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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 85/122
841
- KIM SANG CHUL
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.83-84
- 1996
- 원문 바로보기
842
- DRURY L O'C
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.267-270
- 1996
- 원문 바로보기
The problem of the origin of cosmic rays is considered in an astronomical context and the current observational situation summarised. The evidence for acceleration in supernova remnants is critically examined.
843
- SAHNI V.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.19-21
- 1996
- 원문 바로보기
We apply topological measures of clustering such as percolation and genus curves (PC & GC) and shape statistics to a set of scale free N-body simulations of large scale structure. Both genus and percolation curves evolve with time reflecting growth of non-Gaussianity in the N-body density field. The amplitude of the genus curve decreases with epoch due to non-linear mode coupling, the decrease being more noticeable for spectra with small scale power. Plotted against the filling factor GC shows very little evolution - a surprising result, since the percolation curve shows significant evolution for the same data. Our results indicate that both PC and GC could be used to discriminate between rival models of structure formation and the analysis of CMB maps. Using shape sensitive statistics we find that there is a strong tendency for objects in our simulations to be filament-like, the degree of filamentarity increasing with epoch.
844
- LAI S. P.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.327-328
- 1996
- 원문 바로보기
845
- KURTANIDZE OMAR M.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.129-131
- 1996
- 원문 바로보기
The results on the deep low dispersion (1250 <TEX>${\AA}$</TEX>/mm at <TEX>$H_r</TEX>, <TEX>$30^{\circ}$</TEX> < I < <TEX>$165^{\circ}$</TEX>, <TEX>$195^{\circ}$</TEX> < I < <TEX>$210^{\circ}$</TEX>, [b] < <TEX>$5^{\circ}$</TEX>; 7000<TEX>${\AA}$</TEX>/mm at A band, <TEX>$50^{\circ}$</TEX> < I < <TEX>$115^{\circ}$</TEX>, b=<TEX>$0^{\circ}$</TEX>, b=<TEX>${\pm}3.5^{\circ}$</TEX>) spectral surveys of the MILKY WAY are presented. More than 2250 carbon stars were identified among them 1440 new ones. The C/M5+ ratio increases from 0.02 to 0.3 when longitude varies from <TEX>$30^{\circ}$</TEX> to <TEX>$210^{\circ}$</TEX>. On the basis of A GENERAL CATALOG OF GALACTIC COOL CARBON STARS the surface distribution of carbon stars has been studied.
846
- TRIVEDI CHETNA
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.345-346
- 1996
- 원문 바로보기
The contrasting values of the oscillator strengths for the (0,0) band of SiH+ molecules for the <TEX>$A\;^1II-X\;^1{\sum}+$</TEX> transition reported in literature, motivated us to reinvestigate the same with the help of a new set of well accepted solar photospheric models, elemental abundances and dissociation energy.
847
- Xu WENLI
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.399-400
- 1996
- 원문 바로보기
LAMOST is a special reflecting Schmidt telescope. Both the refleting Schmidt plate <TEX>$M_A$</TEX> and the spherical primary mitrror <TEX>$M_B$</TEX> are segmened mirrors. These two cofocus but not co-phase. The diffraction of the optical system is decided by the shape overlapping of <TEX>$M_A$</TEX> and <TEX>$M_B$</TEX>. This paper describes the diffraction caculating results with different declination and different field angle. The diffraction influence to the image quality is acceptable in the error buget of optical system. It also proves that the size seletion of the sub-mirror is reasonable.
848
- ALMLEAKY Y. M.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.317-319
- 1996
- 원문 바로보기
Utilizing a Calcium filter, a large two ribbon flare of an importance 2.5Xj31? was recorded at. King Abdul-Aziz University Solar Observatory (KAAUSO) at the 30th of October 1991. This chromosphenc flare observation, which is of special importance since it is rarely reported, was for a flare that occurred near the south west of the equator at the vicinity of a large sunspot group on an active region known as AR 6891. The observed foot points of this flare had a strange behavior in which the separating motion of the ribbons were not typical of most flares, rather were nearly orthogonal. In this article we present the characteristics of the main sunspot group of this active region and try to investigate its evolution and fragmentation with time. Information regarding magnetic fields and velocity fields are necessary to understand the restructuring of the magnetic field pattern and plasma motion, and hence the changes that could lead to the occurrence of such an interesting flare.
849
- 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.
850
- MATSUHARA H.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.171-172
- 1996
- 원문 바로보기
We present the results of an rocket-borne observation of far-infrared [CII] line at 157.7 <TEX>${\mu}m$</TEX> from the diffuse inter-stellar medium in the Ursa Major. We also introduce a part of results on the [CII] emission recently obtained by the IRTS, a liquid-helium cooled 15cm telescope onboard the Space Flyer Unit. From the rocket-borne observation we obtained the cooling rate of the diffuse HI gas due to the [CII] line emission, which is <TEX>$1.3{\pm}0.2 {\times} 10^{-26}$</TEX> <TEX>$ergss^{-1} H^{-1}_{atom}$</TEX>. We also observed appreciable [CII] emission from the molecular clouds, with average CII/CO intensity ratio of 420. The IRTS observation provided the [CII] line emission distribution over large area of the sky along great circles crossing the Galactic plane at I = <TEX>$50^{\circ}$</TEX> and I = <TEX>$230^{\circ}$</TEX>. We found two components in their intensity distributions, one concentrates on the Galactic plane and the another extends over at least <TEX>$20^{\circ}$</TEX> in Galactic latitude. We ascribe one component to the emission from the Galactic disk, and the another one to the emission from the local interstellar gas. The [CII] cooling rate of the latter component is <TEX>$5.6 {\pm} 2.2 {\times}10$</TEX>.