모달창 닫기
- 홈으로 이동
1968년 ~ 2025년까지 1,227 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 : 1,227건 (DB Construction : 1,227 Articles)
총 게시글 1,227건
페이지 97/123
961
- 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).
962
- 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.
963
- 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.
964
- 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.
965
- 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.
966
- STEINITZ RAPHAEL
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.237-238
- 1996
- 원문 바로보기
967
- KIM SANG-JOON
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.347-350
- 1996
- 원문 바로보기
Spectroscopic data between 7 and 15 microns obtained in 1979 by Voyager 1 and 2 Infrared Interferometer Spectrometer (IRIS) have been revisited. Using the spectral data, Jupit.er images have been constructed at the emission bands of hydrocarbons, such as methane, ethane, and acetylene. The resultant. images show differences in emission intensities in the polar regions, suggesting inhomogeneous distributions of the hydrocarbons over the auroral regions of Jupiter.
968
- ANDERSEN J.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.127-128
- 1996
- 원문 바로보기
The solar neighbourhood is the starting point for studies of the structure and evolution of the Galactic disk. Yet, our knowledge of the relative frequencies, distances, ages, chemical abundances, velocities, and birthplaces of the nearby stars is severely incomplete. We have determined complete, homogeneous, and precise such data for a kinematically unbiased sample of <TEX>$\~$</TEX>12,000 local F and G dwarf stars and describe a first, significant result from it.
969
- DHURANDHAR S. V.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.273-276
- 1996
- 원문 바로보기
The world wide efforts for detecting gravitational waves, the detectors in vogue and the expected astrophysical sources of gravitational waves will be discussed. Ground based detectors especially, the resonant bar detectors and laser interferometers will be described with a brief mention of the space based detector (the LISA project). Astrophysical sources of gravitational waves such as coalescing binaries, supernovae, pulsars/ rotating neutron stars, stochastic background will be discussed in the context of detection.
970
- WEE SUN-OK
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.147-148
- 1996
- 원문 바로보기
We have estimated a metal abundance of [Fe/H]= -0.48 <TEX>$\pm$</TEX> 0.14 dex, a reddening of E(B- V)= 0.30 mag, an age of 2.0 <TEX>$\pm$</TEX> 0.4 Gyr, and a distance of 7.9 <TEX>$\pm$</TEX> 0.8 kpc for Tombaugh 2 using the Washington filter system.