• 한국음향학회지
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• 제24권5호
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• pp.271-281
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• 2005

솔레노이드 코일을 이용하여 체외 충격파 치료술에 적합한 전자기식 충격파 발생기를 구성하였다. 충격파 발생기의 충격파의 특성은 바늘형 하이드로폰을 이용하여 평가하였다 충격파 발생기 방전 전압이 8에서 18 kV로 증가할 때 측정된 충격파의 최대 양압 (P+)은 $10\~77\;MPa$사이를 비선형적으로 증가하는 것으로 나타났다. 반면, 충격파 최대 음압 (P-)은 $-3.2\~-6.8\;MPa$ 에서 변화하고 있으며, 방전 전압이 14 kV에서 -6.9 MPa로 가장 낮은 값을 보였다. 동일한 설정에서 반복 측정된 충격파의 크기 P+는 평균값의 $5\;\%$ 이내에서 변화하며, 전기 수력학적 방식 충격파 발생기 경우의 $50\;\%$ 정도와 비교하여, 매우 작은 것으로 나타났다. 시간 축에서 1 ms 동안 측정한 하이드로폰 신호로부터 충격파에 의해 야기된 음향 공동 현상, 즉, 기포의 파열 현상으로 발생된 다수의 순차적인 음향 임펄스를 관찰할 수 있었다. 웨이블렛 변환 기법을 이용하여, 충격파 강도와 밀접한 관련이 있는 것으로 알려진, 첫 번째와 두 번째 기포 파열 시간 지연을 정확히 측정하였다. 충격파 크기 P+가 10 에서 77 MPa로 증가할 때 측정된 기포 파열 지연 시간은 120부터 $700\;{\mu}s$ 로 거의 선형적으로 증가함을 관찰할 수 있었다.

• 한국추진공학회:학술대회논문집
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• 한국추진공학회 1996년도 제7회 학술강연회논문집
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• pp.107-116
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• 1996

Numerical simulations have been conducted to characterize unsteady flow structures in an axisymmetric supersonic inlet diffuser with sinusoidal pressure oscillations at the diffuser exit. The formulation is based on the unsteady Navier-Stokes equations and turbulence closure is achieved using a two-layer model with a too-Reynolds-number scheme for the near-wall treatment. The governing equations are formulated in an integral form, and are discretized by the four-stage Runge-Kutta scheme for temporal terms and the Harten-Yee upwind TVD scheme for convective terms. Results indicated that the inlet shock characteristics are significantly modified by acoustic oscillations originating from the combustor. The characteristics of shock/boundarv-layer interactions (such as the size of separation bubble, terminal shock shape, and vorticity intensity) are also greatly iufluenced by the shock oscillation due to acoustic waves.

• 한국추진공학회:학술대회논문집
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• 한국추진공학회 1998년도 제10회 학술강연회논문집
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• pp.18-18
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• 1998

평판에 충돌하는 초음속 세트에 관한 연구는 수직/단거리 이·착륙기의 발진, 미사일 발사시스템, 다단계 로켓 분리 등 실제적인 분야에 응용되고 있으며 고온의 충돌제트와 화염에 의한 가열문제와 관련된 산입분야에서도 많은 연구가 이루어지고 있다. 과소팽창하는 초음속 제트가 평판에 충돌할 때 Barrel shock, exhaust gas boundary, Mach disk, contact surface, reflected shock, plate shock, stagnation bubble 등 매우 복잡한 유동 구조가 표면에 나타나는데 이것은 평판으로부터 반사된 shock과 free jet의 충격파 구조 사이에서의 상호간섭 때문이다. 노즐로부터 방출되는 고속, 고온가스가 주변 장비 등에 부딪힐 때 발생하는 이러한 복잡한 간섭현상의 연구는 관련 주변장비 설계 및 상황예측에 필수적인 자료를 제공하며 이해를 도와준다.

• 천문학회보
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• 제43권1호
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• pp.54.4-55
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• 2018

Propagating speeds of coronal mass ejections (CMEs) have been calculated by several geometrical models based on multi-view observations (STEREO/SECCHI and SOHO/LASCO). But in 2015, we were unable to obtain radial velocity of a CME because the STEREO satellites were located near the backside of the sun. As an alternative to resolve this problem, we propose a method to combine a coronal shock front, which appears on the outermost of the CME, and an EUV-wave that occurs on the solar disk. According to recent studies, EUV-wave occurs as a footprint of the coronal shockwave on the lower solar atmosphere. In this study, the shock, observed as a bubble shape, is assumed as a perfect sphere. This assumption makes it possible to determine the height of a coronal shock, by matching the position of an EUV-wave on the solar disk and a coronal shock front in coronagraph. The radial velocity of Halo-CME is calculated from the rate of coronal shock position shift. For an event happened on 2011 February 15, the calculated speed in this method is a little slower than the real velocity but faster than the apparent one. And these results and the efficiency of this approach are discussed.

• 대한의용생체공학회:의공학회지
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• 제22권2호
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• pp.205-210
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• 2001

결석 파쇄에 ES지 장치가 이용되기 시작한 이래, 장치의 성능 및 장치에서 발생시킨 충격파가 생체에 미치는 영향등에 관한 연구가 다수 행해지고 있다. 그 중의 하나가 충격파가 전달되는 곳에는 항상 거론되는 캐비테이션 문제이다. 본 연구에서는 압전식 ESWL 장치로 대상물을 파쇄한다는 가정하에, 그 때의 매질을 캐비테이션이 미치는 영향과 관련지어 둘로 구분한다. 그것에 따라 각 매질에서의 방사음을 관측하고, 매질에 따른 파쇄효율과의 관계를 분석한 결과를 제시한다. 본 논문의 결과들은 캐비테이션 기포의 발생율이 작은 탈기수쪽이 방사음에 있어서도 분산성이 작고, 파쇄효율면에 있어서도 안정된 점을 확실히 나타내고 있다.

• 천문학논총
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• 제12권1호
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• pp.111-143
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• 1997

We have developed a spherical FCT code in order to simulate the interaction of supernova remnants with stellar wind bubbles. We assume that the density profile of the supernova ejecta follows the Chevalier mode1(1982) where the outer portion has a power-law density distribution($\rho{\propto}\gamma^{-n}$) and the SN ejecta has a kinetic energy of $10^{51}$ ergs. The structure of wind bubble has been calculated with the stellar mass loss rate $\dot{M}=5\times10^{-6}M_{\odot}/yr$ and the wind velocity $\upsilon=2\times10^3$ km/s We have simulated seven models with different initial conditions In the first two models we computed the evolution of SNRs with n=7 and n=14 in the uniform medium The numerical results agree with the Chevalier's similarity solution at early times. When all of the power-law portion of the ejecta is swept up by the reverse shock, the evolution slowly converges to the Sedov-Taylor stage. There is not much difference between the two cases with different n's The other five models simulate SNRs produced inside wind bubbles. In model III, we consider the SN ejecta of 1.4 $M_{\odot}$ and the radius of bubble ~2.76 pc so that ratio of the mass $\alpha(=M_{W.S}/M_{ej}$ is 2. We follow the complex hydrodynamic flows produced by the interaction of SN shocks with stellar shocks and with the contact discontinuities, In the model III, the time scale for the SN shock to cross the wind shell $\tau_{cross}$ is similar to the time scale for the reverse shock to sweep the power-law density profile $\tau_{bend}$. Hence the SN shock crosses the wind shell. At late times SN shock produces another shell in the ambient medium so that we have a SNR with double shell structure. From the numerical results of the remaining models, we have found that when $\tau_{cross}/\tau_{bend}\leq2$, or equivalently when $\alpha\leq50$, the SNRs produced inside wind bubbles have double shell structure. Otherwise, either the SN shock does not cross the wind shell or even if it crosses at one time, the reverse shock reflected at the center accelerates the wind shell to merge into the SN shock Our results confirm the conclusion of Tenorio-Tagle et a1(1990).

• 한국전산유체공학회:학술대회논문집
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• 한국전산유체공학회 1998년도 춘계 학술대회논문집
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• pp.1-14
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• 1998

Underwater explosion properties for TNT, an ideal explosive, and DXD-04, a nonideal explosive, were numerically modeled with a one-dimensional Lagrangian hydrodynamic code. The equation of state parameters for detonation products for TNT and DXD-04 were obtained from the BKW code, assuming complete reaction. Burn of TNT was modeled by using the Chapman-Jouguet(CJ) volume burn technique, a programmed-burn technique, assuming instantaneous detonation reaction. Burn of DXD-04 was modeled by using the same technique and by using the reaction rate calibrated from two-dimensional steady-state detonation experiments. The calculations for TNT reproduced the experimental peak pressure of the shock wave propagating through water with an error of $3.0\%$ and the experimental oscillation period of the bubble formed of detonation products with an error of $2.3\%$. For DXD-04, the CJ volume burn technique could not reproduce the experimental observations. When the reaction rate calibrated from two-dimensional steady-state detonation experimental data, the calculated peak pressure was slightly higher by $7.3\%$ than the experimental data, but the calculated shock profile was in good agreement. The bubble period was reproduced with an error of $1.8\%$. These results demonstrated that underwater explosion properties for an ideal explosive can be predicted by using a programmed burn technique, and that, however, those for a nonideal explosive can be predicted only when a well-calibrated reaction rate is used.

• 대한기계학회논문집B
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• 제35권7호
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• pp.677-683
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• 2011

지금껏 TNT 폭발에 의한 피해를 계산하는 방법에는 몇 가지 실험에 의한 모델이 제안되었다. 본 논문에서는 fire-ball 중심에서 가스가 단열이라는 가정하에 연속방정식, 오일러 및 에너지 방정식에 대한 해석적 해를 얻어 TNT 가 폭발 후 팽창하는 fire-ball 에 대한 시간에 따른 반경의 변화를 얻었다. 급격히 팽창하는 fire-ball 에 의한 충격파의 전파는 Kirkwood-Bethe 가정에 의해 구하였다. 해저에서 TNT 가폭발하게 되면 fire-ball 이 생성, 팽창해 기포로 거동하게 된다. 이 기포의 주기와 최대반경에 대한 계산 값을 실험 값과 비교한 결과 계산 값은 실험 값과 잘 일치 하였다.

• Journal of Astronomy and Space Sciences
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• 제19권3호
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• pp.173-180
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• 2002

Images taken with the Chandra X-ray telescope have for the the first time revealed the central, wind-driven, hot bubble (Chu et al. 2001), while Hubble Space Telescope (HST) WFPC2 images of the Cat's Eye nebula, NGC 6543, show that the temperature of the halo region of angular radius ~ 20", is much higher than that of the inner bright H II region. With the coupling of a photoionization calculation to a hydrodynamic simulation, we predict the observed 〔O III〕 line intensities of the halo region with the same O abundance as in the core H II region: oxygen abundance gradient does not appear to exist in the NGC 6543 inner halo. An interaction between a (leaky) fast stellar wind and halo gas may cause the higher excitation temperatures in the halo region and the inner hot bubble region observed with the Chandra X-ray telescope.

• Metals and materials international
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• 제24권6호
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• pp.1327-1332
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• 2018

In this study, a novel approach to the explosive synthesis of titanium carbide (TiC) is discussed. Nonstoichiometric $TiC_x$ powder was produced via the underwater explosion of a Ti powder encapsulated within a spherical explosive charge. The explosion process, bubble formation, and synthesis process were visualized using high-speed camera imaging. It was concluded that synthesis occurred within the detonation gas during the first expansion/contraction cycle of the bubble, which was accompanied by a strong emission of light. The recovered powders were studied using scanning electron microscopy and X-ray diffraction. Submicron particles were generated during the explosion. An increase in the carbon content of the starting powder resulted in an increase in the carbon content of the final product. No oxide byproducts were observed within the recovered powders.