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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 95/122
941
- XU CHONGMING
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.17-18
- 1996
- 원문 바로보기
COBE's results on the anisotropy of the cosmic microwave background radiation (CMBR) is discussed. Some ambiguities in the linear GI cosmic perturbation theory are clarified. The problem of the last scattering surface and the deficiencies of the linear cosmic perturbation theory are mentioned. The possible ways to overcome the theoretical difficulties are discussed also.
942
- RIAZI N.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.283-284
- 1996
- 원문 바로보기
Wormhole solutions of general theory of relativity are known to violate energy conditions. We have considered the possibility of having wormhole solutions in Brans-Dicke theory which is the prototype of scalar-tensor theories of gravity.
943
- WATANABE TETSUYA
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.291-294
- 1996
- 원문 바로보기
The .Japanese sun observing satellite, Yohkoh, has been operational for five years and her scientific instruments are still in good condition. They have revealed ample of evidences that solar flares were triggered by magnetic reconnection, which was, for the first time, clearly indicated to take place in the solar corona. Cusp structures in soft X-rays and a new type of hard X-ray sources at the top of flaring loops have strongly supported the scenario originally proposed by C-S-H-KP. Nonthermal energy input in hard X-rays and thermal energy estimated from soft X-rays are fundamentally consistent with the interpretation of thick-target and chromospheric-evaporation models (Neupert effect). X-ray jets, another discovery of Yohkoh, were also associated with magnetic reconnection, as a result of the interaction of emerging fluxes with pre-existing coronal loops. Temperature structures of active regions, quiet sun, and coronal holes had very dynamic differential-emission-measure (DEM) distributions and high-temperature tails of DEM were considered to come from the contribution of flare-like activity.
944
- MANCHESTER R. N.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.209-211
- 1996
- 원문 바로보기
Recent surveys at Parkes, in particular the 70 cm survey of the southern sky, have discovered many pulsars, including 17 miilisecond pulsars in the Galactic disk. Timing and polarization observations of some of these pulsars are described. The only two pulsars known to be in orbit around massive non-degenerate stellar compamons were also discovered at Parkes, and some recent observational results for these pulsars are also presented.
945
- NEIZVESTNY S. I.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.77-78
- 1996
- 원문 바로보기
We perfom a large project for complex study of Blue Compact Galaxies (BCGs) with strong star formation, which includes optical spectroscopy, BVR CCD photometry and HI 21 cm radio survey. The most interesting galaxies are studied also with HST and VLA. In the frame of this project we began the study of H<TEX>$\alpha$</TEX> morphology of BCGs with 6-m telescope. We present and discuss here the results for the first 6 galaxies. We found the noticeable variety of forms for H<TEX>$\alpha$</TEX> morphology comparing to broad band images: from very compact HII region in very center of stellar body (Mark 996, possible dwarf post-merger, old galaxy experiencing strong star formation burst), to very extended gas emission encompassing the whole area traced by stars (SBS 0335-052, the most probable young galaxy in formation).
946
- MCGREGOR PETER J.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.119-122
- 1996
- 원문 바로보기
The case for a massive black hole in the center of the Galaxy is reassessed using improved modeling techniques and observational data. A dark mass of <TEX>${\~}{\times} 10^6$</TEX> Mo is present within 0.2 pc of the Galactic center. However, the available data can be modeled, without appealing to a massive black hole, using an extended distribution of dark stellar remnants (neutron stars and stellar mass black holes) provided that the stellar initial mass function in the central parsec is deficient in stars less massive than <TEX>$\~$</TEX>1 Mo. Such a situation may be a natural consequence of repeated gas build-up followed by starbursts in the central region. A clear distinction between this and the massive central black hole model cannot be made using red giant tracers outside 0.2 pc due to uncertainties in the radial velocity dispersion distribution. The cluster of massive early-type emission-line stars in the central parcsec more effectively probe the mass distribution close to Sgr A <TEX>$\ast$</TEX>, but their small number and partial rotational support complicate mass determinations. Proper motion determinations for stars within 0.5' of Sgr A<TEX>$\ast$</TEX> may be the most effective means of unambiguously determining the mass distribution in the immediate vicinity of the Galactic center.
947
- KANG IVIIN-YOUNG
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.263-264
- 1996
- 원문 바로보기
We have solved the radiative transfer problem using a Sobolev approximation with an escape probability method in case of the supersonic expansion of a stellar envelope to an ambient medium. The radiation from the expanding envelope turns out to produce a P-Cygni type profile. In order to investigate the morphology of the theoretical P-Cygni type profile, we have treated <TEX>$V{\infty},\;V_{sto},\;{\beta}$</TEX> (parameter for the velocity field), M and <TEX>$\epsilon$</TEX> (parameter for collisional effect) as model parametrs. We have found that the velocity field and the mass loss rate affect the shapes of the P-Cygni type profiles most effectively. The secondarily important factors are <TEX>$V{\infty},\;V_{sto}$</TEX>. The collisional effect tends to make the total flux increase but not so .much in magnitude. We have infered some physical parameters of 68 Cyg, HD24912, and <TEX>$\xi$</TEX> persei such as V<TEX>$\infty$</TEX>, M from the model calculation, which shows a good agreement with the observational results.
948
- YOSHIDA S.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.381-383
- 1996
- 원문 바로보기
A new CCD camera equipped with a large format chip is now under construction for the Kiso 105-cm Schmidt telescope. We use SITe TK2048E, of which pixel size is 24 <TEX>${\mu}m$</TEX> and chip size is 48 mm square. TK2048E is thinned back-illuminated so that it has high sensitivity in U-band. The chip is cooled by a refrigerator instead of liquid nitrogen. MESSIA III is used as CCD control system.
949
- LEE C. W.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.161-163
- 1996
- 원문 바로보기
We have studied the response of molecular clouds in the Galactic disk to a rotating bar by conducting Smoothed Particle Hydrodynamics (SPH) simulations for the Galaxy in order to understand the dynamical structures of the Galactic Center (GC) molecular clouds, and their implications. In our study it was found that the structures of GC molecular clouds could be induced by the combined effects of rotating bar potential, the hydrodynamic collisions and gravitational miss collisions between the clouds.
950
- STEINITZ RAPHAEL
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.237-238
- 1996
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