Polycyclic aromatic hydrocarbons (PAHs) in Galactic planetary nebulae (PNe) are investigated by means of the unidentified infrared (UIR) bands. Continuous near- to mid-infrared spectra of PNe are obtained with the AKARI/IRC and the Spitzer/IRS. All 19 PNe in the present study show prominent dust emissions and we investigate the variation in the intensity ratios among the UIR bands. The ionization fraction and the size distribution of PAHs in PNe are derived using the UIR band ratios. We find that the ionization fraction of PAHs in PNe is around 0.0-0.6 and that small PAHs are scarce. The present result indicates a systematic trend of the 3.4 μm aliphatic feature to become weak as the PAH ionization fraction increases.

구조 역섭동 문제에서, 신뢰할 만한 결과를 얻기 위해서는 정의되지 않은 모든 자유도가 미지변수로 간주되기 때문에 많은 전산자원이 필요하다. 본 연구에서는 축소시스템 기법과의 연동을 통해 정의되지 않은 자유도를 축소시스템에서 정의된 자유도 정보로 대체함으로써 해의 정확성과 계산의 효율성을 확보하는 기법을 제안한다. 일반적으로 구조 시스템을 축소할 경우, 시스템 축소변환 행렬에 오차가 포함되게 된다. 이 오차로 인해 축소기법을 적용하여 역섭동 문제의 정확한 해를 구하는 것은 쉽지 않은 문제이다. 이러한 문제를 해결하기 위해서 자유도 변환행렬을 매 단계마다 개선하는 반복적 축소 시스템 기법을 적용한다. 자유도 기반 축소시스템의 신뢰성은 주자유도 선정 위치와 변환행렬의 반복 계산 횟수에 의해 결정되며, 변환행렬의 반복 계산을 줄이기 위해서는 시스템 구축 초기에 주자유도가 잘 선정되어야 한다. 따라서, 본 연구에서는 축소모델의 정확도를 향상시키고 변환 행렬의 반복 계산을 최소화하기 위해 2단계 축소기법을 적용하여 주자유도 위치를 선정한다. 최종적으로 수치예제를 통해서 반복적 역섭동법의 효용성을 확인한다.

We present images of L1551 IRS5 at angular resolutions as high as ~30 mas, corresponding to a spatial resolution of ~5 AU, made at 7 mm with the VLA. Previously known to be a binary protostellar system, we show that L1551 IRS5 is likely a triple protostellar system. The primary and secondary components have a projected separation of ~46 AU, whereas the tertiary component has a projected separation of ~11 AU from the primary component. The circumstellar dust disks of the primary and secondary components have dimensions of ~15 AU, whereas that of the tertiary component has a dimension of ~10 AU. Their major axes are closely, but not perfectly, aligned with each other, as well as the major axis of the surrounding flattened, rotating, and contracting molecular condensation (pseudodisk). Furthermore, the orbital motion of the primary and secondary components is in the same direction as the rotational motion of this pseudodisk. We suggest that all three protostellar components formed as a result of the fragmentation of the central region of the molecular pseudo disk. The primary and secondary components, but apparently not the tertiary component, each exhibits a bipolar ionized jet that is centered on and which emergers perpendicular to its associated dust disk. Neither jets are resolved along their base, implying that they are driven within a radial distance of ~2.5 AU from their central protostars. Finally, we show evidence for what may be dusty matter streams feeding the two main protostellar components.

An x-ray astronomy experiment consisting of three collimated proportional counters and an X-ray Sky Monitor (XSM) was flown aboard the Indian Satellite IRS-P3 launched on March 21, 1996 from SHAR range in India. The Satellite is in a circular orbit of 830 km altitude with an orbital inclination of 98° and has three axis stabilized pointing capability. Each pointed-mode Proportional Counter (PPC) is a multilayer, multianode unit filled with P-10 gas (90% Ar + 10% CH4) at 800 torr and having an aluminized mylar window of 25 micron thickness. The three PPCs are identical and have a field of view of 2°×2° defined by silver coated aluminium honeycomb collimators. The total effective area of the three PPCs is about 1200 cm2. The PPCs are sensitive in 2-20 keV band. The XSM consists of a pin-hole of 1 cm2 area placed 16 cm above the anode plane of a 32 cm×32 cm position sensitive proportional counter sensitive in 3-8 keV interval. The position of the x-ray events is determined by charge division technique using nichrome wires as anodes. The principal objective of this experiment is to carry out timing studies of x-ray pulsars, x-ray binaries and other rapidly varying x-ray sources. The XSM will be used to detect transient x-ray sources and monitor intensity of bright x-ray binaries. Observations of black-hole binary Cyg X-1 and few other binary sources were carried out in early May and July-August 1996 period. Details of the x-ray detector characteristics are presented and preliminary results from the observations are discussed.