Quasars at cosmological distances can be gravitationally lensed by galaxies into two or more images. The probability of this lensing and the angular separation between the images depend on the geometry and the expansion history of the universe as well as the lensing galaxies. The time delay between lensed images is also a direct indicator of the size of the universe. I review these cosmological applications of multiple-image gravitationally lensed quasars to determine or constrain the cosmological parameters.

Since the first proposal by Paczynski, great efforts to detect Galactic dark matter by detecting light variations of stars located in the Magellanic Clouds and Galactic bulge caused by gravitational microlensing have been and are being carried out and more than 1,000 events have been successfully detected. In this paper, we review the progress in the theoretical and experimental progresses in microlensing. We begin with basics of microlensing and summarize the results obtained from the last 8 year observations along with the implications of the results. We also discuss the usefulness of microlensing in other fields of astronomy such as the stellar atmosphere, Galactic binary systems, and extra-solar planets. We finally discuss the problems of the current experiments and the new types of observations that can overcome these problems.

We have analyzed the sunspot and aurora data recorded in Go-Ryer-Sa. We have collected 35 records of sunspot observations for 46 days, and 232 records of auroral observations. To objectively estimate the periods of the solar activity appearing in these records a method of calculating the one-dimensional power spectrum from inhomogeneous data is developed, and applied to the sunspot and auroral data. We have found statistically significant 10.5 and 10 year periodicities in the distributions of sunspot and aurora records, respectively. These periods are consistent with the well-known solar activity cycle. There are indications of the long-term variations, but the period is not certain. We have also calculated the cross-correlations between the sunspot and auroral data. In particular, we have divided the aurora data into several subgroups to study their nature. We conclude that the historical records of strong auroral activity correspond to non-recurrent magnetic storms related to the sunspots. On the other hand, the records of weak auroral activity are thought to be related with the recurrent magnetic storms which occur frequently due to the coronal hole near the sunspot minimum.

리모트 수소 플라즈마를 이용하여 Si 기판 위의 구리 오염의 제거 효과에 관하여 조사하였다. 최적의 공정 조건을 찾기 위하여 Si 기판을 1ppm CuCI2 표준 화학 용액으로 인위적으로 오염시킨 후 rf power와 세정시간, 거리 (수소플라즈마 중심에서 Si 기판표면까지의 거리)등의 공정 변수를 변화시키며 리모트 수소 플라즈마 세정을 실시하였다. 리모트 수소 플라즈마 세정 후 Si 표면의 분석을 위하여 TXRF(total x-ray reflection fluorescence)와 AFM(atomic force microscope)측정을 실시하였다. 리모트 수소 플라즈마 세정이 Cu의 제거에 효과적이며 Si 표면의 거칠기에 나쁜 영향을 주지 않음을 TXRF와 AFM 분석결과로부터 알 수 있었다. Cu 불순물의 흡착 메커니즘은 산화 환원 전위 이론으로 설명될 수 있으며, Cu 불순물의 제거 메커니즘은 XPS(x-ray photoelectron spectroscopy)분석결과를 근거로 하여 다음과 같이 설명할 수 있다. :먼저 Cu 이온이 Si 표면에 흡착되어 화학적 산화막을 생성한다. 그 다음, 수소 플라즈마 중의 반응성이 강한 수소이온이 이 산화막을 분해시켜 제거하며 Cu 불순물은 산화막이 제거될 때 함께 제거된다.

리모트 수소 플라즈마를 이용하여 실리콘 웨이퍼 표면 위에 있는 금속불순물의 제거 및 제거기구에 관하여 조사하였다. 실리콘의 표면과 내부분석을 위하여 TXRF(total reflection x-ray fluorescence)와 SPV(surface photovoltage), AFM(atomic force microscope)을 사용하였다. TXRF 분석결과 리모트 수소 플라즈마가 금속오염물질 제거에 상당한 효과가 있는 것으로 나타났다. TXRF분석결과 리모트 수소 플라즈마가 금속오염물질 제거에 상당한 효과가 있는 것으로 나타났다. 리모트 수소플라트마 처리 후 금속오염은 금속원소의 종류에 따라 1010atoms/cm2-1011atoms/cm2수준이었다. SPV분석결과를 보면 수소 플라즈마 처리에 의해 minority carrier 수명이 전반적으로 증가하였다. AFM 분석을 통하여 수소 플라즈마 처리가 표면 손상을 일으키지 않으며 표면의 거칠기에 나쁜 영향을 미치지 않음을 알 수 있었다. 또한 본 실험에서 나타난 결과들을 종합해 볼 때 금속오염물의 제거기구는 자연산화막 혹은 수소로 passivate된 실리콘 웨이퍼 표면을 수소 플라즈마에서 발생된 수소원자가 실리콘표면을 약하게 에칭할 때 떨어져 나가는 'lift-off'가 유력한 것으로 판단된다.

The unique compact radio source, Sgr $A^*$, at the Galactic center show many observational signs that it is powered by supermassive black hole. Recent observations also imply that it is surrounded by winds from nearby IR sources. So we explore the model in which multiwavelength spectrum from Sgr $A^*$ is due to the spherical accretion of these winds onto the central supermassive black hole. Improving upon the previous work, we allowed the possibility that ions and electrons have different temperatures, included the Compton effects and pair processes. Electrons radiate via cyclosynchrotron and bresstrahlung with comptoniztion. We find that ion approaches the virial temperature ${\sim}10^{13}K$ while electron temperature saturates at ${\sim}10^{10}K$. However, decoupling between ion and electron does not greatly affect the shape of the emission spectrum. When the mass of the black hole is ${\sim}10^6M_{\odot}$, radio, IR, X-ray, $\gamma$-ray band spectrum is reasonably explained by the model. Yet Compton effect which is neglected in previous works produces significant emission in IR band, which is marginally compatible with observations. Pair production is negligible and annihilation lines cannot be observed.