• 대기
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• 제28권3호
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• pp.317-324
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• 2018

In this study, we review the ground-based whole-sky camera (WSC), which is developed to continuously capture day and night cloud images using the illumination data from a precision Lightmeter with a high temporal resolution. The WSC is combined with a precision Lightmeter developed in IYA (International Year of Astronomy) for analysis of an artificial light pollution at night and a DSLR camera equipped with a fish-eye lens widely applied in observational astronomy. The WSC is designed to adjust the shutter speed and ISO of the equipped camera according to illumination data in order to stably capture cloud images. And Raspberry Pi is applied to control automatically the related process of taking cloud and sky images every minute under various conditions depending on illumination data from Lightmeter for 24 hours. In addition, it is utilized to post-process and store the cloud images and to upload the data to web page in real time. Finally, we check the technical possibility of the method to observe the cloud distribution (cover, type, height) quantitatively and objectively by the optical system, through analysis of the captured cloud images from the developed device.

• 천문학회지
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• 제43권6호
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• pp.183-190
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• 2010

According to the historical documents and paintings in many civilizations, rocks that fell from the sky fascinated humans as the message from the God or supernaturals. Scientific progress allows humans to recognize these exciting extraterrestrial objects as meteorites. Meteorites contain a wealth of pivotal information regarding formation of the early Solar System. Meteorites also provide broader scientific insights on, for example, the origin of life, interplanetary transfer of life forms, massive depletion of biosphere on Earth, and evolution of lithosphere on Earth-like planetary bodies.

• 천문학회보
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• 제37권2호
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• pp.108.1-108.1
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• 2012

Previously we introduced ray-tracing based 3D optical earth system model for specular and scattering properties of all components of the system (i.e. clear-sky atmosphere, land surfaces and an ocean surface). In this study, we enhanced 3-dimensional atmospheric structure with vertical atmospheric profiles for multiple layer and cloud layers using Lambertian and Mie theory. Then the phase dependent disk averaged spectra are calculated. The main results, simulated phase dependent disk averaged spectra and light curves, are compared with the 7 bands(300~1000nm) light curves data of the Earth obtained from High Resolution Instrument(HRI) in Deep Impact spacecraft during Earth flyby in 2008. We note that the results are comparable with the observation.

• Advances in aircraft and spacecraft science
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• 제9권5호
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• pp.449-462
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• 2022

Space-telescopes placed in the Sun-Earth second Lagrange point (L2) observe the sky following a scan strategy that is usually based on a spin-precession motion. Knowing which regions of the sky will be more observed by the instrument is important for the science operations and the instrument calibration. Computing sky observation parameters numerically (discretizing time and the sky) can consume large amounts of time and computational resources, especially when high resolution isrequired.This problem becomesmore critical if quantities are evaluated at detector level instead of considering the instrument entire Field of View (FoV). In previous studies, the authors have derived analytic solutions for quantities that characterize the observation of each point in the sky in terms of observation time according to the scan strategy parameters and the instrument FoV. Analytic solutions allow to obtain results faster than using numerical methods as well as capture detailed characteristics which can be overseen due to discretization limitations. The original approach is based on the analytic expression of the instrument trace over the sky. Such equations are implicit and thusrequiresthe use of numeric solversto compute the quantities.In this work, a new and simpler approach for computing one ofsuch quantities(mean observation time) is presented.The quantity is first computed for pure spin motion and then the effect of the spin axis precession is incorporated under the assumption that the precession motion is slow compared to the spin motion.In this sense, this new approach further simplifies the analytic approach, sparing the use of numeric solvers, which reduces the complexity of the implementation and the computing time.

• 대한원격탐사학회지
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• 제28권1호
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• pp.121-128
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• 2012

조간대 지역의 고해상 지형도는 해수 운동에 의한 퇴적 및 침식량의 변화와 같이 과학적인 연구의 기초자료로 쓰일 뿐만 아니라 연안 습지의 실제적인 관리 및 환경변화 모니터링의 도구로서도 그 활용의 가치가 높다. 그러나 조간대는 하상 퇴적물의 유입과 조석현상에 의해 빠르게 변화하고 있어 원격탐사와 같이 단기간에 넓은 지역을 조사할 수 있는 기술의 적용이 필요하다. 레이더 간섭기술은 가장 보편적이면서 성공적인 고해상 지형도 작성 기술로 알려져 있으나, 조간대에서는 지표노출시간의 제약 및 빠른 상태변화로 인해 일반적인 repeat-pass 간섭기술로는 충분한 긴밀도를 얻기 힘들다. 이 연구에서는 재방문주기가 짧은 Cosmo-SkyMed 1일 간격 관측자료와 ERS2-ENVISAT 30분 간격 관측자료를 이용하여 레이더 간섭기술을 이용한 조간대 지형도 작성을 실험하였다. 두 자료 모두 긴 수직기선으로 인한 높은 고도민감도와 짧은 관측주기로 인한 높은 긴밀도로 간섭위상을 구할 수 있었으나, Cosmo-SkyMed 관측자료에서는 대기에 의한 위상지연 효과와 조석에 의한 조간대 표층의 함수율 변화로 인하여 조간대와 같이 평평한 지역의 지형정보를 추출하는데에 어려움이 발생한다. 반면에 ERS2-ENVISAT 관측자료는 이종센서간의 관측중심주파수 차이를 상쇄하기 위해 설정된 긴 수직기선 덕분에 매우 높은 고도민감도를 가지며, 30분이라는 짧은 관측주기는 간섭쌍을 이루는 두 영상에 포함된 대기지연효과를 대부분 상쇄시키므로 조간대의 지형도 작성에 이상적인 자료로 판단된다.

• 천문학회보
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• 제41권2호
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• pp.49.3-50
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• 2016

Deep Ecliptic Patrol of the Southern Sky (DEEP-South) observations have been conducted officially during the off-season for exoplanet search since October 2015. Most of the allocated time for DEEP-South is devoted to targeted photometry, Opposition Census (OC), of Near Earth Asteroids (NEAs) to increase the number of such objects with known physical properties. It is efficiently achieved by multiband, time series photometry. This Opposition Census (OC) mode target objects near their opposition, with km-sized PHAs in the early stage and goes down to sub-km objects. Continuous monitoring of the sky with KMTNet is optimized for spin characterization of various kinds of asteroids, including binaries, satellites, slow/fast- and non-principal axis-rotators, and hence is expected to facilitate the debiasing of previously reported lightcurve observations. We present the preliminary lightcurves of NEAs from year one of the DEEP-South with our long term plan.

• 전기전자학회논문지
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• 제1권1호
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• pp.47-54
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• 1997

오늘날 통신은 인터넷 사용의 증가 멀티미디어 서비스의 요구등으로 인해 점차 다량의 정보를 정확하고 신속하게 전송하기 위한 고속의 데이터 전송시스템이 요구되고 없으며, 머지않아 지구상공 20km 지점의 성층권에 플랫폼이라 불리는 위성을 띄워 고속의 정보 서비스가 가능할 것이다. 이 시스템은 레이저광을 사용함으로써 높은 데이터 전송율을 갖는 광무선통신망을 구축할 수 있으나, 대기공간을 전송채널로 사용하기 때문에 대기효과로 인한 극복해야할 많은 문제점을 갖고 있다. 따라서 본 논문에서는 교란대기 하에서 교란대기 효과에 따른 데이터 전송율과 비트오류율을 제시함으로써 교란대기효과가 광 위성통신시스템에 미치는 영향을 고찰하고자 한다.

• 동의생리병리학회지
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• 제19권6호
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• pp.1483-1490
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• 2005

This study was written in order to help understanding of visible diagnosis of appearance(形). Visible diagnosis of appearance(形) is a very important factor of diagnosis and a first step of visible diagnosis. appearance(形) is closely connection with spirit(神), so is house of spirit(神). If we make a visible diagnosis of appearance(形), we know the prosperousness of energy and the relative seriousness of an illness. Spirit(神) is understood by appearances and movements of patient, and influenced by seasons, lands, human's relationship and the grade of age. By visible diagnosis of appearance(形), we can conclude existence or nonexistence of spirit(神), As comparing spirit(神) with appearance(形), we can decide good or bad prognoses. One man's own appearance(形) is determined by the five human type(五形人). There are very various points of changing form. As divided into principal groups, there are three main groups, that is, sky(天), earth(地) and man(人). The age and sex belong 治 the factor of sky(天), a direction and configuration of the ground(地形) belong to the factor of earth(地), the five human type(五形人) and white fatness(肥白) and black emaciation(黑瘦) belong to the factor of man(人).

• 한국지구과학회지
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• 제26권2호
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• pp.149-159
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• 2005

Simultaneous observations of MODIS (Moderate-resolution Imaging Spectroradiometer) onboard the Aqua and Terra satellites and weather station at ground near the Inchon International Airport (37.2-37.7 N, 125.7-127.2 E) during the period from December 2002 to September 2004 have been utilized in order to analyze the characteristics of satellite-observed infrared (IR) and visible data under fog and clear-sky conditions, respectively. The differences $(T_{3.7-11})$ in brightness temperature between $3.75{\mu}m\;and\;11.0{\mu}m$ were used as threshold values for remote-sensing fog (or low clouds) from satellite during day and night. The $T_{3.7-11}$ value during daytime was greater by about 21 K when it was foggy than that when it was clear, but during nighttime fog it was less by 1.5 K than during nighttime clear-sky. The value was changed due to different values of emission of fog particles at the wavelength. Since the near-IR channel at $3.7{\mu}m$ was affected by solar and IR radiations in the daytime, both IR and visible channels (or reflectance) have been used to detect fog. The reflectance during fog was higher by 0.05-0.6 than that during clear-sky, and varied seasonally. In this study, the threshold values included uncertainties when clouds existed above a layer of fog.

• 한국환경과학회지
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• 제16권3호
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• pp.261-267
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• 2007

In this study, the Slab Ocean Model (SOM) is coupled with an Atmospheric General Circulation Model (AGCM) which developed in University of Kangnung based on the land surface model of Biosphere-Atmosphere Transfer Scheme (BATS). The purposes of this study are to understand radiative role of clouds considering of the atmospheric feedback, and to compare the Clouds Radiative Forcing (CRF) come from the analyses using the clear-cloud sky method and CGCM. The new CGCM was integrated by using two sets of the clouds with radiative role (EXP-A) and without radiative role (EXP-B). Clouds in this two cases show the negative effect $-26.0\;Wm^{-2}$ of difference of radiation budget at top of atmosphere (TOA). The annual global means radiation budget of this simulation at TOA is larger than the estimations ($-17.0 Wm^{-2}$) came from Earth Radiation Budget Experiment (ERBE). The work showed the surface negative effect with $-18.6 Wm^{-2}$ in the two different simulations of CRF. Otherwise, sensible heat flux in the simulation shows a great contribution with positive forcing of $+24.4 Wm^{-2}$. It is found that cooling effect to the surface temperature due to radiative role of clouds is about $7.5^{\circ}C$. From this study it could make an accurate of the different CRF estimation considering either feedback of EXP-B or not EXP-A under clear-sky and cloud-sky conditions respectively at TOA. This result clearly shows its difference of CRF $-11.1 Wm^{-2}$.