본 연구는 창주둥이바구미과 갑충의 구기가 부드러운 식물조직을 섭식하는 바구미과 갑충과 거의 같은 구조를 하고 있다는 사실을 잘 나타내고 있다. 창주둥이바구미과 갑충에 대하여 주사전자현미경을 사용하여 구기를 본래의 위치에서 관찰하고, 여기에 해부에 의한 연구도 병행하여 얻은 구기구조에 대한 연구의 결과는 다음과 같다. 창주둥이바구미아과의 바구미는 두순 가장자리가 꾸불꾸불한 모양이고, 큰턱은 수축시 전후로 만나며 안쪽으로 약간 굽어있는 구조를 하고 있다.

바구미류의 섭식행동과 산란공을 파는 운동과 구기의 복합적인 구조를 알기 위해서는 원래의 위치에서의 복잡한 구기구조의 관찰이 행하여져야만 한다. 이러한 목적을 위하여 Brentidae의 바구미류에 대하여 주사전자현미경을 사용하여 구기를 본래의 위치에서 관찰하고, 여기에 해부에 의한 연구도 병행하여 얻은 구기구조에 대한 연구의 결과는 다음과 같다. 이과에 속하는 바구미는 아랫입술 수염이 퇴화되어 하순전기절의 꼭대기의 구멍에 위치하고 있다. 대악후관절구는 깊

In this study we present the study of solar active regions based on BOAO vector magnetograms and Hα filtergrams. With the new calibration method we analyzed BOAO vector magnetograms taken from the SOFT observational system to compare with those of other observing systems. In this study it has been demonstrated that (1) our longitudinal magnetogram matches very well the corresponding Mitaka's magnetogram to the extent that the maximum correlation yields r=0.962 between our re-scaled longitudinal magnetogram and the Mitaka's magnetogram; (2) according to a comparison of our magnetograms of AR 8422 with those taken at Mitaka solar observatory their longitudinal fields are very similar to each other while transverse fields are a little different possibly due to large noise level; (3) main features seen by our longitudinal magnetograms of AR 8422 and AR 8419 and the corresponding Kitt Peak magnetograms are very similar to each other; (4) time series of our vector magnetograms and H-alpha observations of AR 8419 during its flaring (M3.1/1B) activity show that the filament eruption followed the sheared inversion line of the quadrupolar configuration of sunspots, indicating that the flare should be associated with the quadrupolar field configuration and its interaction with new filament eruption. Finally, it may be concluded that the Solar Flare Telescope at BOAO works normally and it is ready to do numerous observational and theoretical works associated with solar activities such as flares.

We present BVRI CCD photometry and near-infrared K photometry of the intermediate-aged open cluster NGC 7790. The reddening, E(B - V) = 0.54 ± 0.05 and the distance modulus, (m - M)o = 12.45 ± 0.10 for the cluster were determined by zero-age-main-sequence fitting and theoretical isochrone fitting using not only (V, B - V), (V, V - 1), (V, V - R) but also (V, V - K) color-magnitude diagrams. The reddening corresponded approximately to the average value derived from previous studies, while the distance modulus was found to be almost midway between the CCD photometric results of Romeo et al. (1989) and those of Mateo & Madore (1988). We have used four colors to distinguish members from field stars. The expected colors were calculated using the derived distance modulus, and were then were compared with the observed colors (B - V), (V - 1), (V - R), and (V - K). Thus, a color excess E(B - V) for each star was determined which could give the minimum difference between the calculated and observed colors. Single and binary members of the cluster were determined on the basis of the E(B - V) distribution of stars.

The formation, microstructure and properties of novel ceramic composite materials manufactured by active-filler-controlled polymer pyrolysis were investigated. In the presence of active filler particles such as transition metals, bulk components of various geometry could be fabricated from siliconorganic polymer. Molybdenum- and tungsten-filled polymer suspensions were prepared and their conversion to ceramic composites by annealing in atmosphere were studied. Dimensional change. porosity and phase distribution (filler network) were analyzed and correlated to the resulting hardness values. Molybdenum and tungsten as active filler were carburized completely to , and WC in atmosphere. Consequently, microcrystalline composites with the filler reaction products embedded in a silicon oxycarbide glass matrix were formed. Hardness was increased with increasing carburization and reached 8.6-9.5 GPa in the specimen pyrolyzed in atmosphere.