1호
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• pp.25-30
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• 2006

We completed four color light curves of the near-contact binary CN And during three nights from September to December 2004 using the 61-cm reflector and BV RI filters at Sobaeksan Observatory. We determined four new times of minimum light (two timings for primary eclipse, two for secondary). Newly obtained BV RI light curves and the radial velocity curves from Rucinski et a1. (2000) were simultaneously analyzed to derive the system parameters of CN And. We used the semi-detached mode 4 of the 2003-version of the Wilson-Devinney binary model, and interpreted the asymmetry of the light curve by introducing two spots; a cool spot on the primary component and a hot spot on the secondary component. New photometric parameters are not much different from those of Cicek et a1. (2005), and it is considered that the system is in the era of broken contact. From the orbital period study with all available timings including our data, we found a continous period decrease with a rate of $P_{obs}=--1.82{\times}10^{-7}\;d\;yr^{-1}$ that can be explained with two possible mechanisms. We think the most likely cause of the period decrease is a thermal mass transfer from the primary to the secondary component, rather than angular momentum loss due to a magnetic stellar wind.

• 생물환경조절학회지
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• 제3권2호
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• pp.106-118
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• 1994

동계 무가온 다중피복 plastic house내 고추육묘의 생장에 영향을 미치는 온도, 광도 및 지온의 변화를 노지와 시설내 피복별로 조사 분석하여 고추의 적정 육묘생장 환경과 실제 무가온 다중피복 plastic house내의 환경요인과의 관련성을 파악코자 수행한 결과는 다음과 같다. 1. 12월 20일부터 2월 25일 까지 P. E.필름으로 4중피복된 턴널내에서도 최저온도는 대부분 5$^{\circ}C$를 보여 고추의 냉해온도에 대한 노출을 피할 수 없었고 이 기간에 최고온도는 대부분 33$^{\circ}C$를 보였으며 극값은 42$^{\circ}C$를 보여 다소간 환기의 필요도 인정되었다. 2. 피복이 증가할수록 온도 일교차가 크게 나타나 노지는 5-1$0^{\circ}C$를 보인 반면 피복내에는 16-38$^{\circ}C$의 일교차를 보였다. 3. 저온기에 다중피복에 의한 보온효과는 뚜렷하였으나 4중피복하에서도 12$^{\circ}C$이하의 온도출현이 많아서 고추 시설내 육묘시 냉해피해 가능성이 상존하며, 3$0^{\circ}C$이상의 고온출현회수도 200회 이상이었다. 4. 광도에 있어서도 피복이 증가할수록 광도는 감소하였고 온도증가는 크게 광의존성이었으며, 최저광도는 피복에 관계없이 고추의 광보상점 이하를 보여주었다. 5. 12월 20일부터 2월 중순까지 기온은 오전 10시 이후에야 고추의 생육한계온도인 10-12$^{\circ}C$이상이 되었고, 오후 4시 이후에는 기온은 12$^{\circ}C$이상이 되어도 광도가 급격히 낮아 고추유묘의 광합성 및 생장에 제한적일 것으로 사료되었다. 6. 시설내 최저지온은 동계 4중피복내에서도 1$0^{\circ}C$내외로서 고추생장에는 생리적 피해온도 범위에 속하였다. 7. 광주지방에 45년간 온도자료를 보면 노지 최저온도의 극값은 1월 5일에 -19.4$^{\circ}C$를 기록하였으며 대부분 장기자료로부터 얻은 평균에서 $\pm$5$^{\circ}C$의 편차를 보였다.

• Journal of Astronomy and Space Sciences
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• 제19권1호
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• pp.47-56
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• 2002

2000년 11월 21일부터 23일가지 3일간 식쌍성 V65l Cas의 극심시각 관측을 수행하였다. 이 관측으로부터 총7개의 새로운 극심시각을 얻었다. 이 관측치를 포함한 V651 Cas의 광전관측 및 CCD 극심시각을 재분석하여, 김천휘와 이재우(2000)가 제안한 제3 천체에 의한 광시간 궤도를 확인하였고, 개선하였다. 최종적으로 구한 광시간 궤도의 주기, 반-진폭, 그리고 이심율은 각각 $6.^{y}3,\;0.^{d}0013$, 그리고 0.78이다. 제3 천체의 궤도경사각이 $30^{\circ}$보다 클 경우, 제3 천체의 질량은 $0.09M_{\odot}\;{\leq}\;M_3\;{\leq}\;0.20M_{\odot}$의 범위에 있다. V65l Cas 계에 상정된 제3 천체가 진실로 존재하고, 주계열성이라면, 그 제3 천체는 주계열 끝에 위치한다.

• Journal of Astronomy and Space Sciences
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• 제15권1호
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• pp.75-82
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• 1998

A total of 842 observations (277 in B, 282 in V, and in R) for U Pegasi were made in October of 1996 at Mt. Sobaek Observatory. With our data we constructed the BVR light curves and determinded 5 times of minimum light. We also obtained physical parameters of the system by combined analysis of both light and radial velocity curves using the Wilson-Devinney code.