다변량통계기법은 수리지구화학 자료의 분석 및 해석에 많이 이용되어 왔다. 본 연구에서 대응분석과 주성분분석을 동시에 사용하여 인위적인 활동에 의한 지하수의 특징을 살펴보았다. 본 연구의 목적은 NETPATH 프로그램 속의 WATEQ4F를 이용하여 지하수 화학성분의 분화를 계산하고 이를 다변량통계기법을 이용하여 지구화학적인 정보를 추출하는 것이다. 연구지역은 한반도의 남동쪽에 위치한 울산의 LPG 저장시설이다. 본 연구지역에서는 다른 저장시설에서 관찰되는 초염기성의 조성을 가지는 지하수가 관찰되었다. 이러한 인위적인 영향에 의한 높은 pH를 가지는 지하수로 인해 Al의 분화특징과 탄산염의 침전을 유발할 수 있다. 본 연구에서는 연구지역에 지하수에 영향을 주는 두 인위적인 요소(세정작용와 시멘트영향)에 의해서 수리지구화학적인 특징과 상이 어떻게 변하는 가에 초점을 두었다. 이전 연구결과와 두 통계분석을 통해 제시된 결과를 비교하여 지구화학적인 정보를 이용한 주성분분석과 대응분석인 수리지구화학 연구에서 기초연구로 활용될 수 있음을 알 수 있다.

A new type of object called "Very Low Luminosity Objects (VeLLOs)" has been discovered by the Spitzer Space Telescope. VeLLOs might be substellar objects forming by accretion. However, some VeLLOs are associated with strong outflows, indicating the previous existence of massive accretion. The thermal history, which significantly affects the chemistry, between substellar objects with a continuous low accretion rate and objects in a quiescent phase after massive accretion (outburst) must be greatly different. In this study, the chemical evolution has been calculated in an episodic accretion model to show that CO and N2H+ have a relation different from starless cores or Class 0/I objects. Furthermore, the CO2 ice feature at 15.2μm will be a good tracer of the thermal process in VeLLOs.

The previous study of chemical evolution of the Galaxy is extended to the radial properties of the Galactic disk. The present model includes radial dependency of the time-dependent bimodal IMF, radial flow of material in the disk, and the change of type I supernova explosion rate with radial distance from the disk center as model parameters and observed gas and stellar density distributions and metallicity abundance gradient as observational constraints. The results of two models in this study explain the observed gas and stellar density distributions well, with the slope of the gas density gradient in the region of 4.5 kpc<r<12kpc as -0.136dex/kpc in model Y1 and -0.123dex/kpc in model Y2, respectively, which fit well the observed gradient of -0.l1dex/kpc. The abundance gradient reproduced in model Y1 is getting flatter with decreasing radius, while that in model Y2 is getting steeper, which fits better the observed abundance gradient. This result shows the necessity of exponentially increasing type I supernova explosion rate with decreasing radius in order to explain the observed abundance gradient in the disk. The fitness of observed density distribution and star formation rate distribution justifies the reliability of time-dependent bimodal IMF as a compound quantitative chemical evolution model of the Galaxy. The temporal variations of metallicity gradients for carbon, nitrogen and oxygen are also shown.

From the uvby, H β photometry of intermediate population II F-stars in the catalogue of Olsen (1983), we derived age-metallicity relations for these stars, using Hejlesen's (1980) isochrone. The derived age-metallicity relations well coincide with the theoretical predictions by the unclosed two-zone model of Lee and Ann (1981). There are few extremely metal poor F-stars in the vicinity of the Sun, and it is very likely that the initial rapid metal enrichment in the galactic disk might have been processed through the fast collapse of the disk at the very early epoch.

On the basis of observational constraints, particularly the relationship between metal abundance and cumulative stellar mass, a simple two-zone disk-halo model for the chemical evolution of our Galaxy was investigated, assuming different chemical processes in the disk and halo and the infall rates of the halo gas defined by the halo evolution. The main results of the present model calculations are: (i) The halo formation requires more than 80% of the initial galactic mass and it takes a period of 2 ∼ 3 × 10 9 yrs. (ii) The halo evolution is divided into two phases, a fast collapse phase ( t = 2 ∼ 3 × 10 8 yrs) during which period most of the halo stars ( ∼ 95 are formed and a later slow collapse phase which is characterized by the chemical enrichment due to the inflow of external matter to the halo. (iii) The disk evolution is also divided into two phases, an active disk formation phase with a time-dependent initial mass function (IMF) up to t ≈ 6 × 10 9 yrs and a later steady slow formation phase with a constant IMF. It is found that at the very early time t ≈ 5 × 10 8 yrs, the metal abundance in the disk is rapidly increased to ∼ 1 / 3 of the present value but the total stellar mass only to ∼ 10 of the present value, finally reaching about 80% of the present values toward the end of the active formation phase.

The abundances of simple molecules are examined in terms of the time-dependent cloud evolution. The formation and destruction mechanisms of H 2 C O are reviewed. The average value of the fractional abundance of H 2 C O is derived to be in the range of 10 − 10 t o 5 × 10 − 9 . This is comparable to the observed values. The expected variations of the molecules formed from or destroyed by CO, CI, and C + whose abundances depend on the evolutionary state of the cloud are discussed.