• Journal of the Korean Vacuum Society
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• v.15 no.5
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• pp.458-464
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• 2006

The construction and the performance test of an ultra high vacuum (UHV) molecular beam epitaxy (MBE) system has been completed successfully. We have done domestic development and tried performance test for ultra high vacuum molecular beam epitaxy system. This system has reached pressure $2X10-^{10}$ Torr and the substrate has reached temperature $1,100^{\circ}C$. We have investigated into the characteristic of ZnSe/GaAs(001) by using scanning electron microscope (SEM), atomic force microscope (AFM), x-ray diffraction (XRD) and photolumi-nescence (PL).

• Journal of the Korean Institute of Telematics and Electronics
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• v.22 no.6
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• pp.34-40
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• 1985

Characteristics of GaAE epilayers grown on (100) CaAs wa(tors by molecular beam epitaxy (MBE) under various single crystal growing conditions were investigated. In fabrica-ting GaAs, epilayer by MBE, the most important factors are a substrate temperature(ts) and a flux density ratio (As/Ga). In this experiment, the substrate temperature was varied in the range of 48$0^{\circ}C$ to $650^{\circ}C$ and As and Ga cell temperatures were varied in the range of 218$^{\circ}C$ to 256$^{\circ}C$ and 876$^{\circ}C$ to 98$0^{\circ}C$, respectively. At the substrate temperature of 54$0^{\circ}C$, As cell temperature of 23$0^{\circ}C$, and Ga cell temperature of 91$0^{\circ}C$, the As/Ga ratio was 5"10, the surface morphology was most smooth . Investigation of As-stabilized surface by RHEED and of depth profile by SIM5 showed that As is less stable than Ga. Also, X-ray diffraction measurement revealed that single crystals of (400) and (200) were formed at the both sub-strate temperatures of 52$0^{\circ}C$ and 54$0^{\circ}C$.TEX>.

• The Bulletin of The Korean Astronomical Society
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• v.36 no.1
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• pp.43.2-43.2
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• 2011

목성 극지방의 분광 관측 자료에는 $H_3+$, $H_2$, 탄화수소 분자들($CH_4,C_2H_2,C_2H_6$)이 방출선의 형태로 나타난다. 이 분자선들은 2 ~ 3 mm에서는 대부분 관측이 이루어졌지만, 7.8 mm 파장대에서는 탄화수소 분자들 중에서 $CH_4$가 hotspot 형태로 관측이 되었다. 본 연구에서는 마우나케아 천문대의 NASA IRTF (InfraRed Telescope Facility) 망원경 중에 중적외선 고분산 분광기 TEXES (Texas Echelon Cross Echelle Spectrograph)를 설치하여 $CH_4$와 함께 처음 발견된 $C_2H_2$의 특성을 분석하였다. 텍사스 주립대학에서 개발한 TEXES는 5 ~ 25 mm의 관측 파장대에서 저분산(R~3,000), 중 분산(R~15,000), 고분산(R~100,000)으로 관측할 수 있다 (Lacy et al., 2002). 본 연구에 사용된 자료는 2009년 5월 29일에 관측되었으며, 파장대는 7.8 mm 이다.

• Bulletin of the Korean Space Science Society
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• 1993.04a
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• pp.12-12
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• 1993

암혹성운 B5 영역의 중심 부분을 분자흡수선 BSCO의 6cm와 방출선인 2mmE 관측하였다. 관측은 독일의 Bonn에 있는 전파망원경과 미국의 Arizona주의 Kit Peak에 있는 전파망원정을 사용하였다. 본 관측 결과에서 얻어진 antenna temperature (Ta)의 분포를 mappin 하였다. 이 두 종류의 판측을 상호 비교한 결과 최대 황도의 위치가 서로일치하지 않음을 확인하였다. 6cm의 관측결과는 star count 방법에 의하여 결정된 extionction map에 나타나는 중심지역과 거의 일치하나, 2mm 관측은 B5 내에 있는 적외선광인 IRS 1의 위치와 일치하였다. 본 연구에서는 다른 분자선 관측 결과와 비교하므로써 H2CO의 관측 결과를 분석하였다.

• Polymer(Korea)
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• v.26 no.4
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• pp.508-515
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• 2002

The effects of the crosslinking caused by irradiation dose, molecular weights of the foaming materials, and various foaming processes on the foam structure of the polypropylene (PP) were investigated. The maximum gel content of the PP was 48% when the sheet was irradiated with 3.2 Mrad. This high gel content improved the cell structures by providing high thermal stability. The increase of both the gel content and structural development were stopped at the irradiation dose exceeding 3.2 Mrad. The increase of the molecular weights served to help produce a foam with particularly fine and even cell structures, along with improved thermal stability as well.

• Journal of Astronomy and Space Sciences
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• v.21 no.4
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• pp.243-248
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• 2004

We present measurements of interstellar CO absorption lines in the spectra of 7 early-type stars that were observed with the FUSE(Far Ultraviolet Spectroscopic Explore.) Among 54 early-type target stars in the Galactic disk and halo observed with the BBFS(Berkeley Extreme and Far-ultraviolet Spectrometer), we choose 7 program stars (HD 37903, HD 97991, HD 149881, HD 156110, HD 164794, HD 214080 and HD 219188) which have only a single velocity component in the high-resolution optical measurements, in order to avoid line blending. To analyze the CO molecule, we select the E-X (0-0) band at $1076{\AA}$, which has a large oscillate. strength and is not blended with other interstellar absorption lines. We detect the CO absorption lines in three (HD 37903, HD 164794, and HD 214080) out of seven targets, and derive CO column densities for those targets. We also estimated the CO to $H_2$ ratios toward the three stars, based on the previously estimated $H_2$ column densities.

• Bulletin of the Korean Space Science Society
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• 1995.04a
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• pp.20-20
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• 1995

• The Bulletin of The Korean Astronomical Society
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• v.30 no.2
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• pp.45.1-45.1
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• 2005

• The Bulletin of The Korean Astronomical Society
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• v.22
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• pp.20.1-20.1
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• 1997

• Proceedings of the Materials Research Society of Korea Conference
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• 1993.11a
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• pp.60-60
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• 1993