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1968년 ~ 2023년까지 1,187 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 : 1,187건 (DB Construction : 1,187 Articles)
총 게시글 1,187건
페이지 85/119
841
- IWASAKI KYOSUKE
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.357-358
- 1996
- 원문 바로보기
Reanalysis of the observations of Mars made at the Hida Observatory in 1975 with a new image processing method is reported. Red filter images taken in the period before vernal equinox (areocentric longitude of the sun Ls=<TEX>$0^{\circ}$</TEX>) revealed dark surface features at the northern high latitudes, while blue filter images taken at the same time showed the extensive polar hood. The latitude of the northernmost feature observed was about <TEX>$67^{\circ}$</TEX>N. An extensive north polar cap, which is predicted by most of the existing models and observed with Viking, did not exist in our reanalyzed images obtained at the Hida Observatory in 1975.
842
- LEE SANG-GAK
- Journal of the Korean astronomical society = 천문학회지
- 29, n.2
- pp.157-170
- 1996
- 원문 바로보기
In order to determine the metallicity of a globuar cluster, M3,by using the spectral indices, a kind of index grid has been establshed by stars in globular clusters, M3, M15, M71 and old open cluster, NGC 188. The indices were measured from the medium resolution spectra of about <TEX>$2{\AA}$</TEX>. The summed indices were used to determine metallicity in order to increase signals. It is found that the core depth index is measured more accurately and leads result more accurate than the pseudo-equivalent width index. This method can be further improved by including many more calibration globular clusters of various metallicity to make finer grids. By this method, the metallicity of M3 is determined as <TEX>$[Fe/H] = -1.46\pm0.15$</TEX>.
843
- MAKOTO INOUE
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.419-420
- 1996
- 원문 바로보기
The VLBI Space Observatory Program (VSOP) is a worldwide project of one radio telescope in space with many ground radio telescopes. The concerted space VLBI network enables us to reveal high resolution and high quality images of radio sources. The space radio telescope is anticipated to be launched in January/February 1997, and collaborative observations have been coordinated. The basic parameters of the system and present status are given.
844
- LI BI-QIANG
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.299-301
- 1996
- 원문 바로보기
It. has been discovered that. active regions commonly have numerous flare-like transient. loop brightenings. We use a magnetic reconnection theory driven by a ponderamotive force on account. of the basic properties of a transient. brightening: lifetime a few mins, total energy <TEX>$10^{25}\~10^{29}$</TEX> erg. The numerical results are consistent with the observations.
845
- ANDERSEN J.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.239-240
- 1996
- 원문 바로보기
Precise masses, radii, and luminosities from eclipsing binaries and colour-magnitude diagrams for open clusters are classic tools in empirical tests of stellar evolution models. We review the accuracy and completeness required for such data to discriminate between current models and describe some recent. results with implications for convection theory.
846
- LYO A-RAN
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.65-66
- 1996
- 원문 바로보기
847
- ISOBE SYUZO
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.451-453
- 1996
- 원문 바로보기
There is a question, 'Which is beautiful, a flower or a star?'. Its answer is different from one person .to another. It is only a matter of what one is interested in. It is very difficult for most school pupils, who will have non-scientific jobs, to understand science courses taught currently in school, because each science (physics, chemistry, biology, and earth science) is independently taught from the other sciences. Therefore, their knowledge of sciences obtained during their school period does not significantly help their understanding of global environmental problems. I am proposing that several scientific stories should be prepared to connect all the related scientific phenomena in order to give those pupils ideas in understanding global environmental problems. I believe that astronomy is able to play an important role in this context.
848
- LEE MYUNG GYOON
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.67-68
- 1996
- 원문 바로보기
849
- CHAKRABARTI SANDIP K.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.229-230
- 1996
- 원문 바로보기
850
- AGRAWAL P. C.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.429-432
- 1996
- 원문 바로보기
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 <TEX>$98^{\circ}$</TEX> and has three axis stabilized pointing capability. Each pointed-mode Proportional Counter (PPC) is a multilayer, multianode unit filled with P-10 gas (<TEX>$90\%$</TEX> Ar + <TEX>$10\%\;CH_4$</TEX>) 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 <TEX>$2^{\circ}{\times}2^{\circ}$</TEX> defined by silver coated aluminium honeycomb collimators. The total effective area of the three PPCs is about 1200 <TEX>$cm^2$</TEX>. The PPCs are sensitive in 2-20 keV band. The XSM consists of a pin-hole of 1 <TEX>$cm^2$</TEX> area placed 16 cm above the anode plane of a 32 cm<TEX>$\times$</TEX>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.