• 천문학논총
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• 제32권1호
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• pp.77-81
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• 2017

A wide spectral coverage from near-infrared (NIR) to far-infrared (FIR) of AKARI both for imaging and spectroscopy enables us to efficiently study the emission from gas and dust in the interstellar medium (ISM). In particular, the Infrared Camera (IRC) onboard AKARI offers a unique opportunity to carry out sensitive spectroscopy in the NIR ($2-5{\mu}m$) for the first time from a spaceborn telescope. This spectral range contains a number of important dust bands and gas lines, such as the aromatic and aliphatic emission bands at 3.3 and $3.4-3.5{\mu}m$, $H_2O$ and $CO_2$ ices at 3.0 and $4.3{\mu}m$, CO, $H_2$, and H I gas emission lines. In this paper we concentrate on the aromatic and aliphatic emission and ice absorption features. The balance between dust supply and destruction suggests significant dust processing taking place as well as dust formation in the ISM. Detailed analysis of the aromatic and aliphatic bands of AKARI observations for a number of H ii regions and H ii region-like objects suggests processing of carbonaceous dust in the ISM. The ice formation process can also be studied with IRC NIR spectroscopy efficiently. In this review, dust processing in the ISM divulged by recent analysis of AKARI data is discussed.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2006년도 한국우주과학회보 제15권2호
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• pp.177-180
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• 2006

우리은하 중심부의 Sgr A East에 인접한 별탄생 지역인 수소이온화영역 A주변에서 충격파가 별탄생에 미치는 영향을 조사하기 위하여 $2.1218{\mu}m$ 수소분자 방출선($H_2$ 1-0 S(1))을 관측하였다. 관측은 3.8m United Kingdom Infrared Telescope(UKIRT)에서 에셀 분광 모드의 Cooled Grating Spectrometer 4(CGS4)를 사용하여 각분해능 약 2arcsec, 파장 분해능 약 18km s^{-1}$으로 수행 되었다. 검출된 수소분자선을 공간적인 구조와 속도 분포의 측면에서 각각 전파 연속선 방출광 및 암모니아 방출광과 비교한 결과, 수소분자 방출광은 Sgr A East의 충격파와 무관하며 수소이온화영역 자체의 분자해리영역에서 방출된 것이라는 결론에 도달하였다. 이는 해당 지역에서의 별탄생이 Sgr A East의 충격파에 의해 촉발된 것이 아니라는 것을 의미한다.

• 한국대기환경학회지
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• 제17권6호
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• pp.451-461
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• 2001

Backward trajectories were calculated from five urban areas in Korea in 1999 in order to assess the effects of long-range transport on the air quality variations on an annual basis. The five areas selected were Seoul, Mokpo, Cheju, Pohang, and Kangnung, which are evenly distributed along the shoreline in Korea. Meteorological fields used in the work were prepared by the Korea Meteorological Administration using the RDAPS(Regional Data Assimilation and Prediction System) with grid spacing of 40 km and 12-h intervals(0000 and 1200 UTC). Upwind regions around the Korean Peninsula were divided into five sectors including the region to the northeast(I), northern China (II), southern China(III), the northwestern Pacific(IV), and Japan(V). The influence of air flow from these sectors on the variations of carbon monoxide concentrations in the selected areas was investigated. The results showed that the influences of Sectors II and III were persistent although some influences of adjacent sectors were observed according to the location of the areas. In general, the concentration of carbon monoxide tended to go up under the influence of Sectors II and III but tended to go down under the influence of Sector I. However, the influences of other sectors were rather mixed. The importance of the long-range transport was examined when the whole country was uniformly influenced by Sectors II and III with strong synoptic winds. The effects of long-range transport were large in Mokpo and Cheju, close to Sectors II and III, where the local emissions were considered small. The effects of local emissions were significant in Pohang and Seoul; such effect was more distinct in Pohang located farther from Sectors II and III.

• 한국지구과학회지
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• 제27권5호
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• pp.569-578
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• 2006

CFHT 천문대 3.6 m 망원경에 부착된 OASIS 분광기를 사용하여 얻은 자료로부터 continuum, $H{\alpha},\;H{\beta}$, [O III], [N II] 등의 영상을 만들어 활동 은하핵 NGC 5728의 물리적 특성을 분석하였다. NGC 5728의 중심부에 NLR 영역으로 판단되는 약 $15"{\times}12"$ 범위 영역에 3개의 밝은 부분(NW knot, SE knot, nucleus)이 존재하고 있고, 이는 핵(nucleus)을 중심으로 북서방향이나 서쪽으로 물질의 흐름이 일어나고 있음을 암시한다. 우리는 직경 10"인 ring과 이의중심에 있는 NW knot의 구조가 은하중심과 일치하지 않음을 발견하였다. 우리는 이러한 구조의 생성 원인에 대해 알아보기 위하여 핵과 knot의 운동학적 특성을 비교하여 보았고, 방출선 영상에서 보이는 차이점을 비교함으로써 활동 은하 중심부의 구조를 살펴보았다.

• 천문학회보
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• 제44권2호
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• pp.51.1-51.1
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• 2019

At the commissioning phase of KVN from 2009 to 2013, single-dish survey and monitoring observations were performed toward about 1000 evolved stars and about 60 relatively strong SiO and H2O maser sources respectively. Based on these single-dish results and VLBI feasibility test observations at K/Q/W/D bands in 2014, KVN Key Science Project (KSP) has started from 2015 and will be completed in 2019 as KSP phase I. Here we present the overview of observational studies on evolved stars using KVN. In KSP phase I, we have focused on nine KSP sources which show a successful astrometrically registered maps of SiO and H2O masers using the source frequency phase referencing method. We aim at investigating the spatial structure and dynamical effect from 43/42/86/129 GHz SiO to 22 GHz H2O maser regions associated with a stellar pulsation and development of asymmetry in circumstellar envelopes. Using the combined network KaVA (KVN+Japanese VLBI network VERA), KaVA Large Program titled on "Expanded Study on Stellar Masers: ESTEMA Phase I" was performed from 2015 to 2016. Based on ESTEMA Phase I, EAVN Large Program titled on "EAVN Synthesis of Stellar Maser Animations: ESTEMA Phase II" was also performed from 2018. The ESTEMA II project aims to publish composite animations of circumstellar H2O and SiO masers, which taken from up to 6 long-period variable stars with a variety of the pulsation periods (333-1000 days). The animations will exhibit the three-dimensional kinematics of the maser gas clumps with complexity caused by stellar pulsation-driven shock waves and anisotropy of clump ejections from the stellar surface. Adding three EAVN telescopes (Tianma 65m, Nanshan 26m and NRO 45m telescopes) with KaVA always secures the high quality of the maser image frames through the monitoring program.

• 한국응용곤충학회지
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• 제37권1호
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• pp.23-30
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• 1998

DNA의 제한요소단편 다형현상(RFLP)이 유전변이 연구에 널리 이용되고 있다. 본 연구는 파밤나방(Spodoptera exigua(H bner)) 미토콘드리아 DNA(mtDNA)의 RFLP방법을 개발하기 위해 게놈 크기 측정 및 PCR primer들을 선발하였다. 파밤나방의 mtDNA 전체크기는 약 16kb였다. 대부분 곤충 mtDNA에 적합하게 구성된 (Simon et al., 1994)29개 promer들중 21개가 파밤나방의 mtDNA증폭에 적합했다. 이들 primer들을 이용하여 여러 유전자 영역(CO-I, CO-II, Cyt-B, ND-1, 12S rRNA, 16S rRNA 및 일부 tRNA)의 일분 또는 전체를 포함하는 유전자 절편을 증폭시켰다. 일반적으로 다형을 보이는 primer조합을 중심으로 4염기 제한부위를 인식하는 8종의 제한 효소를 통해 분석된 PCR-RFLP는 서로 다은 지역(안동, 경산, 순천) 집단들간에 제한부위에 있어서 차이가 없었으나 일부 영역에서는 길이 차이를 보여 유용한 유전지표로서의 가능성을 제시했다.

• 천문학회보
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• 제38권2호
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• pp.92.1-92.1
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• 2013

In this study, we examined chromospheric oscillation signatures in two solar active regions, a limb active region and a sunspot with a light bridge, observed by the Fast Imaging Solar Spectrograph (FISS) of the 1.6m New Solar Telescope (NST) at Big Bear Solar Observatory. The FISS is a slit spectrograph with a fast imaging capability and can observe the solar chromosphere in $H{\alpha}$ and Ca II $8542{\AA}$ bands simultaneously with high spectral resolutions. After dark and flat correction, we compensated for image rotation at the Coude focus and made image alignment. We estimated Doppler shifts over active regions using the bisector method and investigated the temporal and spatial fluctuations of Doppler shifts for some selected cases. And we obtain the power map by using the Lomb-Scargle periodogram technique to examine the oscillation power at different features. Finally, we will discuss our results and implications.

• 천문학회보
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• 제44권1호
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• pp.44.3-44.3
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• 2019

Massive stars, supernovae, and kilonovae are among the most luminous radiation sources in the universe. Observations usually show near- to mid-infrared (NIR-MIR, 1-5~micron) emission excess from H II regions around young massive star clusters (YMSCs) and anomalous dust extinction and polarization towards Type Ia supernova (SNe Ia). The popular explanation for such NIR-MIR excess and unusual dust properties is the predominance of small grains (size a<0.05micron) relative to large grains (a>0.1micron) in the local environment of these strong radiation sources. The question of why small grains are predominant in these environments remains a mystery. Here we report a new mechanism of dust destruction based on centrifugal stress within extremely fast rotating grains spun-up by radiative torques, namely the RAdiative Torque Disruption (RATD) mechanism, which can resolve this question. We find that RATD can destroy large grains located within a distance of ~ 1 pc from a massive star of luminosity L~ 10^4L_sun and a supernova. This increases the abundance of small grains relative to large grains and successfully reproduces the observed NIR-MIR excess and anomalous dust extinction/polarization. We show that small grains produced by RATD can also explain the steep far-UV rise in extinction curves toward starburst and high redshift galaxies, as well as the decrease of the escape fraction of Ly-alpha photons observed from HII regions surrounding YMSCs.

• 천문학회보
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• 제40권1호
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• pp.47.1-47.1
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• 2015

We present an optical spectroscopic study of 28 supernova remnant (SNR) candidates in M81 and two SNR candidates in M82. The optical spectra of these SNR candidates were obtained using the MMT/Hectospec as a part of the K-GMT Science Program. Based on the [S II]/$H{\alpha}$ ratio and the radial velocity, we find that twenty six out of the M81 candidates are genuine SNRs. Two SNR candidates in M82 are thought to be shocked condensations in the galactic outflow or SNRs. In the spectral line ratio diagrams, M81 SNRs are divided into two groups: an [O III]-strong group and an [O III]-weak group. The [O III]-weak SNRs have larger sizes, and may have faster shock velocity. We estimate the nitrogen and oxygen abundance of the SNRs from the comparison with shock-ionization models. We find a radial gradient in nitrogen abundance, $dLog(N/H)/dlogR=-0.023{\pm}0.009\;dex\;kpc^{-1}$ little evidence for the gradient in oxygen abundance. The nitrogen abundance shows shallower gradient than those of the planetary nebulae and H II regions of M81. We find five X-ray emitting SNRs. Their X-ray hardness colors are consistent with thermal SNRs.

• 한국초전도학회:학술대회논문집
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• 한국초전도학회 1999년도 High Temperature Superconductivity Vol.IX
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• pp.280-290
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• 1999

The microstructures of a Tl$_{0.8}Pb_{0.2}Bi_{0.2}Sr_{1.6}Ca_2Cu_3O_{9+{\delta}}$/Ag tape (tape I ) with J$_c$ of 17,600 A/cm$^2$ at 77 K and 0 T and three Tl$_{0.8}Pb_{0.2}Bi_{0.2}Sr_{1.8}Ba_{0.2}Ca_{2.2}Cu_3O_{9+{\delta}}$/Ag tapes with J$_c$'s of 9,300 (tape II), 16,700 (tape III) and 25,200 A/cm$^2$ (tape IV)prepared using the powder-in-tube method and an in-situ reaction method, were investigated using scanning electron microscopy and high-resolution transmission electron microscopy, and compared each other. ln the tape preparation, an intermediate rolling process was incorporated during final heat-treatment for the last tape, but not for the rest of the tapes. The microstructural analysis revealed clear differences in grain-texturing, crystallographic defects and impurity phases, depending on the chemical composition of the tape. Tendency of directional grain-alignment increased in an order of tapes I, II III and IV. In tape IV, T1-1223 grains are textured, at least in local regions. In crystallographic defects, while stacking faults were prevalent in the former composition, dislocations and voids were frequently observed in the latter. Also impurity phases were appeared to be more abundant in the former than in the latter. The relationship between 1,and the microstructure in the tapes was attempted to explain in a term of grain-linking.