• Journal of Oral Medicine and Pain
• /
• 제25권2호
• /
• pp.205-214
• /
• 2000

This study was performed to investigate the relationship between mandibular midline shift and anteroposterior first molar occlusal relation, and their effects on the mandibular height and the occlusal plane angle. For this study, 49 patients with temporomandibular disorders were selected. They did not show facial asymmetry and their facial midline coincide with maxillary dental midline. Upper and lower mandibular impression were taken and the casts were fabricated. Amount and direction of the mandibular midline shift and the anteroposterior shift between the two occluding first molars were measured on the casts. Several items related to height such as mandibular height from top of the articular surface of the condyle to curve changing point between antegonial notch and mandibular angle, condylar height which was the vertical distance from the articular surface to retroepicondyle of the condyle, and sigmoid height from the deepest point of sigmoid notch to the curve changing point and the occlusal plane angle were also measured on the panoramic and on the transcranial radiographs. Correlation between midline shift and anteroposterior first molar relation and comparison between right and left mandibular height by the midline shift and the first molar relation were analysed by SPSS windows program. The results of this study were as follows : 1. Mean amount of midline shift in the subjects with midline shift were 2.0mm for both side, respectively. The first molar relation of the ipsilateral side of midline shift showed Angle class II tendency and the contralateral side showed Angle class III tendency, which meant drift of the dentition to the side of the midline shift. 2. The occlusal plane angle on the panoramic radiograph were $13.0^{\circ}$ in right, and $12.5^{\circ}$ in left side, and their were no correlation between occlusal plane angle and mandibular midline shift and the first molar occlusal relation. 3. Angle's classification for both sides of the first molar relation were same in about half of all the subjects. Amount of deviation from class I first molar relation, however, were decreased in the contralateral side of observed side. 4. Mandibular height of the ipsilateral side to which mandibular midline shift showed tendency of lower than that of the contralateral side, and there was a tendency that the height was higher in class III subjects, then class II subjects, and lower in class I subjects. However, condylar height did not show any difference in the subjects with midline shift and also show no difference by the first molar occlusal relation.

• 한국해양공학회지
• /
• 제25권4호
• /
• pp.42-47
• /
• 2011

In this paper, wake equalizing duct (WED) form optimization was carried out using computational fluid dynamics (CFD) techniques. A WED is a ring-shaped flow vane with a foil-type cross-section fitted to a hull in front of the upper propeller area. The main advantage of a WED is the power savings resulting from the uniformity of the velocity distribution on the propeller plane, a reduction in the flow separation at the aft-body, and lift generation with a forward force component on the foil section. This paper intends to evaluate these functions and find an optimized WED form for minimizing the viscous resistance and equalizing the wake distribution. In the optimization process, the study uses four WED parameters: the angle of the section, longitudinal location, and angles of the axes for the half rings against the longitudinal and transverse planes of the ship. KRISO 300K VLCC2 (KVLCC2) is chosen as an example ship to demonstrate the WED optimization. The optimization procedure uses genetic algorithms (GAs), a gradient-based optimizer for the refinement of the solution, and Non-dominated Sorting GA-II(NSGA-II) for Multiobjective Optimization. The results show that the optimized WED can reduce the viscous resistance at the expense of the uniformity of the wake distribution.

• 대한수학회지
• /
• 제45권3호
• /
• pp.781-794
• /
• 2008

Let $\mathbb{H}_g$ and $\mathbb{D}_g$ be the Siegel upper half plane and the generalized unit disk of degree g respectively. Let $\mathbb{C}^{(h,g)}$ be the Euclidean space of all $h{\times}g$ complex matrices. We present a partial Cayley transform of the Siegel-Jacobi disk $\mathbb{D}_g{\times}\mathbb{C}^{(h,g)}$ onto the Siegel-Jacobi space $\mathbb{H}_g{\times}\mathbb{C}^{(h,g)}$ which gives a partial bounded realization of $\mathbb{H}_g{\times}\mathbb{C}^{(h,g)}$ by $\mathbb{D}_g{\times}\mathbb{C}^{(h,g)}$. We prove that the natural actions of the Jacobi group on $\mathbb{D}_g{\times}\mathbb{C}^{(h,g)}$. and $\mathbb{H}_g{\times}\mathbb{C}^{(h,g)}$. are compatible via a partial Cayley transform. A partial Cayley transform plays an important role in computing differential operators on the Siegel Jacobi disk $\mathbb{D}_g{\times}\mathbb{C}^{(h,g)}$. invariant under the natural action of the Jacobi group $\mathbb{D}_g{\times}\mathbb{C}^{(h,g)}$ explicitly.

• 천문학회보
• /
• 제43권2호
• /
• pp.58.2-58.2
• /
• 2018

Theoretically, the magnetic helicity transport flux through the solar surface into the upper atmosphere can be estimated indefinitely precisely by magnetic field footpoint tracking if the observational resolution is infinitely fine, even with magnetic flux emergence or submergence. In reality, the temporal and spatial resolutions of observations are limited. When magnetic flux emerging or submerging, the footpoint velocity goes to infinity and the normal magnetic field vanishes at the polarity inversion line. A finite observational resolution thus generates a blackout area in helicity flux estimation near the polarity inversion line. It is questioned how much magnetic helicity is underestimated with a footpoint tracking method due to the absence of information in the blackout area. We adopt the analytical models of Gold-Hoyle and Lundquist force-free flux ropes and let them emerging from below the solar surface. The observation and the helicity integration can start at different emerging stages of the flux rope, i.e., the photospheric plane initially cuts the flux rope at different levels. We calculate the magnetic helicity of the flux rope below the photospheric level, which is eventually to emerge, except the helicity hidden in the region to be swept by the blackout area with different widths. Our calculation suggests that the error in the integrated helicity flux estimate is about half of the real value or even larger when small scale magnetic structures emerge into the solar atmosphere.

• 한국항행학회논문지
• /
• 제17권5호
• /
• pp.491-496
• /
• 2013

본 논문에서는 보안등의 통합 모니터링과 제어를 위한 3G 이동통신용 RF모듈에 적용 가능한 반파장 폴디드 슬롯 안테나를 제안하였다. 제안된 안테나는 입력임피던스가 $50{\Omega}$에 가까운 총 길이가 ${\lambda}g$인 전형적인 폴디드 슬롯 안테나의 장점을 유지하면서 절반의 크기를 가지고 PCB의 가장자리에 위치할 수 있도록 변형된 폴디드 슬롯 구조이다. 제안된 안테나는 국내 3G 이동통신 대역용으로, $40.5{\times}62mm^2$의 기판 중 상단 $40.5{\times}10mm^2$의 공간을 이용하여 설계 및 제작하였다. 제작된 안테나를 측정한 결과, 390 MHz의 대역폭, 2 dBi의 이득을 얻을 수 있었다.

• Imaging Science in Dentistry
• /
• 제43권4호
• /
• pp.289-293
• /
• 2013

Purpose: This study was performed to determine the relationship between the stage of tooth eruption (both vertical and mesio-angular) and chronological age. Materials and Methods: Indirect digital panoramic radiographs were used to measure the distances from the dentinoenamel junction (DEJ) of the second molars to the occlusal plane of the second molar teeth and of the adjacent third molars in 264 Thai males and 437 Thai females using ImageJ software. The ratio of those distances was calculated by patient age, and the correlation coefficient of the ratio of the third molar length to the second molar length was calculated. Results: The correlation between the height of the vertically erupted upper third molar teeth and age was at the intermediate level. The age range of ${\geq}15$ to <16 years was noted to be the range in which the correlation between the chronological age determined from the eruptional height and actual chronological age was statistically significant. The mean age of the female subjects, in which the position of the right upper third molar teeth was at or above the DEJ of the adjacent second molar but below one half of its coronal height was $19.9{\pm}2.6$ years. That for the left side was $20.2{\pm}2.7$ years. The mean ages of the male subjects were $20.1{\pm}3.3$ years and $19.8{\pm}2.7$ years for the right and left sides, respectively. Conclusion: It might be possible to predict chronological age from the eruption height of the wisdom teeth.

• 한국전자파학회논문지
• /
• 제21권9호
• /
• pp.921-932
• /
• 2010

본 논문에서는 Sierpinski 프랙탈 구조를 이용하여 이중 대역에서 동작하는 배열 안테나를 제안하였다. 거울 대칭 형태의 $2{\times}2$ 배열 구조는 상부 $1{\times}2$ 배열과 하부 $1{\times}2$ 배열 간에 $180^{\circ}$ 위상차를 인가하면 cellular 대역과 WCDMA 대역에서 broadside 방향으로 복사 패턴을 형성한다. 따라서, 동위상 급전 회로를 적용하기 위해 배열 구조에서 상부와 하부 배열 간에 패치와 그라운드의 위치를 변경하여 위상 반전 구조를 구현하였다. 배열 안테나는 $28{\times}30{\times}5\;cm^3$의 크기를 가지며, -10 dB 반사 손실 대역은 1차 대역에서 855~1,380 MHz(47 %), 2차 대역에서 1,770~2,330 MHz(27 %)이다. 이득은 1차 대역에서 9.06~12.44 dBi, 2차 대역에서 11.76~14.84 dBi이다. 1,100 MHz에서 x-z 평면의 반전력 빔 폭은 $57^{\circ}$, y-z 평면의 반전력 빔 폭은 $46^{\circ}$이고, 2,050 MHz에서는 각각 $43^{\circ}$와 $28^{\circ}$이다.

• 대한수학회보
• /
• 제55권3호
• /
• pp.957-965
• /
• 2018

We study the class $C{\mathcal{V}} ({\Omega})$ of analytic functions f in the unit disk ${\mathbb{D}}=\{z{\in}{\mathbb{C}}$ : ${\mid}z{\mid}$ < 1} of the form $f(z)=z+{\sum}_{n=2}^{\infty}a_nz^n$ satisfying $$1+\frac{zf^{{\prime}{\prime}}(z)}{f^{\prime}(z)}{\in}{\Omega},\;z{\in}{\mathbb{D}}$$, where ${\Omega}$ is a convex and proper subdomain of $\mathbb{C}$ with $1{\in}{\Omega}$. Let ${\phi}_{\Omega}$ be the unique conformal mapping of $\mathbb{D}$ onto ${\Omega}$ with ${\phi}_{\Omega}(0)=1$ and ${\phi}^{\prime}_{\Omega}(0)$ > 0 and $$k_{\Omega}(z)={\displaystyle\smashmargin{2}{\int\nolimits_{0}}^z}{\exp}\({\displaystyle\smashmargin{2}{\int\nolimits_{0}}^t}{\zeta}^{-1}({\phi}_{\Omega}({\zeta})-1)d{\zeta}\)dt$$. Let $z_0,z_1{\in}{\mathbb{D}}$ with $z_0{\neq}z_1$. As the first result in this paper we show that the region of variability $\{{\log}\;f^{\prime}(z_1)-{\log}\;f^{\prime}(z_0)\;:\;f{\in}C{\mathcal{V}}({\Omega})\}$ coincides wth the set $\{{\log}\;k^{\prime}_{\Omega}(z_1z)-{\log}\;k^{\prime}_{\Omega}(z_0z)\;:\;{\mid}z{\mid}{\leq}1\}$. The second result deals with the case when ${\Omega}$ is the right half plane ${\mathbb{H}}=\{{\omega}{\in}{\mathbb{C}}$ : Re ${\omega}$ > 0}. In this case $CV({\Omega})$ is identical with the usual normalized class of convex univalent functions on $\mathbb{D}$. And we derive the sharp upper bound for ${\mid}{\log}\;f^{\prime}(z_1)-{\log}\;f^{\prime}(z_0){\mid}$, $f{\in}C{\mathcal{V}}(\mathbb{H})$. The third result concerns how far two functions in $C{\mathcal{V}}({\Omega})$ are from each other. Furthermore we determine all extremal functions explicitly.

• 한국전통조경학회지
• /
• 제28권3호
• /
• pp.72-84
• /
• 2010

본 연구는 서산마애삼존불을 중심으로 삼국시대 조성된 마애삼존불상 조형에 담겨진 비례미 등 구성적 원리가 어떻게 표현되고 있는지를 확인함으로써 전통 석조 방식의 하나인 삼존석조의 구축 및 응용을 위한 기초자료 구축을 모색하였다. 총 17개 마애삼존불의 크기 및 비율 분석 결과, 본존불의 평균 전고는 2.96m, 우협시는 2.19m, 좌협시는 2.16m였다. 이에 따른 높이비는 100:75:75로 좌우 대칭균형의 관계를 보였고, 좌우협시의 면적비는 13.4:16.7 로 우협시의 면적비가 높았다. 서산마애삼존불은 용현계곡의 삼불교를 건너 인암(印岩) 바위에 새겨져 있으며, 좌향은 방위각 $S47^{\circ}E$로 측정되었다. 이는 예배자의 눈부심을 차단하면서 햇빛의 방향에 따른 불상의 이미지 변화와 미감을 노린 것으로 판단된다. 서산마애불의 도상적 특징은 반가상과 봉지보주형 보상입상을 협시도 하고 있으며, 좌우비대칭형의 삼존 구성임에도 불구하고 동일한 선과 형태가 반복되는 가운데 통일성을 보임으로서 안정된 시각적 균형을 보이고 있다. 특히 서산마애삼존불의 경우, 본존불과 좌협시 그리고 우협시의 전고는 각각 2.80m, 1.66m, 1.70m였다. 좌우협시불의 높이비는 0.60:0.62로 거의 대등한 반면 면적비는 28.8:25.2로 보다 큰 차이를 보여 평면상의 면적비가 삼재미적 비례에 더욱 근접한 것으로 파악되었다. 광배 중심의 사윗각비는 88:44:48로 직각에 가까운 반면 연화좌 중심 사윗각의 비는 127:30:23으로 측정됨으로서 둔각에 가까운 부등변삼각형의 형태를 보였다. 따라서 서산마애삼존불의 상부와 하부는 직각과 둔각의 부등변삼각형의 각도 비례를 통한 대응적 관계를 유지하는 가운데 안정적 비례감을 취하고 있다. 상반부의 거리비는 0.51:0.36:0.38인 반면 하반부의 거리비는 0.53:0.33:0.27로 보다 부등변삼각형에 가까운 모습을 보이면서 상하 좌우대칭의 비대칭균형을 이루고 있다. 서산마애삼존불을 대상으로 삼재미의 관계를 살펴본 결과, 길이비 보다는 면적비나 삼각도형을 이루는 각도비가 더욱 두드러져 나타났다. 각 불상 상호간의 높이 및 면적비 못지않게 상부 광배와 하부 연화좌를 중심으로 형성되는 부등변삼각이 이루는 구도는 삼재간의 구성적 아름다움을 배가시키는 매우 중요한 내부적 동인이 되고 있다.