본 연구에서는 열대우림인 브루나이 MDF와 PSF의 주요 수종 (D. aromatic, D. rappa, C. arborescens)을 대상으로 초기 분해 단계의 수종별 질량 감소율과 탄질율의 변화를 파악하였다. 2019년 5월에 총 48개의 고사목 시료 (15 cm×4.8 cm×5 cm)를 산림 지표면에 배치하고 16개월 후 수거하였다. 분해 전 수종별 고사목의 밀도 (g cm-3)는 0.64±0.01 (D. aromatic), 0.60±0.00 (D. rappa), 0.44±0.02 (C. arborescens) 등이었으며, 16개월 동안 수종별 연간 질량 감소율 (%)은 6.37 (D. aromatic), 8.17 (D. rappa), 18.53 (C. arborescens) 등으로 나타났다. 부후등급은 C. arborescens에 서 III등급이 약 25%로 높았으며 흰개미의 분해 흔적이 나타났다. 한편, 16개월 후 탄질율은 D. aromatic과 D. rappa에 서 통계적으로 유의하게 감소하였으나, C. arborescens에서는 감소하는 경향이 유의하지 않았다. 이러한 연구 결과는 열대우림 내 고사목의 초기 분해는 밀도와 같은 수종의 물리적 특성에 따라 차이가 나타날 수 있으며, 주요 분해자의 유형에 따라 탄질율의 변화에도 상대적으로 차이가 있을 수 있음을 시사하는 것이다.

At q = 1.81 ± 0.20 × 10-5, KMT-2018-BLG-0029Lb has the lowest planet-host mass ratio q of any microlensing planet to date by more than a factor of two. Hence, it is the first planet that probes below the apparent "pile-up" at q = 5-10 ×10-5. The event was observed by Spitzer, yielding a microlens-parallax πE measurement. Combined with a measurement of the Einstein radius θE from finite-source effects during the caustic crossings, these measurements imply masses of the host Mhost = 1.14+0.10-0.12 M⊙ and planet Mplanet = 7.59+0.75-0.69 M⊕, system distance DL = 3.38+0.22-0.26 kpc and projected separation a⊥ = 4.27+0.21-0.23 AU. The blended light, which is substantially brighter than the microlensed source, is plausibly due to the lens and could be observed at high resolution immediately.

본 연구는 가상 질량 동조기(VMT)를 이용하여 구조물의 응답으로부터 구조물의 감쇠비를 구하는 기법을 다룬다. 백색잡음 뿐만아니라, 특정 진동수 가진, 충격하중 가진 등 다양한 하중종류 및 특성에 의하여 발생한 구조물의 계측응답에 대하여 VMT를 적 용하였을 때 구조물의 감쇠비를 추정하는 기법에 대해서 다루고, VMT의 동적특성이 구조물 감쇠비 추정에 미치는 영향을 수치적으로 분석하였다. 수치해석결과에 의하면, VMT에 의하여 구조물 감쇠비 추정이 충분한 신뢰성을 가지고 예측되는 것을 확인 할 수 있었다. 충격하중을 받는 응답을 이용하는 경우 VMT에 의하여 가장 안정적으로 구조물 감쇠비 추정이 가능한 것을 알 수 있었으며, 백색잡음, 협소대역 하중에 대해서도 VMT의 지정 감쇠비를 너무 작게 산정하지 않으면 감쇠비 추정이 가능한 것으로 나타났다. 정현파의 경우에는 가진 진동수의 VMT 비율을 이용하여 감쇠비 추정이 가능한데 고유진동수와 인접할수록 정밀도가 높아지는 것을 알 수 있었다.

We analyze the dependence of the mass-to-light ratio of spiral galaxies on the present star formation rate (SFR), and find that galaxies with high present star formation rates have low mass-to-light ratios, presumably as a result of the enhanced luminosity. On this basis we argue that variations in the stellar content of galaxies result in a major source of intrinsic scatter in the Tully-Fisher relation (TF relation). Ideally one should use a 'population-corrected' luminosity. We have also analyzed the relation between the (maximum) luminous mass and rotational velocity, and find it to have a small scatter. We therefore propose that the physical basis of the Tully-Fisher relation lies in a relationship between the luminous mass and rotational velocity, in combination with a 'well-behaved' relation between luminous and dark matter. This implies that the Tully-Fisher relation is a combination of two independent relations: (i) a relation between luminosity and (luminous) mass, based mainly on the star formation history in galaxies, and (ii) a relation between mass and rotation velocity, which is the outcome of the process of galaxy formation. In addition to a 'population-corrected' Tully-Fisher relation, one may also use the relation between mass and luminosity, and the relation between luminous mass and rotation velocity as distance estimators.

We present new BVRI light curves of UY UMa with no O’Connell effect and a flat bottom secondary eclipse. Light curve synthesis with the Wilson-Devinney code gives a new solution, which is quite different from the previous study: UY UMa is an A-subtype over-contact binary with a small mass ratio of q = 0.21, a high inclination of 81˚.4, a small temperature difference of ΔT = 18˚, a large fill-out factor of f = 0.61, and a third light of approximately 10% of the total systemic light. The absolute dimensions were newly determined. Seventeen new times of minimum light have been calculated from our observations. The period study indicates that the orbital period has intricately varied in a secular period increase in which two cyclical terms with periods of 12y.0 and 46y.3 are superposed. The secular period increase was interpreted to be due to a conservative mass transfer of 2.68 × 10–8 M⊙/yr from the less massive to the more massive star. The cyclical components are discussed in terms of double-light time contributions from two additional bound stars. The statistical relations of Yang & Qian (2015) among the physical parameters of 45 deep, low mass ratio contact binaries were revisited by using the physical parameters of UY UMa and 25 Kepler contact binaries provided by Şenavci et al. (2016).

본 연구는 유방 전단파 탄성 초음파에서 탄성도 점수와 변형비를 이용한 방법이 양성과 악성병변의 감별진단에 유용한지를 평가하였다. 탄성 초음파를 시행한 224명을 대상으로 하였으며, 유방조직검사 결과를 바탕으로 후향적인 분석을 하였다. 유방 종괴의 양성과 악성에 따른 5단계의 탄성도 점수와의 동질성 비교는 Fisher's Exact test, 변형비와의 차이검증은 Mann-Whitney U test를 실시하였다. ROC 곡선분석을 통해 악성병변의 예측을 위한 탄성도 점수와 변형비의 최적 cut off 값을 결정하였다. 양성과 악성 결절 군의 분류에 따른 탄성도 점수의 동질성 비교와 변형비의 차이검증 결과에서 각각 통계적으로 유의한 차이를 보였으며(p=.000), ROC 곡선분석에서 양성과 악성 결절의 예측을 위한 탄성도 점수와 변형비의 AUC 0.824, 0.806, cut off 값 3, 4.4로 결정되었다(p=.001). 따라서 탄성도 점수와 변형비는 유방 종괴의 감별진단에 도움을 줄 수 있을 것이다.

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 semiamplitude 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(mc/mh)=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.

Vortex shedding occurred at relatively low mean wind velocities between 13m/s and 16m/s in the 2nd Jindo grand bridge. To control the vortex shedding Multiple Tuned Mass Damper(MTMD) was installed in the mid span. The control effects of MTMD was verified by assessing the damping ratio before and after installing MTMD. This paper present the evaluation of damping ratio of a cable- stayed bridge based on measuring data through unified remote monitoring system.