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1968년 ~ 2024년까지 1,211 건의 한국천문학회지를 격월간 확인하실 수 있습니다.
- The Korean Astronomical Society (The Korean Astronomical Society)
- 계간 (Quarterly)
- ISSN : 1225-4614 (ISSN : 1225-4614)
1225-4614
- DB구축현황 : 1,211건 (DB Construction : 1,211 Articles)
총 게시글 1,211건
페이지 47/122
461
- MATSUMOTO TOSHIO
- Journal of the Korean astronomical society = 천문학회지
- 38, n.2
- pp.93-95
- 2005
- 원문 바로보기
ASTRO-F is the first Japanese dedicated infrared astronomical satellite which will be launched in 2005FY and is now in the final stage of the development. ASTRO-F is a 70 cm aperture cryogenically cooled telescope and designed for the infrared survey with much higher sensitivity and angular resolution than IRAS. We present the current status of the mission, focal plane instruments, and the observation plan now being discussed.
462
- OHASHI NAGAYOSHI
- Journal of the Korean astronomical society = 천문학회지
- 38, n.2
- pp.103-106
- 2005
- 원문 바로보기
The Submillimeter Array (SMA), a collaborative project of the Smithsonian Astrophysical Observatory (SAO) and the Academia Sinica Institute of Astronomy & Astrophysics (ASIAA), has begun operation on Mauna Kea in Hawaii. A total of eight 6-m radio telescopes comprise the array with currently working receiver bands at 230, 345, and 690 GHz. The array will have 8 receiver bands covering the frequency range of 180-900 GHz. The backend is flexible analog-digital correlator with a full bandwidth of 2GHz, which is very powerful to cover several line emissions simultaneously. The current status and future plans of the SMA are described with emphasis on Taiwanese efforts.
463
CURRENT STATUS OF THE INSTRUMENTS, INSTRUMENTATION AND OPEN USE OF OKAYAMA ASTROPHYSICAL OBSERVATORY
- YOSHIDA MICHITOSHI
- Journal of the Korean astronomical society = 천문학회지
- 38, n.2
- pp.117-120
- 2005
- 원문 바로보기
Current instrumentation activities and the open user status of Okayama Astrophysical Observatory (OAO) are reviewed. There are two telescopes in operation and one telescope under reforming at OAO. The 188cm telescope is provided for open use for more than 200 nights in a year. The typical over-subscription rate of observation proposals for the 188cm telescope is <TEX>${\~}$</TEX> 1.5 - 2. The 50cm telescope is dedicated to <TEX>$\gamma$</TEX>-ray burst optical follow-up observation and is operated in collaboration with Tokyo Institute of Technology. The 91cm telescope will become a new very wide field near-infrared camera in two years. The high-dispersion echelle spectrograph (HIDES) is the current primary instrument for the open use of the 188cm telescope. Two new instruments, an infrared multi-purpose camera (ISLE) and an optical low-dispersion spectrograph (KOOLS), are now under development. They will be open as common use instruments in 2006.
464
- Tadross, A.L.
- Journal of the Korean astronomical society = 천문학회지
- 38, n.3
- pp.357-363
- 2005
- 원문 바로보기
A deep stellar analysis is introduced for the poorly studied open cluster NGC 2509. The Near-IR database of the digital Two Micron All Sky Survey (2MASS) has been used to re-estimate and refine the fundamental parameters of the cluster, i.e. age, reddening, distance, and diameter. As well as, luminosity function, mass function, total mass, relaxation time, and mass segregation of NGC 2509 have been estimated here for the first time..
465
- KIM YONG HA
- Journal of the Korean astronomical society = 천문학회지
- 38, n.2
- pp.59-66
- 2005
- 원문 바로보기
A new ion transport code for planetary ionospheric studies has been developed with consideration of velocity differences among ion species involving ion-ion collision. Most of previous planetary ionosphere models assumed that ions diffuse through non-moving ion and neutral background in order to consolidate continuity and momentum equations for ions into a simple set of diffusion equations. The simplification may result in unreliable density profiles of ions at high altitudes where ion velocities are fast and their velocity differences are significant enough to cause inaccuracy when computing ion-ion collision. A new code solves explicitly one-dimensional continuity and momentum equations for ion densities and velocities by utilizing divided Jacobian matrices in matrix inversion necessary to the Newton iteration procedure. The code has been applied to Martian nightside ionosphere models, as an example computation. The computed density profiles of <TEX>$O^+,\;OH^+$</TEX>, and <TEX>$HCO^+$</TEX> differ by more than a factor of 2 at altitudes higher than 200 km from a simple diffusion model, whereas the density profile of the dominant ion, <TEX>$O_2^+$</TEX>, changes little. Especially, the density profile of <TEX>$HCO^+$</TEX> is reduced by a factor of about 10 and its peak altitude is lowered by about 40 km relative to a simple diffusion model in which <TEX>$HCO^+$</TEX> ions are assumed to diffuse through non-moving ion background, <TEX>$O_2^+$</TEX>. The computed effects of the new code on the Martian nightside models are explained readily in terms of ion velocities that were solved together with ion densities, which were not available from diffusion models. The new code should thus be expected as a significantly improved tool for planetary ionosphere modelling.
466
- LEE HYUNG MOK
- Journal of the Korean astronomical society = 천문학회지
- 38, n.2
- pp.333-334
- 2005
- 원문 바로보기
Astronomical research in Asian Pacific region has been growing rapidly in recent years. However, most important papers have been published in well established existing journals in US and Europe because we do not have high impact international journals in this region. I review the current trends of the local journals of East Asian countries and propose to establish a new regional journal by combining domestic journals.
467
- ANN HONG BAE
- Journal of the Korean astronomical society = 천문학회지
- 38, n.2
- pp.121-124
- 2005
- 원문 바로보기
High resolution images of the nuclear regions of nearby galaxies show that nuclear spirals are preponderant in normal galaxies as well as in active galaxies. These nuclear spirals, especially the grand-design nuclear spirals are found to be formed by the gas flow driven by the bar. Hydrodynamical simulations exploring a wide range of parameter space show that the morphology of nuclear spirals depends not only on the inner dynamics but on the global dynamics resulting from the global mass distribution of galaxies. Thus, the nuclear morphology can be a diagnostic tool for the inner dynamics of galaxies when the global mass distribution is taken into account.
468
- YUAN CHI
- Journal of the Korean astronomical society = 천문학회지
- 38, n.2
- pp.337-338
- 2005
- 원문 바로보기
This is to summarize a joint discussion on the future of EAMA in EAMA6. The emphasis was placed on the near future instead of the distant future, Formation of the Working Groups as a means to carry the cooperation for the regions was generally agreed by the attendants of EAMA6 to be the best way toward the establishment of future East Asian Observatory (EAO). Association of Core Observatories (ACO) was proposed to bring resources and foster joint projects for EAMA activities.
469
- NOUMARU JUNICHI
- Journal of the Korean astronomical society = 천문학회지
- 38, n.2
- pp.101-102
- 2005
- 원문 바로보기
Subaru Telescope proposes to hold Subaru East Asia Youth School (Tentative Name) in 2005.
470
- SAKAI TAKESHI
- Journal of the Korean astronomical society = 천문학회지
- 38, n.2
- pp.257-260
- 2005
- 원문 바로보기
We have mapped the W 3 giant molecular cloud in the <TEX>$C^o\;^3P_1-^3 P_o$</TEX> ([CI]) line with the Mount Fuji Submillimeter-wave Telescope. The [CI] emission is extended over the molecular cloud, having peaks at three star forming clouds; W 3(Main), W 3(OH), and AFGL 333. The [CI] emission is found to be strong in the AFGL 333 cloud. We have also observed the <TEX>$C^{18}O,\;CCS,\;N_2H^+$</TEX>, and <TEX>$H^{13}CO^+$</TEX> lines by using the Nobeyama Radio Observatory 45 m telescope. In the AFGL 333 cloud, we find two massive cores, which are highly gravitationally bound and have no sign of active star formation. The high [<TEX>$C^o$</TEX>]/[CO] and [CCS]/[<TEX>$N_2H^+$</TEX>] abundance ratios suggest that the AFGL 333 cloud is younger than the W 3(Main) and W 3(OH) clouds.