We are often faced with the task of having to estimate the hydrogen and helium ionizing luminosities of massive stars in the study of H II regions and the warm ionized medium (WIM). Using the results of the most complete compilation of stellar parameters (the effective temperature, stellar radius and surface gravity) and the latest Kurucz stellar atmosphere models, we calculate the ionizing photon luminosities in the H0andHe0 continua from O3 to B5 stars. We compared the theoretical Lyman-continuum luminosity with the observationally inferred luminosity of the H II region around α Vir, and found that the theoretical value is higher than the observed value in contrast to the eariler result.

We present the results of a 21cm radio continuum aperture synthesis mosaic of the Large Magellanic Cloud (LMC), made by combining data from 1344 separate pointing centers using the Australia Telescope Compact Array (ATCA) and the 64-m Parkes single-dish telescope. The resolution of the mosaicked images is 55' ( 10 pc, using a distance to the LMC) and a region 10° X 12° is surveyed.

In the past, it. was very difficult to distinguish thermal and non-thermal emission. Broadbent et a1. (1989) has developed a new technique with the help of the IRAS 60 micron emission. The distribution of non-thermal or synchrotron emission in the Galactic disk has been modeled from the 408 MHz all sky survey of Haslam et a1. (1982) after removal of the thermal component.. At. 408 MHz, t.here is very little absorption in the interstellar medium and the distribution along the line-of-sight. is inferred mainly from its presumed relationship to other tracers of spiral structure via a. number of fitted parameters. But. at lower frequencies, free-free absorption becomes important and can give some direct. information on the line of sight. distribution. We have modeled the thermal electron density according to the spiral arm models and the distribution of ionized hydrogen in the Galactic plane by Lockman (1976) and Cersosimo et. al. (1989) and have made predictions to compare with the surveys of Dwarakanath et al. (1990) at. 34.5 MHz and .Jones and Finlay (1974) at 29.9 MHz. The result confirms that the absorption model of the synchrotron emissivity in the Galactic plane is broadly corrected and illustrates the potential of the absorption technique.

We have developed a 5GHz continuum receiver system. The receiver is a direct type receiver. In order to reduce the noise due to the fluctuation of the gain in the amplifiers, the system employs the Dicke switching method. We made the 5GHz low-noise amplifier and the bandpass filter. The low-noise amplifier gives ∼35dB ∼35dB gain and has ∼210K ∼210K noise temperature. The bandpass filter has a passband between 4.3 and 5.4GHz. We also made switch driver, video amplifiers, phase detector, and integrator. Using a 1.8 meter offset parabolic antenna, we measured the efficiency of the system. Since the antenna does not have a driver to track objects, observations were performed with the antenna fixed. The measured noise temperature of the system is ∼650K ∼650K . From the observation of the blank sky, noise level was measured. It was found that the systematic noise(∼0.5K ∼0.5K : peak to peak value) is much larger than the thermal noise. The systematic noise is possibly related to the stability of the DC power supplied to the receiver system. Besides the noise of the system, it was found that the airplanes are the very serious noise sources. We measured the radio flux of the Sun using the developed system. The observed radio flux of the Sun is ∼106Jy ∼106Jy , which is close to the known value of the quiet Sun. The test observation of the Sun shows that the angular beam size of the antenna is ∼2.2∘ ∼2.2∘ .

We have decomposed the 11-cm radio continuum emission of the W51 complex into thermal and non-thermal components. The distribution of the thermal emission has been determined by analyzing HI, CO, and IRAS 60-μm data. We have found a good correlation between the 11-cm thermal continuum and the 60- 11m emissions, which is used to obtain the thermal and non-thermal 11-cm continuum maps of the W51 complex. Most of the thermal continuum is emanating from the compact H II regions and their low-density ionized envelopes in W51A and W51B. All the H II regions, except G49.1-0.4 in W51B, have associated molecular clumps. The thermal radio continuum fluxes of the compact H II regions are proportional to the CO fluxes of molecular clumps. This is consistent with the previous results that the total mass of stars in an H II region is proportional to the mass of the associated molecular clump. According to our result, there are three non-thermal continuum sources in W51: G49.4-0.4 in W51A, a weak source close to G49.2-0.3 in W51B, and the shell source W51C. The non-thermal flux of G49.5-0.4 at 11-cm is ~28 Jy, which is ~25% of its total 11-cm flux. The radio continuum spectrum between 0.15 and 300 GHz also suggests an excess emission over thermal free-free emission. We show that the excess emission can be described as a non-thermal emission with a spectral index α≃-1.0 (Sv∝Va) attenuated by thermal free-free absorptions at low-frequencies. The non-thermal source close to G49.2-0.3 is weak (~9 Jy). The nature of the source is not known and the reality of the non-thermal emission needs to be confirmed. The non~thermal shell source W51C has a 11-cm flux of ~130Jy and a spectral index α≃-0.26.

The environmental structure of T Tauri star can be understood by its continuum energy distribution. We suggest four evolutionary stages on the base of this environmental change from molecular cloud to the main sequence. A protostar is embedded in a dense envelope which can be attributed to the overall infrared region in continuum spectra. The infalling material from the envelope results in producing a hump in the mid-infrared region. This matter produces a surrounding disk around a central star afterwards. The disk emission changes the spectral index in the overall infrared region. The disk will be developed to a ring structure owing to the formation of planets by its instability and/or the cleaning effect of the inner region of the disk by a central star outflow, contributing to producing a hump in the far-infrared region. The pre-main sequence evolution points of T Tauri stars in H-R diagram strongly support the environmental structure evolution.

거대한 평판형 격자구조물올 연속체 평판으로 모델링하기 위한 보다 용이한 기법올 에너지동둥 개 념에 근기 하여 제시하였다. 단위 격 자가 갖 는 탄성변형에너지와 운동에너지를 구 할때 기폰의 유한요소 행렬을 이용하였다. 연속체 평 판의 퉁 가불성치 는 연속체평판과 격자평판에 해당하는 축소된 강성 및 질 량행 렬들 올 직 접 비 교 하여 구하였다- 본 연구에서 제안된 모 델링기법이 기존의 잘 알려진 기볍들에 옷지 않는 좋 은 결 과를 보여주고 있음을 예제해석을 통해 확인하였다.