We developed an efficient Monte-Carlo algorithm to solve dust-scattering radiative transfer problems for continuum radiation. The method calculates the scattered intensities for various anisotropic factors ( gi) all at once, while actual photon packets are tracked following a scattering phase function given by a single anisotropic factor ( g0). The algorithm was tested by applying the method to a dust cloud embedding a star at the cloud center and found to provide accurate results within the statistical fluctuation that is intrinsic in Monte-Carlo simulations. It was found that adopting g0 = 0.4 - 0.5 in the algorithm is most efficient. The method would be efficient in estimating the anisotropic factor of the interstellar dust by comparing the observed data with radiative transfer models.

Astrochemistry provides powerful tools to understand various cosmic phenomena, including those in our solar system to the large-scale structure of the universe. In addition, the chemical property of an astronomical body is a crucial factor which governs the evolution of the system. Recent progress in astrophysical theories, computational modelings, and observational techniques requires a detailed understanding of the interactions between the constituents of an astronomical system, which are atoms and molecules within the system. Especially the far-infrared/sub-millimeter wave range, which is called as the last frontier in astronomical observations, contains numerous molecular lines, which may provide a huge amount of new information. However, we need an astrochemical understanding to use this information fully. Although this review is very limited, I would like to stress the importance of astrochemical approach in this overview for the field, which is getting much more attention than ever before.

We present analytical approximations for calculating the scattering and escape of non-ionizing photons from a plane-parallel medium with uniformly illuminated by external sources. We compare the results with the case of a spherical dust cloud. It is found that more scattering and absorption occur in the plane-parallel geometry than in the spherical geometry when the optical depth perpendicular to the plane and the radial optical depth of the sphere are the same. The results can provide an approximate way to estimate radiative transfer in a variety interstellar conditions and can be applied to the dust-scattered diffuse Galactic light.

We present measurements of interstellar H2 absorption lines in the continuum spectra of 54 early-type stars in the Galactic disk and halo and 3 stars in the Magellanic Clouds. The data were obtained with the Berkeley Extreme and Far-Ultraviolet Spectrometer (BEFS), part of the ORFEUS telescope, which flew on the ORFEUS-SPAS I and II space-shuttle missions in 1993 and 1996, respectively. The spectra extend from the interstellar cutoff at 912＼AA to about 1200＼AA with a spectral resolution of ∼3000 and statistical signal-to-noise ratios between 10 and 65. Assuming a velocity profile derived from optical observations (when available), we model the column densities N(J) of the rotational levels J = 0 through 5 for each line of sight. Our data reproduce the relationships among molecular and total hydrogen column density, fractional molecular abundance, and reddening first seen in Copernicusobservations of nearby stars (Savage et al. 1977). The results show that most of these molecular clouds have H2 total column densities between 1015cm−2 and 1021cm−2, and kinetic temperatures from 21 K to 232 K, with average of 89 K, consistent with the result of Copernicus (Savage et al. 1977).

We present the results of one-dimensional numerical simulations of SNR evolution in the in­homogeneous medium considering the effects of the evaporation of the cloud and the thermal conduction. We have included the effects of changing evaporation rate as a function of cloud size and the ambient temperature so that the clouds could be evaporated completely before they reach the center of the SNR. The heat conduction markedly changes the density distribution in the remnant interior. To explain the observed morphologies of the centrally peaked X-ray SNRs(for example W44), the maximal thermal conduction is required. However, this is unlikely due to the magnetic field and the turbulent motion. The effects of the evaporation of the cloud and the thermal conduction described here may explain the class of remnants observed to have centrally peaked X-ray emmision.

We observed the molecular transitions of 12CO(1−0) 12CO(1−0) , 13CO(1−0) 13CO(1−0) , C18O(1−0) C18O(1−0) , CS(2-1), HCO+(1−0) HCO+(1−0) , and HCN(1-0) toward the high-latitude mole cular cloud MBM12. We derived total H2 H2 column densities for the two velocity components using the optically thin C18O C18O transition. Molecular abundances have been derived for the observed species at the core of this cloud, which appear to be less than an order of magnitude in fractional abundances relative to H2 H2 , compared to typical cold dark clouds.

목적: 본 연구의 목적은 대학 운동선수들의 지각된 코칭행동과 노력/지속성 간의 관계에서 정서와 정서지능의 매개효과를 검증하고, 운동경력 수준 간 구조모형의 교차 타당성을 검증하는데 두었다. 방법: 연구대상은 대학 운동 선수 368명(남자=307명, 여자=61명)이며, 자료는 기술통계, 확인적 요인분석, 상관분석, 구조방정식모형 분석 및 다집단 분석을 통해 분석되었다. 결과: 첫째, 대학 운동선수들의 지각된 자율성지지 코칭행동은 긍정적 정서와 정서지능을 통해서 뿐만 아니라 직접적으로 노력과 지속성을 증진시키는데 기여하였다. 둘째, 통제적 코칭행동은 선수들의 노력/지속성에 직접 영향을 주지만, 부정적 정서와 정서지능을 통해 노력/지속성에 영향을 미치지 않았다. 셋째, 선수들의 노력과 지속성에 대한 지각된 코칭행동과 정서 및 정서지능의 영향력은 선수들의 운동경력 수준에 따라 차이가 있다. 결론: 이 결과는 코치의 행동이 선수들의 수행을 위한 노력과 지속성에 영향을 주지만, 코치가 선수들의 자율성을 지지할수록 선수들은 긍정적인 정서가 촉진되어 자신과 타자의 정서를 적절히 평가하고 조절함으로써 스포츠 수행을 위해 지속적인 노력을 기울인다는 사실을 시사한다.