• Proceedings of the IEEK Conference
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• 2003.07d
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• pp.1491-1494
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• 2003

Video adaptation in response to dynamic resource conditions and user preferences is required as a key technology to enable universal multimedia access (UMA) through heterogeneous networks by a multitude of devices in a seamless way. Although many adaptation techniques exist, selections of appropriate adaptations among multiple choices are often ad hoc. To provide a systematic solution, we present a general conceptual framework to model video entity, adaptation, resource, utility, and relations among them. It allows for formulation of various adaptation problems as resource-constrained utility maximization. We apply the framework to a practical case of dynamic bit rate adaptation. Furthermore, we present a description tool, which has been accepted as a part of the MPEG-21 Digital Item Adaptation (DIA), along with a brief overview of the .elated descriptors to support terminal and network quality of service (QoS).

• 한국정보통신설비학회:학술대회논문집
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• 2007.08a
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• pp.260-263
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• 2007

무선 사업자가 각자의 네트웍 기반으로 제공하던 유무선 통신서비스는 무선사업자들은 음성서비스에 의한 유선서비스 대체(FMS)로 나타나고 있으며, 유선사업자들은 All-IP 기반의 NGN 진화에 따라 유선사업자 중심으로 유무선 서비스 통합(FMC)이라는 형태로 진화하고 있다. 초기의 FMC는 하나의 단말기로 실내의 유선서비스와 실외의 무선서비스를 Seamless 보장없이 제공하였으나, 유선전화(PSTN)의 무선랜 기반 VoIP 진화 등에 의해 무선랜-CDMA 듀얼폰 기반의 FMC Seamless 서비스를 유무선 사업자들이 준비 중에 있다. Seamless 서비스를 위한 이동성기술은 네트웍 기반에서 음성/데이터 이동성을 제공하는 기술(UMA/UNC)을 유럽에서 상용화 서비스 중이며 최근 플랫폼 진화(IMS)로 IMS/VCC기반의 음성이동성 기술이 개발되고 있으며 향후 유무선 사업자간의 IP 기반 서비스를 위한 이동성 기술 또한 다양한 기술들이 표준화 중에 있다. 이에 본 논문에서는 이러한 음성/IP이동성 기술에 대한 고찰을 통해 무선랜 중심으로 듀얼폰 기반의 이동성 기술 적용 방안을 고찰코자 한다.

• Bulletin of the Korean Space Science Society
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• 2008.10a
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• pp.29.2-29.2
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• 2008

The CCD photometric observations of the W UMa type contact binary GX Aur were performed for 33 nights from 2004 to 2008 using a 2K CCD camera and Johnson BVRI filter system attached to the 61cm reflector at Sobaeksan Optical Astronomy Observatory (SOAO). From our observations, the first BVRI light curves of GX Aur were completed and eight new times of minima (primary: 4, secondary: 4) were obtained. All the times of minima including our timings were collected and analyzed to see the dynamical behavior of GX Aur system. Intensive analysis of our BVRI lightcurves with the recent Wilson-Devinney binary model shows that GX Aur is an over-contact binary whose component stars have equal mass and time-variable spots.

• Journal of The Korean Astronomical Society
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• v.43 no.6
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• pp.201-211
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• 2010

We present an analysis of the measurements of mid-eclipse times of V839 Oph, collected from literature sources. Our analysis indicates a period increase of $3.2{\times}10^{-7}$ day/yr. This period increase of V839 Oph can be interpreted in terms of mass transfer of rate $1.76{\times}10^{-7}M_{\odot}/yr$, from the less to the more massive component. The O - C diagram shows a damping sine wave covering two different complete cycles of 36.73 yr and 19.93 yr with amplitudes approximately equal to 0.0080 and 0.0043 day, respectively. The third cycle has to be expected to cover about 13.5 years with lower amplitude than those of the former two cycles. These unequal duration cycles show a non periodicity which may be explained as resulting from either the presence of a tertiary component to the system or cyclic magnetic activity variations due to star spots. For the later mechanism, the obtained characteristics are consistent when applying Applegate (1992) mechanism.

• Journal of Astronomy and Space Sciences
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• v.14 no.1
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• pp.18-23
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• 1997

We present X-ray light curves and the energy spectra for two contact binaries SW Lac and W UMa, which are obtained from the ASCA(Advanced Satellite for Cosmology and Astrophysics) observations. We find that both sources show appreciable flux variations during the observatoins, and the variations are erratic and are not orbital-phase dependent. From a spectral analysis, we also find that the W UMa spectrum can be reproduced by a variable-abundance plasma model with a single temperature of $T_1=6.8{\times}10^6K$, while the SW Lac spectrum requires two different temperatures $T_1=6.5{\times}10^6K$ and $T_2=1.4{\times}10^7K$.

• Publications of The Korean Astronomical Society
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• v.30 no.2
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• pp.247-249
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• 2015

We review recent results on superhump period variations in SU UMa-type dwarf novae. Our statistical studies have revealed that the evolution of the superhump period is basically composed of three stages: stage-A, during which the superhump period is long and constant, stage-B, during which the superhump period increases as the superoutburst proceeds, and stage-C, during which the superhump period is short and constant. We also introduce a new method of estimating a mass ratio using the stage-A superhump period. This method can extend to, for example, low mass X-ray binaries or AM CVn stars if the stage-A superhump period is well determined.

• The Bulletin of The Korean Astronomical Society
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• v.24 no.2
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• pp.30-30
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• 1999

• Bulletin of the Korean Space Science Society
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• 1999.09a
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• pp.22-22
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• 1999

No Abstract, See Full Text

• Bulletin of the Korean Space Science Society
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• 1997.04a
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• pp.12.1-12
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• 1997

No Abstract.See Full-text

• Journal of Astronomy and Space Sciences
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• v.23 no.4
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• pp.311-318
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• 2006

High-precision photometric observations were performed in BVI bandpasses using Am robotic telescope at Mt. Lemmon Observatory for two binary stars, which are reclassified as W UMa-type systems from ROTSE(Robotic Optical Transient Search Experiment) follow-up observations and show peculiar light variations. In order to analyze W UMa-type eclipsing binaries systematically, the light curve analysis script using 2005 version of Wilson-Devinney binary code is constructed. The orbital inclinations of GSC2S84-1731 and GSC2576-0319 are $43.^{\circ}5\;and\;57.^{\circ}6$ from light-curve analysis, respectively. Spot model is applied to explain the asymmetric light curve for GSC2S84-1731 and the spot parameters are derived.