• 방사선산업학회지
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• 제4권3호
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• pp.277-283
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• 2010

Rape (Brassica napus L.) plants are one of the major oilseed crops. The main components of rapeseed are oil (35 to 47%) and protein (15 to 32%). For the biodiesel production, the development of a new variety of rape plant with high biomass and/or oleic acid contents is required. In order to determine the optimum dose of gamma-ray irradiation, the rape seeds of cvs. Hanra (Hr), Youngsan (Ys), Tammi (Tm), and Tamra (Tr) were irradiated with a 100~4,000 Gy dose range of gamma-rays. Considering the growth factors, the optimum doses were determined to be within the range of 600~1,000 Gy for the selection of useful mutant lines. Six-hundred and eighty-eight (688) $M_2$ mutant lines were obtained from 600~1,000 Gy gamma-ray-irradiated $M_1$ plants through selfing. The growth characteristics, leaf shape, early flowering, and flower color were all investigated. The selected mutant numbers of early flowering, leaf shape, and flower color were 34, 52, and 3 from the four cultivars, respectively. These mutant lines will be used for the development of a new variety of rape plant with high biomass and oleic acid contents.

• 천문학회지
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• 제38권2호
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• pp.257-260
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• 2005

We have mapped the W 3 giant molecular cloud in the $C^o\;^3P_1-^3 P_o$ ([CI]) line with the Mount Fuji Submillimeter-wave Telescope. The [CI] emission is extended over the molecular cloud, having peaks at three star forming clouds; W 3(Main), W 3(OH), and AFGL 333. The [CI] emission is found to be strong in the AFGL 333 cloud. We have also observed the $C^{18}O,\;CCS,\;N_2H^+$, and $H^{13}CO^+$ lines by using the Nobeyama Radio Observatory 45 m telescope. In the AFGL 333 cloud, we find two massive cores, which are highly gravitationally bound and have no sign of active star formation. The high [$C^o$]/[CO] and [CCS]/[$N_2H^+$] abundance ratios suggest that the AFGL 333 cloud is younger than the W 3(Main) and W 3(OH) clouds.

• 천문학회보
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• 제40권2호
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• pp.52.3-53
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• 2015

It has been known that there is "dark gas" invisible either in 21-cm HI or 2.6-mm CO emission which are general tracers of atomic and molecular gas, respectively. Many researchers consider that the dark gas is "Dark Molecular Gas (DMG)" composed of CO-free $H_2$ in the intermediate zone between atomic and full-fledged molecular gas and that HCO+ and OH molecules are good tracers of the DMG since they can form in much lower $H_2$ column densities where CO does not. We have carried out HCO+ J=1-0 absorption observations toward nine bright extragalactic radio continuum sources using the KVN 21-m telescopes as single dishes. We detected HCO+ absorption lines toward two sources. We derive HCO+ and $H_2$ column densities or their limits, and discuss the implications of our results.

• 천문학회지
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• 제29권spc1호
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• pp.95-95
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• 1996

We present the recent results of an HI aperture synthesis mosaic of the Large Magellanic Cloud(LMC), made by combining data from 1344 separate pointing centers using the Australia Telescope Compact Array(ATCA). The resolution of the mosaiced images is 1'.0 (15 pc, using a distance to the LMC of 50 kpc). In contrast with its appearance at other wavelengths, the LMC is remarkably symmetric in HI on the largest scales, with the bulk of the HI residing in a disk of diameter 7.3 kpc. Outer spiral structure is clearly seen, though the features appear due to differential rotation, therefore transient in nature. A good correlation is seen between the supershells previously identified in Halpha (e.g. Meaburn 1980) and HI structures.

• 천문학회지
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• 제37권2호
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• pp.61-77
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• 2004

We have searched for HI 21 cm line emission from shocked atomic gas associated with southern supernova remnants (SNRs) using data from the Southern Galactic Plane Survey. Among the 97 sources studied, we have detected 10 SNRs with high-velocity HI emission confined to the SNR. The large velocity and the spatial confinement suggest that the emission is likely from the gas accelerated by the SN blast wave. We also detected 22 SNRs which show HI emission significantly brighter than the surrounding regions over a wide ($>10 km\;s^{-1}$) velocity interval. The association with these SNRs is less certain. We present the parameters and maps of the excess emission in these SNRs. We discuss in some detail the ten individual SNRs with associated high-velocity HI emission.

• 한국진공학회지
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• 제18권2호
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• pp.102-107
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• 2009

본 연구에서는 ZnO 박막을 성장하기 위한 plasma-assisted molecular beam epitaxy (PAMBE)에 장착된 플라즈마건에 13.56 MHz의 rf 전력을 인가하였을 때 발생되는 산소 플라즈마의 발광 스펙트럼을 광발광 분광기(optical emission spectroscopy: OES)를 이용하여 조사하였다. 실험은 산소 가스 유량을 1 sccm에서 20 sccm, rf 전력을 25W에서 250 W 범위에서 플라즈마건의 오리피스의 직경을 각각 3 mm 와 5 mm로 달리하여 행해졌다. 산소 플라즈마를 발생시켰을 때 오리피스의 직경에 상관없이 전형적인 산소 플라즈마의 발광 스펙트럼이 관측되었다. 특히 776.8 nm와 843.9 nm에서 $3p^{5}P-3s^{5}S^{0}$, $3p^{3}P-3s^{3}S^{0}$ 천이에 기인하는 강한 산소 원자 발광선이 관측되었다. 산소 유량과 rf 파워가 증가함에 따라 776.8 nm와 843.9 nm의 발광 세기는 증가하였고, 776.8 nm의 스펙트럼 발광 세기의 증가율이 843.9 nm의 스펙트럼 발광 세기 증가율보다 컸다. 또한 오리피스 직경이 3 mm일 때가 5 mm일 때보다 산소 플라즈마가 더 안정적으로 발생하였다.