• PNF and Movement
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• 제21권2호
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• pp.151-158
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• 2023

Purpose: This study aimed to examine the immediate effects of different breathing training techniques on diaphragm excursion and vital capacity in healthy adults. Specifically, the study focused on comparing respiratory exercise without PNF, bilateral pattern respiratory exercise, and bilateral pattern with spiral pattern respiratory exercise. Methods: Twenty-seven healthy adults in their 20s participated in the study. Diaphragm excursion and vital capacity were evaluated under three different conditions. A one-way repeated ANOVA was used to analyze the differences in diaphragm excursion and vital capacity among the interventions. Results: Statistically significant differences were observed in diaphragm excursion among the interventions, comparing respiratory exercise without PNF, bilateral pattern respiratory exercise, and bilateral pattern with spiral pattern respiratory exercise. Similarly, statistically significant differences were found in vital capacity among the interventions without PNF respiratory exercise, bilateral pattern respiratory exercise, and bilateral pattern with spiral pattern respiratory exercise. Conclusion: The study demonstrated that incorporating the spiral technique in respiratory exercise led to increased diaphragm excursion and lung capacity compared to other interventions. These findings suggest that PNF respiratory exercise combined with the spiral pattern may have clinical implications for the treatment of respiratory diseases. Further research is warranted to explore the long-term effects and clinical application of these approaches.

• 한국자기학회지
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• 제6권3호
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• pp.179-188
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• 1996

spiral 패턴과 meander 패턴의 공심 평면 인덕터에 대해 주파수, 도체간격, 도체폭, 턴수등을 변화시켜 저항, 인덕턴스와 같은 전기적인 특성치의 이론적인 예측에 대해 검토하였다. 도체폭이 커짐에 따라 저항과 인덕턴스는 감소한다. 이때 Q는 spiral pattern에서는 최대치를 가지는 도체폭이 존재하는 반면 meander pattern에서는 저항의 감소가 인덕턴스의 감소보다 작아지므로 도체폭이 증가하면 Q가 증가하였다. spiral pattern에서는 도체간격을 작게할 때 저항, 인덕턴스, Q는 더 이상 증가하지 않는 도체간격이 존재하지만 meander pattern에서는 인접 도체 사이의 상호 인덕턴스의 부호가 (-)가 됨에 따라 도체 간격은 가능한 한 커야 한다. 턴수가 증가함에 따라 저항, 인덕턴스는 증가하며 spiral pattern에서는 최대의 Q를 가지는 턴수가 존재하지만 meander pattern에서는 인덕턴스의 증가보다 저항의 증가가 크기 때문에 턴수의 증가에 따라 Q는 감소하였다.

• 한국정밀공학회지
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• 제25권4호
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• pp.134-139
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• 2008

A spirally arrayed nano-pattern is designed as a model pattern for the next generation optical storage media. The pattern consists off types of embossed rectangular dot, which are 50nm, 100nm, 150nm and 200nm in length and 50nm in width. The height of the dot is designed to be 50nm. The pitch of the spiral track of the pattern is 100nm. A ER(Electron resist) master for this pattern is fabricated by e-beam lithography process. The ER is first spin-coated to be 50nm thick on a Si wafer and then the model pattern is written on the coated ER layer by e-beam. After developing this pattern written wafer in the solution, a ER pattern master is fabricated. The most conventional e-beam machine can write patterns in orthogonal way, so we made our own pattern generator which can write the pattern in circular or spiral way. This program generates the patterns to be compatible with the e-beam machine from Raith(Raith 150). To fabricate 50nm pattern master precisely, a series of experiments were done including the design compensation for the pattern size, optimization of the dose, acceleration voltage, aperture size and developing. Through these experiments, we conclude that the higher accelerating voltages and smaller aperture size are better for mastering the nano pattern which is in order of 50nm. With the optimized e-beam lithography process, a spiral arrayed 50nm pattern master adopting PMMA resist was fabricated to have dimensional accuracy over 95% compared to the designed. Using this pattern master, a metal pattern stamp will be fabricated by Ni electro plating for injection molding of the patterned plastic substrate.

• 천문학회보
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• 제36권2호
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• pp.57.1-57.1
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• 2011

Using high-resolution numerical simulations, we investigate the formation of gaseous substructures and mass inflow rates in barred spiral galaxies in the presence of both bar and spiral potentials. The gaseous medium is assumed to be infinitesimally-thin, isothermal, unmagnetized, and non-self-gravitating. To consider various galactic situations, we vary the pattern speed and strength of spiral arms as well as the black hole mass. We find that spiral arms with pattern speed smaller than that of the bar remove angular momentum from the gas outside corotation which transports to the bar region, making the dust lanes strong and live long. When the arm pattern speed is identical to that of the bar, on the other hand, the gas outside corotation gains angular momentum and thus moves outward, without affecting the bar region. Overall gaseous morphologies in simulations match well with observed IR images of barred spiral galaxies such as NGC 1097, when the arms and bar are in phase at the corotation radius. The presence of spiral arms increases the mass inflow rate as well, making it larger than $0.01M_{\odot}/yr$ when MBH is $4{\times}10^7M_{\odot}$, possibly explaining AGN activities in Seyfert galaxies.

• 대한수학회보
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• 제52권4호
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• pp.1113-1122
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• 2015

This paper is concerned with the pattern formation of a diffusive predator-prey model with two time delays. Based upon an analysis of Hopf bifurcation, we demonstrate that time delays can induce spatial patterns under some conditions. Moreover, by use of a series of numerical simulations, we show that the type of spatial patterns is the spiral wave. Finally, we demonstrate that the spiral wave is asymptotically stable.

• 천문학회보
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• 제38권1호
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• pp.31.1-31.1
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• 2013

Barred-spiral galaxies possess double patterns: a bar and spiral arms. While their angular speeds play an important role in governing gas dynamical evolution of barred spiral galaxies, there is no direct way to observe them. The Tremaine-Weinberg (TW) method has been one of the most reliable indirect methods to estimate pattern speeds, although it requires a few strict assumptions, notably one that the gas tracer is in a quasi-steady state. In barred-spiral galaxies, however, non-steady gas flows are significant especially when the double patterns have different angular speeds. Using numerical models, we explore the effect of non-steady gas motions on the determination of double pattern speeds based on the TW method. We find that the TW method is accurate within 15% when there is only a single pattern or when double patterns have the same angular speed. When double patterns have different speeds, on the other hand, neglecting the non-steady flows leads to quite large errors (> 30%) in the derived pattern speeds, and severely underestimate the real values for the viewing angle parallel to the bar minor axis. This suggests that one should be cautious when applying the TW method to galaxies with double patterns with different speeds.

• 대한전자공학회논문지SP
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• 제49권4호
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• pp.16-22
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• 2012

본 논문에서는 어안렌즈의 교정(calibration)과 기하학적 왜곡을 보정하기 위해서 광학 시뮬레이터에 적합한 나선형 패턴을 제안하고, 이를 이용하여 별도의 수학적 모델링이 필요 없는 교정 알고리듬을 제안한다. 나선형 패턴을 광학 시뮬레이터의 입력 영상으로 이용하여 어안렌즈로 왜곡 시킨 영상에서 기하학적으로 이동된 점들의 정합을 통하여 교정을 수행한다. 이러한 과정에서 나선형 패턴 영상에서 중심으로부터 멀어지는 점들이 어안렌즈의 기하학적 왜곡을 거쳐 이동되는 정보를 왜곡되기 전의 위치와 정합하기 때문에 정확한 교정이 가능한 동시에, 별도의 모델링이 필요 없기 때문에 효율적인 처리가 가능하다. 제안된 기술은 어안렌즈를 이용한 패턴인식 시스템에서 손실 없는 디지털 영상 확대를 통하여 정확한 정보를 추출하는 데에 이용할 수 있다. 또한 넓은 시야각을 필요로 하는 다양한 영상처리 분야에 적용하여 어안렌즈의 교정과 왜곡 보정을 가능하게 한다.

• 천문학회보
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• 제39권1호
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• pp.56.1-56.1
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• 2014

With the advent of high-resolution high-sensitivity observations, spiral patterns have been revealed around several asymptotic giant branch (AGB) stars. Such patterns can provide possible evidence for the existence of central binary stars embedded in outflowing circumstellar envelopes. It is, however, not generally recognized that the binary induced pattern, vertically extended from the orbital plane, exhibits a ring-like pattern with an inclined viewing angle. I will first review the binary-induced spiral-shell patterns on the AGB circumstellar envelopes with the effect of inclination angle with respect to the orbital plane, of which large inclination cases reveal incomplete ring-like patterns. I will describe a method of extracting such spiral-shell from the gas kinematics of an incomplete ring-like pattern to place constraints on the characteristics of the (unknown) central binary stars. This first success may open the possibility of connecting the ring-like patterns commonly found in the AGB circumstellar envelopes and in the outer parts of (pre-)planetary nebulae and pointing to the conceivable presence of central binary systems, which may give a clue for the onset of asymmetrical planetary nebulae.

• 한국통신학회논문지
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• 제19권5호
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• pp.857-871
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• 1994

본 논문에서는 스파이럴 암폭이 넓은 경우와 좁은 경우, 곡률이 큰 경우와 작은 경우에 대한 스파이럴 안테나를 모먼트법을 이용하여 해석하였다. 그 방법은 안테나를 N개 선소로 분할하고 갤러킨 방법을 이용하여 각 선소의 전류분포를 구하고, 방사패턴을 계산한 다음 이들을 실험 결과와 비교하였다. 안테나의 이득이 주파수에 따란 +_ 5dB 이내로 변화가 있는 것은 밸런과 안테나간의 접속에서 나타나는 반사손실에 의한 것이다. 시뮬레이션 및 실험결과를 통하여, 본 스파이럴 안테나의 광대역 무지향 특성을 확인하였다.

• 천문학회지
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• 제37권4호
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• pp.199-203
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• 2004

The gas response to a proposed spiral stellar pattern for our Galaxy is presented here as calculated via 2D hydrodynamic calculations utilizing the ZEUS code in the disk plane. The locus is that found by Drimmel (2000) from emission profiles in the K band and at 240 ${\mu}m$. The self-consistency of the stellar spiral pattern was studied in previous work (see Martos et al. 2004). It is a sensitive function of the pattern rotation speed, $\Omega$p, among other parameters which include the mass in the spiral and its pitch angle. Here we further discuss the complex gaseous response found there for plausible values of $\Omega$p in our Galaxy, and argue that its value must be close to $20 km s^{-l}\;kpc^{-1}$ from the strong self-consistency criterion and other recent, independent studies which depend on such parameter. However, other values of $\Omega$p that have been used in the literature are explored to study the gas response to the stellar (K band) 2-armed pattern. For our best fit values, the gaseous response to the 2-armed pattern displayed in the K band is a four-armed pattern with complex features in the interarm regions. This response resembles the optical arms observed in the Milky Way and other galaxies with the smooth underlying two-armed pattern of the old stellar disk populations in our interpretation. The complex gaseous response appears to be related to resonances in stellar orbits. Among them, the 4:1 resonance is paramount for the axisymmetric Galactic model employed, and the set of parameters explored. In the regime seemingly proper to our Galaxy, the spiral forcing appears to be marginally strong in the sense that the 4:1 resonance terminates the stellar pattern, despite its relatively low amplitude. In current work underway, the response for low values of $\Omega$p tends to remove most of the rich structure found for the optimal self-consistent model and the gaseous pattern is ring-like. For higher values than the optimal, more features and a multi-arm structure appears.