N2처리에 의해 Si (001) 기판에 형성된 C49상의 구조를 갖는 에피택셜 TiSi2상의 열적 거동과 결정학적 특성을 X선 회절법 (XRD)과 고분해능 투과전자현미경법 (HRTEM)으로 조사하였다. 에피택결 C49-TiSi2상은 1000˚C 정도의 고온에서도 안정상인 C54상으로 상변태하지 않고 형태적으로도 고온 특성이 우수하다는 것이 밝혀졌다. HRTEM 결과로부터 에피택결 TiSi2상과 Si 사이의 결정학적 방위관계는 (060) [001]TiSi2//(002) [110]Si임을 알 수 있었고 계면에서의 격자 변형에너지는 misfit 전위의 형성에 의하여 해소되는 것을 확인할 수 있었다. 또한 HRTEM상의 해석과 원자 모델링을 통하여 Si에서 에피택셜 C49-TiSi2상의 형성기구와 C49상의 (020) 면에 존재하는 적층결함을 고찰하였다.

Many publications of pointology have been conflicted to define fixed positions of acu-points. These underlying cause results from the historical fact that most of acu-points and meridian systems began at anonymous experiences of many generations. However, if we would believe that the acupoints and meridian systems exit clearly in all of the organism, there were exit the fixed position of acupoints. In this study, we performed bibliographically the investigation fixing the position of CV16. From the investigation, although supported that it exit 1.6 chon (寸) below CV17 in human being, we suggest that CV16 exit below the sternum met with the 7th rib, or the joined point between the sternum and the xiphoid process.

We have reviewed the magnetic activity in close binaries. Solar like magnetic activity indicators such as photometric spots, chromo spheric emission, coronal X-ray and radio emission, and flare activity are commonplace in many cool stars with convective envelopes. Using the UV spectra we confirmed the strength of stellar activity increases with more rapid rotation and later spectral types which corresponds to the increasing depth of the star's convective envelope. Apart from very young stellar objects such as T Tauri stars, the stars with the highest levels of activity are close binary systems composed of cool stars, i.e., the chromospherically active binaries such as RS CVn, BY Dra, W UMa and related systems. The IUE low and high dispersion spectra of V711 Tau, VW Cep and SW Lac are used for ultraviolet photometry and for a variation study of chromospheric activity. Evidence of chromospherically activity is indicated by the intensity variation of the Mg II emission line with orbital phase.