• 한국지구물리탐사학회:학술대회논문집
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• 2004.06a
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• pp.3-17
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• 2004

Space-borne Earth observation technique is one of the most cost effective and rapidly advancing Earth science research tools today and the potential field and micro-wave radar applications have been leading the discipline. The traditional optical imaging systems including the well known Landsat, NOAA - AVHRR, SPOT, and IKONOS have steadily improved spatial imaging resolution but increasing cloud covers have the major deterrent. The new Earth observation satellites ENVISAT (launched on March 1 2002, specifically for Earth environment observation), ALOS (planned for launching in 2004 - 2005 period and ALOS stands for Advanced Land Observation Satellite), and RADARSAT-II (planned for launching in 2005) all have synthetic aperture radar (SAR) onboard, which all have partial or fully polarimetric imaging capabilities. These new types of polarimetric imaging radars with repeat orbit interferometric capabilities are opening up completely new possibilities in Earth system science research, in addition to the radar altimeter and scatterometer. The main advantage of a SAR system is the all weather imaging capability without Sun light and the newly developed interferometric capabilities, utilizing the phase information in SAR data further extends the observation capabilities of directional surface covers and neotectonic surface displacements. In addition, if one can utilize the newly available multiple frequency polarimetric information, the new generation of space-borne SAR systems is the future research tool for Earth observation and global environmental change monitoring. The potential field strength decreases as a function of the inverse square of the distance between the source and the observation point and geophysicists have traditionally been reluctant to make the potential field observation from any space-borne platforms. However, there have recently been a number of potential field missions such as ASTRID-2, Orsted, CHAMP, GRACE, GOCE. Of course these satellite sensors are most effective for low spatial resolution applications. For similar objects, AMPERE and NPOESS are being planned by the United States and France. The Earth science disciplines which utilize space-borne platforms most are the astronomy and atmospheric science. However in this talk we will focus our discussion on the solid Earth and physical oceanographic applications. The geodynamic applications actively being investigated from various space-borne platforms geological mapping, earthquake and volcano .elated tectonic deformation, generation of p.ecise digital elevation model (DEM), development of multi-temporal differential cross-track SAR interferometry, sea surface wind measurement, tidal flat geomorphology, sea surface wave dynamics, internal waves and high latitude cryogenics including sea ice problems.

• Korean Journal of Remote Sensing
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• v.30 no.1
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• pp.137-147
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• 2014

We proposed and verified the methods to maintain data qualities as well as to reduce data volume for the Geostationary Ocean Color Imager (GOCI), the world's first ocean color sensor operated in geostationary orbit. For the GOCI level-2 data, 92.9% of data volume could be saved by only the data compression. For the GOCI level-1 data, however, just 20.7% of data volume could be saved by the data compression therefore another approach was required. First, we found the optimized number of bits per a pixel for the GOCI level-1 data from an idea that the quantization bit for the GOCI (i.e. 12 bit) was less than the number of bits per a pixel for the GOCI level-1 data (i.e. 32 bit). Experiments were conducted using the $R^2$ and the Modulation Transfer Function (MTF). It was quantitatively revealed that the data qualities were maintained although the number of bits per a pixel was reduced to 14. Also, we performed network simulations using the Network Simulator 2 (Ns2). The result showed that 57.7% of the end-toend delay for a GOCI level-1 data was saved when the number of bits per a pixel was reduced to 14 and 92.5% of the end-to-end delay for a GOCI level-2 data was saved when 92.9% of the data size was reduced due to the compression.

• Korean Journal of Remote Sensing
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• v.30 no.4
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• pp.431-444
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• 2014

As applications of spaceborne SAR imagery are extended, there are increased demands for accurate registrations for better understanding and fusion of radar images. It becomes common to adopt multi-resolution SAR images to apply for wide area reconnaissance. Geometric correction of the SAR images can be performed by using satellite orbit and attitude information. However, the inherent errors of the SAR sensor's attitude and ground geographical data tend to cause geometric errors in the produced SAR image. These errors should be corrected when the SAR images are applied for multi-temporal analysis, change detection applications and image fusion with other sensor images. The undesirable ground registration errors can be corrected with respect to the true ground control points in order to produce complete SAR products. Speeded Up Robust Feature (SURF) technique is an efficient algorithm to extract ground control points from images but is considered to be inappropriate to apply to SAR images due to high speckle noises. In this paper, an attempt is made to apply SURF algorithm to SAR images for image registration and fusion. Matched points are extracted with respect to the varying parameters of Hessian and SURF matching thresholds, and the performance is analyzed by measuring the imaging matching accuracies. A number of performance measures concerning image registration are suggested to validate the use of SURF for spaceborne SAR images. Various simulations methodologies are suggested the validate the use of SURF for the geometric correction and image registrations and it is shown that a good choice of input parameters to the SURF algorithm should be made to apply for the spaceborne SAR images of moderate resolutions.

• Investigative Magnetic Resonance Imaging
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• v.15 no.2
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• pp.176-180
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• 2011

Metastases to the orbit usually affect the intraorbital fat and bone than the extraocular muscles. Metastasis to the extracoular muscles commonly occurs unilaterally, and diffuse enlargement of the bilateral extraocular muscles due to metastasis is extremely rare. In this report, we will describe a case of diffuse metastasis to the bilateral extraocular muscles from nasal rhabdomyosarcoma masquerading as thyroid associated orbitopathy. We will also discuss about the MR imaging findings helpful for differential diagnosis from thyroid associated orbitopathy.

• Radiation Oncology Journal
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• v.8 no.2
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• pp.169-176
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• 1990

Radiotherapy result was analyzed in 23 children with retinoblastoma treated in Seoul National University Hospital from 1980 to 1987. Three ($17\%$) had bilateral tumor at diagnosis. Among 20 children with unilateral retinoblastoma 13 children got radiotherapy after enucleation, 2 were treated with radiotherapy alone, and 5 were delivered with radiotherapy after relapse. Of 15 non-recurrent unilateral tumors, there were 5 stage II children, 8 stage III, and 2 stage IV by staging system proposed by St. Jude Children's Research Hospital. Chemotherapy was combined when resection margin of the optic nerve was positive or when malignant cell was found in CSF. Of 12 children who completed radiotherapy, local or distant failure was not found but 2 cases of relapse at the contralateral retina were observed. Their 5 year survival rate was $82.2\%$. Another case of contralateral relapse was detected in children who was treated with radiotherapy alone. Thus overall frequency of the bilateral disease was $33\%$. Prognosis of recurrent tumors were so poor that no cases of CR was obtained and that 3 year survival rate was $20\%$. Two of 3 bilateral cases at diagnosis were in NED status. Complication were sunken orbit only. Result of radiotherapy was so good in early stage or small bulk tumor that treatment delay after diagnosis must not be allowed.

• Proceedings of the Korean Vacuum Society Conference
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• 2013.02a
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• pp.476-477
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• 2013

반도체의 성능은 최근 10년 사이에 급격하게 발전했고 아날로그 및 디지털 회로 소자들에 있어 저전력/고속 특성 요구가 커지고 있다 [1]. 상온에서 30,000 $cm^2$/Vs 이상의 전자 이동도를 가지며 큰 conduction band offset을 갖는 InAs/AlSb 2차원전자가스(2DEG) 소자는 Spinorbit-interaction의 값이 매우 커서 SPIN-FET 소자로 크게 주목받고 있다 [2]. 본 발표자들은 GaAs 기판위에 성장한 InAs 2DEG HEMT 소자의 전/자기적인 특성과 고속반응 물질로 주목 받는 InSb 박막소자의 doping 특성에 따른 전기적/물리적인 특성의 평가에 대해 그 결과를 소개하고자 한다. 격자정합과 Semi-insulating 기판의 부재로 상용화되어 있는 GaAs와 InP 기판위에 물질차이에 따른 고유의 한계 특성을 줄이기 위한 Pseudomorphic이라 불리는 특별한 박막 성장 기법을 적용하여 높은 전자 이동도를 가지며 spin length가 길어 Spin-FET로서 크게 주목받고 있는 InAs 2DEG HEMT 소자를 완성시켰다. 60,000 ($cm^2$/Vs) 이상의 높은 전자 이동도를 갖는 소자의 구현을 목표로 연구를 진행하였으며 1.8 K에서 측정된 Spin-orbit interaction의 값은 6.3e-12 (eVm)이다. InAs/InGaAs/InAlAs 및 InGaAs/InAlAs 구조의 InP 기반의 소자에서 보다 큰 값으로 향후 Spin-FET 응용에 크게 기대하고 있다. 또한, GaAs 기판위에 구현된 InSb 소자는 격자부정합 감소를 위해 InAs 양자점을 사용하여 약 $2.6{\mu}m$ 두께로 구현된 InSb 박막 소자는 상온에서 약 60,400 ($cm^2$/Vs)의 상온 전자이동도를 보였으며 현재 동일 두께에서 세계 최고결과(~50,000 $cm^2$/Vs)에 비해 월등하게 높은 값을 보이고 있다. Hall bar pattern 공정을 거쳐 완성된 소자는 측정 결과 10~20% 이상 향상된 전자 이동도를 보였다. 2e18/$cm^3$ 미만의 p-doping의 경우, 상온에서 n-type 특성을 보이나, 저온에서 p-type으로 변하는 특성을 보였고 n-doping의 경우 5e17/$cm^3$까지는 전자 이동도만 감소하고, doping에 의한 효과는 크게 없었다. 1e18/$cm^3$의 높은 doping을 할 경우 carrier가 증가하는 것을 확인했다. 이상의 측정 결과로 Spin-FET 소자로서 아주 우수하다는 것을 확인할 수 있었고 n-/p- type이 특성을 고려한 high quality InSb 박막소자의 응용을 위한 중요한 정보를 얻을 수 있었다.

• Journal of Astronomy and Space Sciences
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• v.21 no.4
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• pp.391-398
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• 2004

Far-ultraviolet Imaging Spectrograph (FIMS) is the main payload of the Korea's first scientific micro satellite STSAT-1, which was launched at Sep. 27 2003 successfully. Major objective of FIMS is observing hot gas in the Galaxy in FUV bands to diagnose the energy flow models of the interstellar medium. Supernova remnants, molecular clouds, and Aurora emission in the geomagnetic pole regions are specific targets for pointing observation. Although the whole system was calibrated before launch, it is essential to perform on-orbit calibration for data analysis. For spectral calibration, we observed airglow lines in the atmosphere since they provide good spectral references. We identify and compare the observed airglow lines with model calculations, and correct the spectral distortion appeared in the detector system to improve the spectral resolution of the system.

• Journal of Astronomy and Space Sciences
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• v.21 no.4
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• pp.283-294
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• 2004

New BV RI photometric observations of the contact binary AH Tau were performed with the 61 cm reflector and a 2K CCD camera at the Sobaeksan Optical Astronomy Observatory during seven nights from September to December, 2001. A total of 144 times of minima observed up to date, including three times of minima obtained from our observation, were analyzed. It is found that the orbital period of AH Tau has varied in a cyclic way superposed on a secular period decrease. The rate of the secular period decrease is calculated to be $1^s$ .04 per century, implying that a mass of about $3.8{\times}10^{-8}M{\odot}/yr$ from the more massive primary flows into the secondary if a conservative mass transfer is assumed. Assuming that the sinusoidal period variation is produced by a light-time effect due to an unseen third body, the resultant semi-amplitude, period, and eccentricity for the deduced light-time orbit are obtained as 35.4 years, 0.014 day and 0.52, respectively. The mass of the third-body is calculated as a tout $0.24M{\odot}$ when the third body is assumed to be coplanar with AH Tau system.

• Journal of Satellite, Information and Communications
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• v.1 no.2
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• pp.95-100
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• 2006

The COMS(Communication, Ocean and Meteorological Satellite) EPS(Electrical Power Subsystem) is derived from an enhanced Eurostar 3000 version. Eurostar 3000 EpS is fully autonomous operation in nominal conditions or in the event of a failure and provides a high level of reconfigure capability. This paper introduces the COMS EPS preliminary design result. COMS EPS consists of a battery, a solar arrat wing, a PSR(Power Supply Regulator), a PRU(Pyrotechnic Unit), a SDAM(Solar Array Drive Mechanism) and relay and fuse brackets. COMS EPS can offer a bus power capability of 3 kW. The solar array is made of a deployable wing with two panels. One type fo solar cells is selected ad GaAs/Ge triple junction cells. Li-ion battery is base lined with ten series cell module of five cells in parallel. PSR associated to battery and solar array wing generates a power bus fully regulated at 50 V. Power bus os centralized protection and distribution by relay and fuse brackets. PRU provides power for firing actuarors devices. The solar array wing is rotated by the SADM under control of the attitude orbit control subsystem. The control and monitoring of the EPS, especially of the battery, is performed by the PSR in combination with the on-board software.

• Journal of Astronomy and Space Sciences
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• v.28 no.3
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• pp.163-172
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• 2011

An intensive analysis of 185 timings of WZ Cep, including our new three timings, was made to understand the dynamical picture of this active W UMa-type binary. It was found that the orbital period of the system has complexly varied in two cyclical components superposed on a secularly downward parabola over about 80y. The downward parabola, corresponding to a secular period decrease of $-9.{^d}97{\times}10^{-8}y^{-1}$, is most probably produced by the action of both angular momentum loss (AML) due to magnetic braking and mass-transfer from the massive primary component to the secondary. The period decrease rate of $-6.^{d}72{\times}10^{-8}y^{-1}$ due to AML contributes about 67% to the observed period decrease. The mass flow of about $5.16{\times}10^{-8}M_{\odot}y^{-1}$ from the primary to the secondary results the remaining 33% period decrease. Two cyclical components have an $11.^{y}8$ period with amplitude of $0.^{d}0054$ and a $41.^{y}3$ period with amplitude of $0.^{d}0178$. It is very interesting that there seems to be exactly in a commensurable 7:2 relation between their mean motions. As the possible causes, two rival interpretations (i.e., light-time effects (LTE) by additional bodies and the Applegate model) were considered. In the LTE interpretation, the minimum masses of $0.30M_{\odot}$ for the shorter period and $0.49M_{\odot}$ for the longer one were calculated. Their contributions to the total light were at most within 2%, if they were assumed to be main-sequence stars. If the LTE explanation is true for the WZ Cep system, the 7:2 relation found between their mean motions would be interpreted as a stable 7:2 orbit resonance produced by a long-term gravitational interaction between two tertiary bodies. In the Applegate model interpretation, the deduced model parameters indicate that the mechanism could work only in the primary star for both of the two period modulations, but could not in the secondary. However, we couldn't find any meaningful relation between the light variation and the period variability from the historical light curve data. At present, we prefer the interpretation of the mechanical perturbation from the third and fourth stars as the possible cause of two cycling period changes.