We present the results of a 21cm radio continuum 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) and the 64-m Parkes single-dish telescope. The resolution of the mosaicked images is 55' ( 10 pc, using a distance to the LMC) and a region 10° X 12° is surveyed.

We have conducted observations toward the molecular cloud associated with the H II region Sh 156 in 13CO(J = 1-0), C18O(J = 1-0), and CS(J = 2 -1) using the TRAO 14 m telescope. Combining with existing 12CO(J = 1- 0) data of the Outer Galaxy Survey, we delineated the physical properties of the cloud. We found that there is a significant sign of interaction between the H II region and the molecular gas. We estimated the masses of the molecular cloud, using three different techniques; the most plausible mass is estimated to be 1.37 X 105M⊙, using a conversion factor of X = 1.9 X 1020cm-2 (K km s-1)-1, and this is similar to virial mass estimate. This implies that the cloud is gravitationally bound and in virial equilibrium even though it is closely associated with the H II region. In addition to existing outflow, we found several MSX and IRAS point sources associated with dense core regions. Thus, more star forming activities other than the existing H II region are also going on in this region.

The Tycho supernova remnant (SNR), as one of the few historical SNRs, has been widely studied in various wavebands and previous observations have shown evidence that Tycho is interacting with a dense ambient medium toward the northeast direction, In this paper, we report our high-resolution (16") 12CO observation of the remnant using the Nobeyama 45m radio telescope. The Nobeyama data shows that a large molecular cloud surrounds the SNR along the northeastern boundary. We suggest that the Tycho SNR and the molecular cloud are both located in the Perseus arm and that the dense medium interacting with the SNR is possibly the molecular cloud. We also discuss the possible connection between the molecular cloud and the Balmer-dominated optical filaments, and suggest that the preshock gas may be accelerated within the cosmic ray and/or fast neutral precursor.

We present the results of an H I 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) and the Parkes multibeam receiver. The resolution of the mosaiced images is 50" (<15 pc, using a distance to the LMC of 55kpc). This mosaic, with a spatial resolution .15 times higher than that which had been previously obtained, emphasises the turbulent and fractal structure of the ISM on the small scale, resulting from the dynamical feedback of the star formation processes with the ISM. We also have done a widefield panoramic survey of Hα emission from the Magellanic Clouds with an imager mounted on the 16-inch telescope at Siding Spring Observatory. This survey produced Hα images which are equal to the ATCA survey in area coverage and resolution. This survey allows us to produce a continuum-subtracted image of the entire LMC. In contrast with its appearance in the Hα image, the LMC is remarkably symmetric in H I on the largest scales, with the bulk of the H I residing in a disk of diameter 8. ̊4 (7.3 kpc) and a spiral structure is clearly seen. The structure of the neutral atomic ISM in the LMC is dominated by H I filaments combined with numerous shells and holes.

구름이 유입하는 경우 해양대기경계층의 발달을 분석하기 위하여, 울릉도에서 관측한 레윈존데 자료와 AWS 자료, 위성사진, 동해에 설치된 부이 자료를 이용하였다. 이 자료를 이용하여 열의 이류와 표층 열속, 구름 유입에 따른 복사에너지를 추정하였다. 혼합층 내의 열 변화 및 혼합층의 발달을 표층 열속과 구름에 의한 장파복사속으로 설명하였다. 열속의 변화를 알아보기 위해 벌크법을 이용하였다. 울릉도, 동해상의 부이, 포항에서 관측한 자료를 이용한 열수지 방정식으로 대기경계층의 열보존 관계를 분석하였다. 구름의 유입으로 인해 일몰 후 지면의 복사냉각이 방해되고, 구름에서 장파복사가 방출된다. 그로 인해 야간에 오히려 기온이 증가하였다. 또 남서쪽으로부터 따뜻한 공기가 이류되어, 하층 대기의 온도를 증가시켰다. 이러한 이유로 혼합층이 파괴되지 않고, 잔류층을 형성하며 남아있었다.

구름이 평지위의 난류속의 변화에 미치는 영향을 연구하기 위하여 스페인 빌라프리아 공항에 설치된 9 m 기상관측탑에서 얻은 역학 및 열역학 자료를 경도법으로 분석하였다. 일몰에 따른 표면 냉각은 표층 풍속을 감소시켰다. 현열속과 운동량속은 열역학적 인자 보다는 역학적 인자에 따라 증가하였고, 현열속은 열적인 조건에 영향을 받지 않았다. 구름이 존재하는 경우 전천일사량이 현열속 변화를 주도하지 못했고 대기 표층은 오히려 바람의 강도에 영향을 받았다.

해수면 온도에 대한 구름복사 강제력의 지역 의존도가 조사되었다. 이 조사는 경년 변동과 계절 시간규모에 대해서 각각 조사되었다. 적도 동태평양에서 경년 변동의 경우 해수면 온도가 1˚C 증가할 때 순 구름복사 강제력은 약 3Wm-2가 증가하였으며, 계절변동이 포함된 경우 약 3.5Wm-2가 증가하는 것으로 나타났다. 반면 열대 해양전체에서 경년 변동의 경우 해수면 온도가 1˚C 증가할 때 순 구름복사 강제력은 1.5Wm-2 감소하였으나, 계절변동이 포함된 경우 약 2.9Wm-2로 증가하였다. 따라서 해수면 온도에 대한 구름복사 강제력의 의존도는 적도 동태평양에서 열대 해양으로 넓어질수록 경년 변동에 의해 영향에서 계절변동에 의한 영향이 더 지배적으로 작용한다. 계절 변동이 포함된 경우 해역에 관계없이 해수면온도가 1˚C 증가할 때, 순 구름복사 강제력은 약 2∼3Wm-2 증가하였다. 이러한 결과는 해수면 온도의 경년 변동이 뚜렷한 적도 동태평양에서는 경년 변동에 의한 구름복사 강제력이 대기를 가열하는 반면, 열대 해양 전체에서는 계절변동에 의한 구름복사 강제력이 대기를 가열한다는 것을 의미한다.

For the unconfined vapor cloud explosion accident by the continuous release of gas-liquid flow of various saturated liquids in a vessel at ground level, overpressures were estimated and analyzed with various release conditions and materials by TNT equivalency model with vapor dispersion. We found that at same release conditions, overpressure showed n-heptane > xylene > n-hexane > toluene > n-heptane > benzene, respectively and that overpressure was increased with increasing the hole diameter and the storage pressure, but it was increased with decreasing the wind speed, the interested distance, and the vessel thickness.

We have mapped 1 deg2 region toward a high latitude cloud MBM 40 in the J = 1 - 0 transition of 12CO and 13CO, using the 3 mm SIS receiver on the 14 m telescope at Taeduk Radio Astronomy Observatory. We used a high resolution autocorrelator to resolve extremely narrow CO linewidths of the molecular gas. Though the linewidth of the molecular gas is very narrow (FWHP < 1 km s-1), it is found that there is an evident velocity difference between the middle upper part and the lower part of the cloud. Their spectra for both of 12CO and 13CO show blue wings, and the position-velocity map shows clear velocity difference of 0.4 km s-1 between two parts. The mean velocity of the cloud is 3.1 km s-1. It is also found that the linewidths at the blueshifted region are broader than those of the rest of the cloud. We confirmed that the visual extinction is less than 3 magnitude, and the molecular gas is translucent. We discussed three mass estimates, and took a mass of 17 solar masses from CO integrated intensity using a conversion factor 2.3 × 10 20 cm -2 (K km s-1)-1. Spatial coincidence and close morphological similarity is found between the CO emission and dust far-infrared (FIR) emission. The ratio between the 100 f.Lm intensity and CO integrated intensity of MBM 40 is 0.7 (MJy/sr)/(K km s-1), which is larger than those of dark clouds, but much smaller than those of GMCs. The low ratio found for MBM 40 probably results from the absence of internal heating sources, or significant nearby external heating sources.

We observed the thermal transitions of SiO (J=I-0, 2-1) and 29SiO (J=l-O) toward the Sgr A molecular clouds. The distribution and the velocity structure of SiO are very similar to previous results for 'quiet' interstellar molecules. We think· that the SiO has been well mixed with other molecules such as H2 which may indicate that the formation of Sgr A molecular clouds was affected by the activities, such as shock waves or energetic photons, from the Galactic center in large scales. The total column density of SiO is about 4.1×1014cm−2 and the fractional abundance SiO/H2 appears to be about 10 times larger than those of other clouds in the central region of our galaxy. The derived values are thought to be lower limits since the optical depths of the observed SiO lines are not very thin. The formation of SiO has been known to be critically related to shocks, and our results provide informative data on the environment of our Galactic center.