• 천문학회보
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• 제38권1호
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• pp.62.2-62.2
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• 2013

It is considered that comets near the ecliptic plane have been injected into inner solar system from Kuiper-belt. Some of them are still active while others are dormant with no detectable tails and comae. These dormant comets have eccentric and/or inclined orbits, which are parameterized by Tisserand parameter TJ<3. In addition, dormant comets can be differentiated from asteroids based on the albedo, because they have low albedo (the geometrical albedos pv<0.1). The conditions of TJ<3 and pv<0.1 have been used as a criteria to discriminate dormant comets from asteroids. However, we must be more careful because there are 'contaminations' from the outer region, i.e. Jovian Trojans (5.05

• 천문학회보
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• 제37권2호
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• pp.204.2-204.2
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• 2012

FPC (Fine-guiding and astroPhysics Camera)는 일본 ISAS/JAXA, 유럽 ESA에서 공동 개발하는 대형적외선우주망원경 SPICA (Space Infrared Telescope for Cosmology and Astrophysics)에 탑재하기 위하여 천문연이 주도하는 한국의 컨소시움에서 개발을 추진하고 있는 정밀 근적외선 카메라이다. FPC는 과학적 목적을 위한 FPC-S와 정밀 자세결정을 위한 FPC-G로 이루어져 있으며 관측 파장 대역은 0.7-5 um이다. FPC-G는 0.05 각초의 초정밀 자세 결정을 위한 기능을 갖추고 있으며, FPC-S는 선형변화필터 LVF (Linear Variable Filter) 등을 사용하여 Pop III stars, High-redshift 영역에서의 별탄생 및 은하 진화 과정에 대한 연구를 수행할 수 있다. FPC는 상대적으로 시스템 자원을 덜 소모하기 때문에, 다른 중 적외선 원적외선 기기와 동시 관측이 가능하다. 다른 기기들과의 잘 짜여진 협력 관측을 통하여, FPC의 활용도를 높일 계획이다.

• 한국추진공학회:학술대회논문집
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• 한국추진공학회 2004년도 제22회 춘계학술대회논문집
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• pp.687-692
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• 2004

For the prediction of sloshing in the propellant tank of rocket vehicle utilized in RVT (reusable rocket vehicle testing) conducted by ISAS/JAXA, the flow field in the propellant tank during the ballistic flight was experimentally reproduced with the sub-scale model of it. The lateral acceleration as large as about 0.8 G was provided with a mechanical exciter and the deformation of liquid surface in the vessel was visualized with a high-speed camera. The several con-figurations of damping devices were installed and tested in the vessel, which should keep the ullage gas away from the outlet port. It was consequently suggested that the combination of a baffle plate and a perforated cylinder could be effective against the gas suction before the re-ignition of the engine. The sloshing phenomena were also simulated with the CFD code, called CIP-LSM. The numerical results showed good agreement with the corresponding data obtained in the experiment.

• 한국항해항만학회:학술대회논문집
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• 한국항해항만학회 2006년도 International Symposium on GPS/GNSS Vol.2
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• pp.125-129
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• 2006

Japan has been investigating a new satellite based positioning system called Quasi-Zenith Satellite System (QZSS). Since the improvement of positioning availability in urban area is one of the most important advantages of the QZSS, multipath mitigation is a key factor for the QZSS positioning system. Therefore, Japan Aerospace Exploration Agency (JAXA) and GNSS Inc. have commenced the R&D of a pseudolite, which transmits the next-generation signal such as BOC(1,1), in order to evaluate the effect of multipath on the new signal. A prototype BOC pseudolite was developed in 2005, and ground tests showed a capability of generating proper pseudorange. Also, preliminary flight experiments using a pseudo quasi-zenith satellite, a helicopter on which the pseudolite is installed, were conducted in early 2006, and the BOC-type correlation function was monitored in real time.

• 한국수자원학회:학술대회논문집
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• 한국수자원학회 2018년도 학술발표회
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• pp.196-196
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• 2018

북한의 에너지 공급은 석탄과 수력 위주로 구성되어 있지만, 수력이 북한 발전량의 약 63%를 차지할 만큼 비중이 높다. 북한은 지리적으로 수력발전 개발에 많은 이점을 가지고 있는 만큼 북한 수자원 개발 사업에 진출하거나, 통일을 대비하기 위해 댐 개발 가능지역에 대한 검토가 필요하다. 본 연구에서는 댐 개발이 가능한 북한지역의 33개 유역에 대해 SWAT 모형을 활용하여 장기유출 모의를 수행하였다. 북한지역에 대한 직접적인 자료 획득이 어려운 현실에서 장기유출 모의를 위해 수치표고자료는 일본우주항공연구개발기구(JAXA)에서 제공하는 30 m DEM을 활용하였으며, 기상자료는 북한이 세계기상기구(WMO)에 제공한 자료를 이용하였고, 토지이용 및 토양 자료는 WaterBase에서 제공하는 자료를 활용하였다. 1988년부터 2017년 까지 30년간의 일 유출량을 모의하였으며, 연간발전가능량 계산을 위한 사용수량은 해당 유역의 풍수량을 사용하였으며, 수차효율과 발전기효율의 합성효율은 댐 설계기준에서 제시한 계획단계의 85%를 적용하였다. 유효낙차와 발전능률은 기존 연구에서 제시한 92%와 66%를 적용하였다. 본 연구에서 추정한 북한 지역의 개발 가능한 댐의 연간발생전력량은 향후 수자원분야의 북한 진출을 위한 기초자료로 활용될 수 있을 것이다.

• 천문학논총
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• 제32권1호
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• pp.163-167
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• 2017

Utilizing a unique capability of AKARI that allows deep spectroscopy at $2.5-5.0{\mu}m$, we performed a spectroscopy study of more than 200 quasars through one of the AKARI mission programs, QSONG (Quasar Spectroscopic Observation with NIR Grism). QSONG targeted 155 high redshift (3.3 < z < 6.42) quasars and 90 low redshift active galactic nuclei (0.002 < z < 0.48). In order to provide black hole mass estimates based on the rest-frame optical spectra, the high redshift part of QSONG is designed to detect the $H{\alpha}$ line and the rest-frame optical spectra of quasars at z > 3.3. The low redshift part of QSONG is geared to uncover the rest-frame $2.5-5.0{\mu}m$ spectral features of active galactic nuclei to gain useful information such as the dust-extinction-free black hole mass estimators based on the Brackett lines and the temperatures of the hot dust torus. We outline the program strategy, and present some of the scientific highlights from QSONG, including the detection of the $H{\alpha}$ line from a quasar at z > 4.5 which indicates a rigorous growth of black holes in the early universe, and the $Br{\beta}$-based black hole mass estimators and the hot dust temperatures (~ 1100 K) of low redshift AGNs.

• 천문학논총
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• 제32권1호
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• pp.239-244
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• 2017

How does the presence of an AGN influence the total SFR estimates of galaxies and change their distribution with respect to the Galaxy Main Sequence? To contribute to solving this question, we study a sample of 1133 sources detected in the North Ecliptic Pole field (NEP) by AKARI and Herschel. We create a multi-wavelength dataset for these galaxies and we fit their multi-wavelength Spectral Energy Distribution (SED) using the whole spectral regime (from 0.1 to $500{\mu}m$). We perform the fit using three procedures: LePhare and two optimised codes for identifying AGN tracers from the SED analysis. In this work we present an overview of the comparison between the estimates of the Infrared bolometric luminosities (between 8 and $1000{\mu}m$) and the AGN fractions obtained exploiting these different procedures. In particular, by estimating the AGN contribution in four different wavelength ranges ($5-40{\mu}m$, $10-20{\mu}m$, $20-40{\mu}m$ and $8-1000{\mu}m$) we show how the presence of an AGN affects the PAH emission by suppressing the ratio $\frac{L_{8{\mu}m}}{L_{4.5{\mu}m}}$ as a function of the considered wavelength range.

• 천문학논총
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• 제32권1호
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• pp.131-133
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• 2017

We present the latest results from the Mission Program NIRLT (PI: I.Yamamura), the near-infrared spectroscopy of brown dwarfs using the AKARI/IRC grism mode with the spectral resolution of ~ 120. The near-infrared spectra in the wavelength range between 2.5 and $5.0{\mu}m$ are especially important to study the brown dwarf atmospheres because of the presence of major molecular bands, including $CH_4$ at $3.3{\mu}m$, $CO_2$ at $4.2{\mu}m$, CO at $4.6{\mu}m$, and $H_2O$ around $2.7{\mu}m$. We observed 27 sources, and obtained 16 good spectra. Our model fitting reveals deviations between theoretical model and observed spectra in this wavelength range, which may be attributed to the physical condition of the upper atmosphere. The deviations indicate additional heating, which we hypothesize to be due to chromospheric activity. We test this effect by modifying the brown dwarf atmosphere model to artificially increase the temperature of the upper atmosphere, and compare the revised model with observed spectra of early- to mid-L type objects with $H{\alpha}$ emission. We find that the chemical structure of the atmosphere changes dramatically, and the heating model spectra of early-type brown dwarfs can be considerably improved to match the observed spectra. Our result suggests that chromospheric activity is essential to understand early-type brown dwarf atmospheres.

• 천문학회보
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• 제41권2호
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• pp.37.2-37.2
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• 2016

MIRIS (Multi-purpose InfraRed Imaging System) is a compact near-infrared space telescope launched in 2013 November as the main payload of STSAT-3 (Science and Technology Satellite 3). The main missions of MIRIS are 1) the $Pa{\alpha}$ line survey along the Galactic plane, 2) the large area (${\sim}10^{\circ}{\times}10^{\circ}$) surveys of three pole regions (north ecliptic pole, and north and south Galactic poles), and 3) the monitoring observations toward the north ecliptic pole. MIRIS started observations for the main missions in 2014 March and finished in 2015 May. While MIRIS was taking the observation data and afterward, we are continuing the analysis of data. Based on the results from analysis, the data reduction pipeline has been revised. In this talk, we introduce the revised version of the MIRIS data reduction pipeline and the status of the data reduction and anlaysis.

• 천문학회보
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• 제41권2호
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• pp.67.3-68
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• 2016

An X1.6 flare occurred in AR 12192 on 2014 October 22 around 14:06 UT and was observed by Hinode, IRIS, SDO and RHESSI. We analyze a bright kernel which produces a white light flare (WLF) with continuum enhancement and a hard X-ray (HXR) peak. Taking advantage of the spectroscopic observations of IRIS and EIS, we measure the temporal variation of the plasma properties in the bright kernel in the chromosphere and corona. We found that explosive evaporation was observed when the WLF occurred, even though the intensity enhancement in hotter lines is quite weak. The temporal correlation of the WLF, HXR peak, and evaporation flows indicates that the WLF was produced by accelerated electrons. To understand the white light emission processes, we calculated the deposited energy flux from the non-thermal electrons observed by RHESSI and compared it to the dissipated energy estimated from the chromospheric lines (Mg II triplet) observed by IRIS. The deposited energy flux from the non-thermal electrons is about $3.1{\times}10^{10}erg\;cm^{-2}s^{-1}$ when we assume a cut-off energy of 20 keV. The estimated energy flux from the temperature changes in the chromosphere measured from the Mg II subordinate line is about $4.6-6.7{\times}10^9erg\;cm^{-2}s^{-1}$, 15 - 22 % of the deposited energy. By comparison of these estimated energy fluxes we conclude that the continuum enhancement was directly produced by the non-thermal electrons.