• 해양환경안전학회지
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• 제26권6호
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• pp.742-750
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• 2020

선체 부가물에서 발생하는 유동소음은 자체소음 관점에서 소나의 성능과 직결되고, 추진기 및 방향타와 상호작용을 통해 2차 소음원을 야기해 근접장 범위의 엄밀한 분석이 요구된다. 하지만 유동소음 해석에 적용되는 기존의 음향상사법은 음향 신호의 전파를 직접 모사하지 않는 간접법에 해당해 회절, 반사, 산란 특성을 고려할 수 없으며, 근접장 해석이 제한적이다. 본 연구에서는 격자 볼츠만 기법을 적용해 수중환경 유동소음의 전파과정을 직접 모사하였다. 격자 볼츠만 기법은 분자의 충돌과 흐름 과정을 통해 유동소음을 해석하는 기법으로, 압축성과 낮은 소산율, 낮은 분산율의 특성을 가지고 있어 소음해석에 적합하다. 선체 부가물 형상을 대상으로 RANS 해석을 통해 유동소음원을 도출하고, 유동-음향 경계면을 적용한 격자 볼츠만 기법으로 유동소음의 전파과정을 직접적으로 모사했다. 도출된 결과를 수음점의 위치에 따라 FW-H 결과 및 유체동압력 결과와 비교를 통해 근접장에서 타 기법 대비 격자 볼츠만 기법의 유용성을 확인했다.

• 한국전자거래학회지
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• 제20권1호
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• pp.79-88
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• 2015

웹 서버나 데이터베이스 서버와 같은 컴퓨터 서버들은 연속적으로 리퀘스트 스트림을 받는다. 이런 서버들은 유저들에게 최선의 서비스를 제공하기 위해 리퀘스트들을 스케줄링하여야 한다. 이 논문은 분할 가능 리퀘스트들을 스케줄링할 때 총 스트레치를 최소화하기 위해 혼합 유전자 알고리즘을 제안한다. 리퀘스트의 스트레치는 리퀘스트가 시스템에 머무는 시간에 대한 반응 시간의 비율로 정의된다. 혼합 유전자 알고리즘은 유전자 알고리즘의 활용과 탐구 능력를 개선하기 위해 시드 선택과 개발의 아이디어를 도입하였다. 혼합 유전자 알고리즘과 유전자 알고리즘의 성능을 비교하기 위하여 광범한 컴퓨터 실험이 실행되었다.

• KSII Transactions on Internet and Information Systems (TIIS)
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• 제6권3호
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• pp.886-905
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• 2012

Set-top Box (STB) has evolved from being a device just sitting on top of a TV shelf to a device providing a gateway to the Internet for a home network, receiving services from multiple content providers, and enabling and ensuring Quality of Service (QoS) for the streaming media. IP Multimedia Subsystem (IMS), with its promise to provide a converged access network for multimedia service delivery (such as Triple play & Quadruple play services), has to guarantee QoS support. To enable QoS in IMS-based networks, we have designed a set-top box which provides feedback to the service provider to ensure end-to-end QoS. Our set-top box is designed to provide virtual platforms such that it can support multiple service providers. Each service provider is able to manage its own multimedia streams and ensures the desired network performance for each flow. The set-top box also works as a Home Gateway and provides end-to-end QoS support to the client nodes.

• 대한기계학회논문집
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• 제12권1호
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• pp.81-94
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• 1988

본 연구에서는 표면상태가 다양한 고온면을 충돌온류에 의하여 냉각하는 방식이 광범위하게 응용되고 있는 점에 유의하여 표면조도, 노즐직경 및 분류속도를 변화시키고 노즐끝에 전열면의 직경과 동일한 원형판을 부착하여 비철액체를 막고 문극내에 온류액체를 강제유동시킴으로써 열전달에 미치는 모든 영향을 실험에 의해 고찰하고 고찰하고 포화수온류에 의한 열류속의 무차원관계식을 도출하는 것을 본 연구의 목적으로 하였다.

• 한국정보통신설비학회:학술대회논문집
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• 한국정보통신설비학회 2008년도 정보통신설비 학술대회
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• pp.45-50
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• 2008

Many applications of sensor network require connection to the Internet. The transmission protocol of traditional sensor network was designed within the sensor network itself. However, based on 6LoWPAN which can be accessed using IPv6, direct connection is possible between the sensor network and the TCP/IP network outside. Transmission of data in applications of sensor network falls into two main categories. One is a small packet that is periodically produced such as packet related to temperature and humidity. The other is a relatively large packet that brings about network overheads such as images. We investigated the conformance test and pros and cons of application data over the transmission protocol of Zigbee and 6LoWPAN. As a result, both Zigbee and 6LoWPAN have shown low rate of loss for periodic data and have in creased reliability of data transfer. When transmitting streaming image data, both ACK, non ACK mode of Zigbee and UDP of 6LoWPAN minimized transmission time but suffered the consequences of high packet loss. Even though TCP of 6LoWPAN required a long transmission time, we were able to confirm that no loss has occurred.

• 한국정보처리학회논문지
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• 제7권2S호
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• pp.721-732
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• 2000

Multimedia communication systems require not only high-performance computer hardwares and high-speed networks, but also a buffer management mechanism to process many data efficiently. Two buffer handling methods, Push and Pull, are commonly used. In the Push method, a server controls the flow of dat to a client, while in the Pull method, a client controls the flow of data from a server. Those buffering schemes can be applied to the data transfer between the packet receiving buffer, which receives media data from a network server, and media playout devices, which play the recived media data. However, the buffer management mechanism in client-sides mainly support either one of the Push or the Pull method. Consequently, they have some limitations to support various media playout devices. Futhermore, even though some of them support both methods, it is difficult to use since they can't provide a unified structure. To resolved these problems, in this paper, we propose an efficient and flexible Push/Pull buffer management mechanism at client-side. The proposed buffer management scheme supports both Push and Pull method to provide various media playout devices and to support buffering function to absorb network jitter. The proposed scheme can support the various media playback devices using a single buffer space which in consequence, saves memory space compared to the case that a client keeps tow types of buffers. Moreover, it facilitates the single buffer as a mechanism for the absorbing network jitter effectively and efficiently. The proposed scheme has been implemented in an existing multimedia communication system, so called ISSA (Integrated Streaming Service Architecture), and it shows a good performance result compared to the conventional buffering methods in multimedia communication environments.

• 전자공학회논문지CI
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• 제46권5호
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• pp.44-56
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• 2009

음성, 영상, 데이터와 같은 다양한 멀티미디어 서비스는 많은 대역폭과 실시간 처리가 필요하기 때문에 데이터의 지연과 손실에 민감한 특성을 가지고 있다. 따라서 네트워크의 흔잡 상황과 무선채널의 에러로 인한 데이터의 손실이 발생하여 사용자에게 QoS를 보장해주지 못하게 된다. 이러한 문제들을 해결하기 위해 멀티미디어 스트리밍 흐름에 속한 데이터 패킷의 중요도에 따른 차등적인 서비스로 멀티미디어의 품질을 개선하는 알고리즘의 연구가 필요하다. 본 논문에서는 무선손실이 발생했을 경우 IWFQ 알고리즘과 같이 동작하다가 멀티미디어 플로의 재생시간이 촉박할 때 우선적으로 채널을 할당하는 WMS-1(Wireless Multimedia Scheduling-1) 알고리즘과, 멀티미디어 플로에 우선권을 부여하고 프레임 유형에 따라 우선순위가 높은 프레임을 갖는 플로를 먼저 서비스하는 WMS-2(Wireless Multimedia Scheduling-2) 알고리즘을 제안한다. 기존의 알고리즘과의 비교를 통해 제안한 알고리즘의 멀티미디어 서비스 품질이 개선되었고 기지국의 큐 사이즈가 클수록 전체 서비스의 품질과 fairness가 향상된 것을 확인할 수 있었다.

• Wind and Structures
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• 제28권2호
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• pp.71-87
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• 2019

The yaw and interference effects of blades affect aerodynamic performance of large wind turbine system significantly, thus influencing wind-induced response and stability performance of the tower-blade system. In this study, the 5MW wind turbine which was developed by Nanjing University of Aeronautics and Astronautics (NUAA) was chosen as the research object. Large eddy simulation on flow field and aerodynamics of its wind turbine system with different yaw angles($0^{\circ}$, $5^{\circ}$, $10^{\circ}$, $20^{\circ}$, $30^{\circ}$ and $45^{\circ}$) under the most unfavorable blade position was carried out. Results were compared with codes and measurement results at home and abroad, which verified validity of large eddy simulation. On this basis, effects of yaw angle on average wind pressure, fluctuating wind pressure, lift coefficient, resistance coefficient,streaming and wake characteristics on different interference zone of tower of wind turbine were analyzed. Next, the blade-cabin-tower-foundation integrated coupling model of the large wind turbine was constructed based on finite element method. Dynamic characteristics, wind-induced response and stability performance of the wind turbine structural system under different yaw angle were analyzed systematically. Research results demonstrate that with the increase of yaw angle, the maximum negative pressure and extreme negative pressure of the significant interference zone of the tower present a V-shaped variation trend, whereas the layer resistance coefficient increases gradually. By contrast, the maximum negative pressure, extreme negative pressure and layer resistance coefficient of the non-interference zone remain basically same. Effects of streaming and wake weaken gradually. When the yaw angle increases to $45^{\circ}$, aerodynamic force of the tower is close with that when there's no blade yaw and interference. As the height of significant interference zone increases, layer resistance coefficient decreases firstly and then increases under different yaw angles. Maximum means and mean square error (MSE) of radial displacement under different yaw angles all occur at circumferential $0^{\circ}$ and $180^{\circ}$ of the tower. The maximum bending moment at tower bottom is at circumferential $20^{\circ}$. When the yaw angle is $0^{\circ}$, the maximum downwind displacement responses of different blades are higher than 2.7 m. With the increase of yaw angle, MSEs of radial displacement at tower top, downwind displacement of blades, internal force at blade roots all decrease gradually, while the critical wind speed decreases firstly and then increases and finally decreases. The comprehensive analysis shows that the worst aerodynamic performance and wind-induced response of the wind turbine system are achieved when the yaw angle is $0^{\circ}$, whereas the worst stability performance and ultimate bearing capacity are achieved when the yaw angle is $45^{\circ}$.

• 천문학회지
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• 제35권4호
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• pp.159-174
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• 2002

Cosmological hydrodynamic simulations of large scale structure in the universe have shown that accretion shocks and merger shocks form due to flow motions associated with the gravitational collapse of nonlinear structures. Estimated speed and curvature radius of these shocks could be as large as a few 1000 km/s and several Mpc, respectively. According to the diffusive shock acceleration theory, populations of cosmic-ray particles can be injected and accelerated to very high energy by astrophysical shocks in tenuous plasmas. In order to explore the cosmic ray acceleration at the cosmic shocks, we have performed nonlinear numerical simulations of cosmic ray (CR) modified shocks with the newly developed CRASH (Cosmic Ray Amr SHock) numerical code. We adopted the Bohm diffusion model for CRs, based on the hypothesis that strong Alfven waves are self-generated by streaming CRs. The shock formation simulation includes a plasma-physics-based 'injection' model that transfers a small proportion of the thermal proton flux through the shock into low energy CRs for acceleration there. We found that, for strong accretion shocks, CRs can absorb most of shock kinetic energy and the accretion shock speed is reduced up to $20\%$, compared to pure gas dynamic shocks. For merger shocks with small Mach numbers, however, the energy transfer to CRs is only about $10-20\%$ with an associated CR particle fraction of $10^{-3}$. Nonlinear feedback due to the CR pressure is insignificant in the latter shocks. Although detailed results depend on models for the particle diffusion and injection, these calculations show that cosmic shocks in large scale structure could provide acceleration sites of extragalactic cosmic rays of the highest energy.

• 천문학회지
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• 제45권5호
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• pp.127-138
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• 2012

We explore how wave-particle interactions affect diffusive shock acceleration (DSA) at astrophysical shocks by performing time-dependent kinetic simulations, in which phenomenological models for magnetic field amplification (MFA), Alfv$\acute{e}$nic drift, thermal leakage injection, Bohm-like diffusion, and a free escape boundary are implemented. If the injection fraction of cosmic-ray (CR) particles is ${\xi}$ > $2{\times}10^{-4}$, for the shock parameters relevant for young supernova remnants, DSA is efficient enough to develop a significant shock precursor due to CR feedback, and magnetic field can be amplified up to a factor of 20 via CR streaming instability in the upstream region. If scattering centers drift with Alfv$\acute{e}$n speed in the amplified magnetic field, the CR energy spectrum can be steepened significantly and the acceleration efficiency is reduced. Nonlinear DSA with self-consistent MFA and Alfv$\acute{e}$nic drift predicts that the postshock CR pressure saturates roughly at ~10 % of the shock ram pressure for strong shocks with a sonic Mach number ranging $20{\leq}M_s{\leq}100$. Since the amplified magnetic field follows the flow modification in the precursor, the low energy end of the particle spectrum is softened much more than the high energy end. As a result, the concave curvature in the energy spectra does not disappear entirely even with the help of Alfv$\acute{e}$nic drift. For shocks with a moderate Alfv$\acute{e}$n Mach number ($M_A$ < 10), the accelerated CR spectrum can become as steep as $E^{-2.1}$ - $E^{-2.3}$, which is more consistent with the observed CR spectrum and gamma-ray photon spectrum of several young supernova remnants.