• Journal of Astronomy and Space Sciences
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• v.16 no.2
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• pp.293-306
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• 1999

Solar activities ejecting high energy particles influence satellites and satellite communications as well as perturb geomagnetic fields. To understand space environments near the Earth being influenced by the Sun, we must study about the magnetosphere, the ionosphere, and the atmosphere beforehand. To study this issue, we investigate some ionospheric models, atmospheric models and geomagnetic field models : IRI(International Reference Ionosphere), PIM(Parameterized Ionospheric Model) and IGRF(International Geomagnetic Reference Field). We develop the models and build a web site to serve IRI, PIM and IGRF model on the internet so that one can easily get information of daily and global ionospheric and geomagnetic variations.

• Publications of The Korean Astronomical Society
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• v.22 no.3
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• pp.83-87
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• 2007

We designed the Intermediate Frequency(IF) distributor for multi beam backend system and manufactured Voltage to Frequency Converter(VFC) to measure the multi-beam receiver performance. Multi beam receiver has 15 channel receivers and can get 15 spectrums at once. The multi beam receiver has more observation efficiency than single beam receiver. We manufactured the 15 IF distributors to distribute IF signal for Autocorrelation spectrometer that is radio signal processor. Also, we manufactured the VF Converter to test the performance measurement of receiver for Korea VLBI Network(KVN) system which is under-construct in Seoul, Ulsan and Jeju. As a result of performance measurement, we could obtain linearity of 99.4% on the input power vs output frequency and measured the operating range of input frequency.

• Journal of the Korean Institute of Telematics and Electronics B
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• v.31B no.9
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• pp.67-75
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• 1994

In this paper, we manufactured the continuum receiver system for observing the continuum waves emitted from the continuum sources with using the 14m radio-telescope. The receiving system measures the total power of the continuum sources and consists of DC-amplifier, beam-chopper system. Phase-Locked Loop(PLL) circuit, blanking circuit and its period selection circuit, V/F converter, and counter part which are capable of interfacing with the computer which is used for a data acquisition and making the radio-telescope track the source. We compared the obsevation results which use the existing DVM method with the observation results which use the continuum receiver to measure the total power of the sources. Moreover, by method of beam switching observation which uses newly installed beam chopper system. We can significantly improve the observational efficiency more than the existing position switching observation method.

• Journal of the Korean Institute of Telematics and Electronics A
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• v.33A no.6
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• pp.90-98
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• 1996

We have evaluated the theoretical conversion loss and noise temperature of mixer using the quantum mixer theory and the method to determine the embedding impedance of waveguide-type mixer mount. At fixed backshort position of the mixer, the calculated SSB mixer conversion loss and mixer noise temperature are 5 dB and 10K within frequency range form 85 GHz to 115 GHz, respectively. The SIS mixer has been developed by using through on the calculated rsutls to observe cosmic radio waves. SIS junction of mixer is Nb/Al-AlOx/Nb and it consists of four series array. Area of each of junction is about 2.5${\mu}m^{2}$. The average receiver noise temperature of manufactured receiver with this mixer is about 30 K(DSB). The receiver noise temperature is much lower than that of receiver with a mixer using mechanical tuning backshort.

• Publications of The Korean Astronomical Society
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• v.8 no.1
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• pp.1-15
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• 1993

We made a pyramidal horn antenna system for 21cm cosmic radio wave. The antenna system has a rectangular waveguide with $TE_{10}$ mode and a copper probe to detect the electromagnetic wave in waveguide. The parameters of the probe are obtained by experiments using two waveguides. Pyramidal horn antenna is designed to get a gain of 20dB. The size of the aperture of this horn is $94cm{\times}74cm$. The beam width of half power is about $14.7^{\circ}$ for the frequency of 1.4GHz. The horn is made of aluminum plate with a thickness of 2mm. The signal from horn and waveguide is amplified in a receiver system and is converted into DC in the detecter. The intensity of the signal is recorded on a chart recorder. We observed the sun using this simple radio telescope and obtained the brightness temperature of $2.2{\times}10^5K$, which indicates that the sun is quiet at 21cm.

• Journal of the Korean Society for Aeronautical & Space Sciences
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• v.30 no.7
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• pp.61-67
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• 2002

In this study a control surface/actuator fault detection, identification, and accommodation system for aircraft is designed. This fault tolerant control system tries to return aircraft to its stable trim condition in a short time. The control system is designed using neural networks with Extended Back Propagation Algorithm which shows fast convergence. F-4 aircraft with possible stabilator or aileron failure/stuck is simulated with the proposed scheme.

• The Bulletin of The Korean Astronomical Society
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• v.41 no.1
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• pp.31.1-31.1
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• 2016

중력파의 존재가 예측된 것은 100년전 일이지만 지난해 9월 14일에야 LIGO에 처음으로 직접 검출되었다. 줄력파는 질량을 가진 물질이 가속될 때 만들어져 빛의 속도로 전파되는 현상이다. LIGO는 레이저 간섭 현상을 이용해 서로 수직인 방향의 두 팔의 길이가 상대적으로 진동하는 것을 측정하는 기기로서 지난 2002년 첫 관측을 시작한 이래 지속적인 감도 향상을 통해 아주 미세한 진폭을 가지는 중력파를 직접 검출하는데 성공하였다. 이번에 관측된 중력파는 두개의 블랙홀로 이루어진 쌍성이 궤도 운동을 하면서 중력파를 방출함에 따라 궤도 반지름이 점차 줄어들어 궁극적으로 충돌하기 직전 0.1초 정도 사이에 방출한 것으로서 이론적인 파형과의 비교를 통해 기존의 어떤 방법보다도 정확하게 블랙홀들의 질량과 거리를 측정할 수 있게 해 주었다. LIGO의 감도가 앞으로도 더욱 향상될 것이며 이에 따라 더 많은 중력파 천체가 발견될 것이다. 중력파 관측을 통해 우리는 기존의 망원경으로 볼 수 없었던 새로운 천체 현상을 자구 관측하게 될 것이며 이에 따라 블랙홀이나 중성자별과 같은 밀집 천체를 더 자세하게 탐구할 수 있을 뿐 아니라 우주의 구조나 진화에 대한 새로운 연구가 가능해질 것이다.

• Journal of Aerospace System Engineering
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• v.4 no.3
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• pp.24-28
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• 2010

The purpose of this study is to define available microwave absorbing structure for aircraft from in the X-band(8.2~12.4GHz) frequencies. The electromagnetic wave absorption or shielding techniques is an important issue not only for military purpose but also for commercial purposes. Aircraft Radar Absorbing Structure(RAS) is absorbed or scattered propagation waves from the enemy radar. There are absorbing technologies at shaping design techniques and using Radar Absorbing Materials(RAM). RAM is more important because shaping design can't include perfect radar absorbing performance. In this study, based on material properties was introduced RAM and to analyze the each characteristics. Finally, we comparison appropriate RAM for aircraft.

• The Science & Technology
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• v.31 no.3 s.346
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• pp.29-31
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• 1998

1958년 어느날 하버드대 대학원생 프랭크 드레이크는 세계최초의 전파망원경을 황소자리의 플레이아테스 별떼를 겨냥하고 있었따. 이윽고 수신장치에는 초당8개의 필스로 된 신호가 들어와다. 외계지능이 보낸 신호로 알고 크게 들뜬 이 신출내기 천문학자는 "인류는 우주에서 외로운 존재가 아니다"라는 생각에서 한순간 두려운 가운데도 기뻐서 어쩔줄을 몰랐다. 그러나 얼마 뒤 망원경을 플레이아테스에서 떼었을때도 수신기에는 여전히 같은 신호가 들어왔다. 결국 이 신호는 가까운 곳을 지나는 항공기에서 온 것이라고 추정하게 되었으나 이런 사건을 계기로 드레이크는 '외계지능탐사'에 평생을 걸게된다.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.42.1-42.1
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• 2010

한국천문연구원 한국우주전파관측망(KVN)은 2008년 KVN연세-VERA 간의 프린지 검출에 이어, 2009년 10월 KVN 모든 기선 간의 22GHz와 43GHz 프린지 검출에 성공하였다. 본 발표에서는 KVN 프린지 검출 시험의 과정과 결과를 요약하고, 또한 현재 수행 중인 KVN의 두 주파수 동시 VLBI 시험관측의 진행과정을 보고 하고자 한다.