이 연구는 경남 고성군 덕명리 일원에 대한 지질 교육적 가치를 탐색하기 위한 것이다. 이를 위하여 이 일대에 대한 야외조사를 통해 퇴적구조(점이층리, 사층리, 연흔, 건열), 해안 퇴적환경(해식애, 파식대지, 자갈 해빈), 상대연령 측정(부정합, 단층, 관입, 포획암) 및 주상절리와 관련된 야외 지질 학습이 가능한 다수의 관찰 지점이 분포하고 있음을 확인하였다. 이후 교육과정의 성취기준 및 교과서의 학습 요소와의 부합 정도를 분석한 결과, 모든 관찰 지점에서 교과 서에 제시된 지질학적 특성이 잘 나타나는 전형성을 보여주고 있으며, 동일한 관찰 지점에서 심화학습이 가능한 학습 요소를 갖추고 있다는 점에서 지질 교육적 가치가 큰 것으로 평가되었다. 덕명리 일원은 뛰어난 지질 교육적 가치 이 외에도 관광 및 교육 인프라가 잘 갖춰져 있는 만큼 안전한 지질 교육을 위한 학습의 장으로서 역할을 할 것으로 기대 된다.

We present the photometric properties of V608 Cas from detailed studies of light curves and eclipse timings. The light curve synthesis indicates that the eclipsing pair is an overcontact binary with parameters of ΔT = 155 K, q = 0.328, and f = 26%. We detected the third light ℓ3, which corresponds to about 8% and 5% of the total systemic light in V and R bands, respectively. Including our 6 timing measurements, a total of 38 times of minimum light were used for a period study. It was found that the orbital period of V608 Cas has varied in some combination of an upward parabola and two periodic variations. The continuous period increase with a rate of +3.99 × 10−7 d yr−1 can be interpreted as a mass transfer from the secondary component to the primary star at a rate of 1.51 × 10−7 M⊙ yr−1. The periods and semi-amplitudes of the two periodic variations are about P3 = 16.0 yr and P4 = 26.3 yr, and K3 = 0.0341 d and K4 = 0.0305 d, respectively. The most likely explanation of both cycles is a pair of light-traveling time effects operated by the possible presence of third and fourth components with estimated masses of M3 = 2.20 M⊙ and M4 = 1.27 M⊙ in eccentric orbits of e3 = 0.66 and e4 = 0.52. Because the contribution of ℓ3 is very low compared to the estimated masses of two circumbinary objects, they can be inferred as very faint compact objects.

뇌 3차원 T1 관상면 검사 시 ENCASE를 적용했을 때 CS 계수의 증가 시 영상획득 시간 변화와 영상의 질의 변화에 따른 유용성에 관하여 알아보고자 한다. 연구 대상은 본원을 내원한 30명의 환자를 대상으로 하였고, 1.5T MRI 장치로 진행하였으며, 24채널 두경부 코일을 사용하였다. 획득한 영상의 상대적신호강도비(rSI)와 상대적대조도비(rC)를 구하였으 며, MIPAV로 뇌실질과 뇌실의 체적을 측정하여 One-way Anova를 사용하여 정량적 분석을 하였고, p<0.05일 때 통계 적으로 유의한 것으로 해석하였다. 또한, 5점 리커트 척도를 이용하여 영상의 질에 대하여 정성적 분석을 하였고, 측정자 내 신뢰도를 확인하기 위해 ICC가 0.75 이상 나오면 측정자간 신뢰성이 높은 것으로 간주하였다. rSI와 rC 모두 p<0.05로 통계적으로 유의미한 차이를 보였고, 급내 상관계수가 0.75이상(p<0.05)으로 통계적으로 매우 높은 신뢰도를 나타냈다. MIPAV를 이용한 체적측정에서는 뇌실질과 뇌실의 체적의 차이는 p=1.000으로 통계학적으로 유의미한 차이는 없었고, 사후분석결과 또한 유의미한 차이를 보이지 않았으며. 급내 상관계수가 0.75이상(p<0.05)으로 통계적으로 매우 높은 신뢰도를 나타냈다. 또한, 정성적 평가에서는 CS 계수가 증가함에 따라 유의미한 차이가 있는 것으로 나타났다(p<0.001). 따라 서 ENCASE 기법을 이용한 3차원 T1 TFE 관상면 검사 시 CS 계수를 증가시킨다면 뇌의 체적 변화 없이 3차원 T1 시상면 영상보다 짧은 150초로 기존의 뇌 3차원 시상면 T1 기본 검사시간 260초 보다 짧은 영상획득 시간으로 진단적 가치가 높은 영상을 제공할 수 있을 것으로 사료된다.

Microalgae are primary producers of aquatic ecosystems, securing biodiversity and health of the ecosystem and contributing to reducing the impact of climate change through carbon dioxide fixation. Also, they are useful biomass that can be used as biological resources for producing valuable industrial products. However, harvesting process, which is the separation of microalgal biomass from mixed liquor, is an important bottleneck in use of valorization of microalgae as a bioresource accounting for 20 to 30% of the total production cost. This study investigates the applicability of sewage sludge-derived extracellular polymeric substance (EPS) as bioflucculant for harvesting microalgae. We compared the flocculation characteristics of microalgae using EPSs extracted from sewage sludge by three methods. The flocculation efficiency of microalgae is closely related to the carbohydrate and protein concentrations of EPS. Heat-extracted EPS contains the highest carbohydrate and protein concentrations and can be a best-suited bioflocculant for microalgae recovery with 87.2% flocculation efficiency. Injection of bioflocculant improved the flocculation efficiency of all three different algal strains, Chlorella Vulgaris, Chlamydomonas Asymmetrica, Scenedesmus sp., however the improvement was more significant when it was used for flocculation of Chlamydomonas Asymmetrica with flagella.

A number of roller-compacted concrete pavements (RCCP) have been constructed without saw-cut joints in order to save construction cost. Then it will allow natural cracks to randomly occur at the early age after concrete placement. Crack spacing of unjointed RCCP is crucial to ensure an adequate crack width and load transfer across the cracks since large crack spacing will result in excessive crack width and reduce load transfer efficiency that may be cause faulting, excessive deflection, and further cracking in RCCP slab. Due to pavement thickness, climatic condition, and material properties, unjointed RCCP may have different natural crack spacing. In this study, an analytical approach to predict natural crack spacing of an unjointed RCCP was developed. An analytical method based on elastic theory to calculate axial restraint stress using a bilinear slab-subbase interfacial constraint assumption was conducted. Curling stress induced by temperature gradient through the depth of the slab was also considered. The analytical model incorporates the environmental effect, strength gain and modulus of elasticity, coefficient of thermal expansion, drying shrinkage, base type materials, and slab geometries. The predicted crack spacing results obtained from the predictive model were validated through field measured data. The results showed a good agreement compared with crack spacing measured in the field. Furthermore, the result from a sensitive analysis using proposed predictive model showed that crack spacing increased when thickness of RCCP increased. The predicted crack spacing results may be used as input parameters to estimate crack widths in unjointed RCCP under given climatic condition, and material properties. If estimated crack width is excessive and cannot maintain an adequate load transfer across the cracks, saw-cut joints with an appropriate spacing should be provided in order to minimize crack width, and to prevent future cracking of RCCP leading to better performance.

We present the results of BV time-series photometry of the globular cluster NGC 288. Ob- servations were carried out to search for variable stars using the Korea Microlensing Telescope Network (KMTNet) 1.6-m telescopes and a 4k pre-science CCD camera during a test observation from August to December, 2014. We found a new SX Phe star and confirmed twelve previously known variable stars in NGC 288. For the semi-regular variable star V1, we newly determined a period of 37.3 days from light curves spanning 137 days. The light-curve solution of the eclipsing binary V10 indicates that the system is probably a detached system. The pulsation properties of nine SX Phe stars were examined by applying multiple frequency analysis to their light curves. We derived a new Period-Luminosity (P-L) relation, hMV i = −2.476(±0.300) logP − 0.354(±0.385), from six SX Phe stars showing the fundamental mode. Additionally, the period ratios of three SX Phe stars that probably have a double-radial mode were investigated; PFO/PF = 0.779 for V5, PTO/PFO = 0.685 for V9, PSO/PFO = 0.811 for V11. This paper is the first contribution in a series assessing the detections and properties of variable stars in six southern globular clusters with the KMTNet system.

We present photometric results of the  Sct star V1162 Ori, which is extensively monitored for a total of 49 nights from mid-December 2014 to early-March 2015. The observations are made with three KMTNet (Korea Microlensing Telescope Network) 1.6 m telescopes installed in Chile, South Africa, and Australia. Multiple frequency analysis is applied to the data and resulted in clear detection of seven frequencies without an alias problem: five known frequencies and two new ones with small amplitudes of 1.2-1.7 mmag. The amplitudes of all but one frequency are significantly different from previous results, confirming the existence of long-term amplitude changes. We examine the variations in pulsation timings of V1162 Ori for about 30 years by using the times of maximum light obtained from our data and collected from the literatures. The O − C (Observed minus Calculated) timing diagram shows a combination of a downward parabolic variation with a period decreasing rate of (1/P)dP/dt = −4.22 × 10−6 year−1 and a cyclic change with a period of about 2780 days. The most probable explanation for this cyclic variation is the light-travel-time effect caused by an unknown binary companion, which has a minimum mass of 0.69 M⊙. V1162 Ori is the first  Sct-type pulsating star of which the observed fast period decrease can be interpreted as an evolutionary effect of a pre-main sequence star, considering its membership of the Orion OB 1c association.