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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 82/119
811
- ZHOU HONG NAN
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.443-444
- 1996
- 원문 바로보기
From 146 B.C. to A.D. 1760, 363 sets of cometary observations have been recorded in Chinese Ancient Records of Celestial Phenomena. The positions of all recorded comets, or their paths, on the sky are compared. Taking into account the perturbations of all nine planets and using the numerical method of N-body problem, the orbits of well-recorded comets are calculated. Identification of a periodic comet is presented.
812
- BESKIN G. M.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.251-252
- 1996
- 원문 바로보기
813
- YERSHOV V. N.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.385-386
- 1996
- 원문 바로보기
A wide-field CCD detector for solar eclipse observations is discussed. The CCD is supposed to be of a moderate size, and the image of the corona is obtained by scanning the field of view. Results of the 1995 solar eclipse observation are shown which have been made with a prototype of the scanning CCD detector.
814
- KOMAROVA V. N.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.217-218
- 1996
- 원문 바로보기
The results of the Crab pulsar observations with the photometrical MANIA (Multichannel Analysis of Nanosecond Intensity Alterations) complex at the 6-m telescope are presented. More than 12 millions photons in UBVR-bands simultaneously with time resolution of <TEX>$10^{-7}s$</TEX> were detected. Using the original software for search for optical pulsar period, we obtained the light curves of the object with time resolution of about 3.3 <TEX>${\mu}s$</TEX>. Their detailed analysis gives the spectral change during pulse and subpulse, the shape of the pulse peaks, which are plateaus (with the duration of about 50<TEX>${\mu}s$</TEX> for the main pulse), limits for an amplitude of fine temporal (stochastic and regular) structure of pulse and sub pulse and the interpulse space intensity. The results of CCD-spectroscopy of the Crab pulsar show that its summarized spectrum is flat. There are no lines, neither emission nor absorbtion ones. Upper limit for line intensity or depth is <TEX>$3.5\%$</TEX> with the confidence probability of <TEX>$95\%$</TEX>.
815
- SANGUANSAK N.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.169-170
- 1996
- 원문 바로보기
In the past, it. was very difficult to distinguish thermal and non-thermal emission. Broadbent et a1. (1989) has developed a new technique with the help of the IRAS 60 micron emission. The distribution of non-thermal or synchrotron emission in the Galactic disk has been modeled from the 408 MHz all sky survey of Haslam et a1. (1982) after removal of the thermal component.. At. 408 MHz, t.here is very little absorption in the interstellar medium and the distribution along the line-of-sight. is inferred mainly from its presumed relationship to other tracers of spiral structure via a. number of fitted parameters. But. at lower frequencies, free-free absorption becomes important and can give some direct. information on the line of sight. distribution. We have modeled the thermal electron density according to the spiral arm models and the distribution of ionized hydrogen in the Galactic plane by Lockman (1976) and Cersosimo et. al. (1989) and have made predictions to compare with the surveys of Dwarakanath et al. (1990) at. 34.5 MHz and .Jones and Finlay (1974) at 29.9 MHz. The result confirms that the absorption model of the synchrotron emissivity in the Galactic plane is broadly corrected and illustrates the potential of the absorption technique.
816
- STALIN C. S.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.341-342
- 1996
- 원문 바로보기
We present here the solar LOG GF values obtained using the Liege solar at las and the standard solar photospheric models for the spectral lines in the wavelength range <TEX>${\lambda}{\lambda}$</TEX> 6209 - 6273 <TEX>${\AA}$</TEX>. These log gf values shall be used to interpret a high resolution spectra of the star <TEX>$\gamma$</TEX> Draconics.
817
- KIM SEUNG-LEE
- Journal of the Korean astronomical society = 천문학회지
- 29, n.1
- pp.31-41
- 1996
- 원문 바로보기
We present results of time-series CCD photometry for 178 stars in the young open cluster M29 (=NGC6913). Total 1036 V-band CCD frames were collected for five nights between August 12 and September 13, 1994. The photometric precision is about 7.6 mmag for 9th-10th mag stars in M29 with exposure times of 30 seconds. From the dispersion diagram and the light curves, one detached eclipsing binary (HD194378) and two suspected variables are newly discovered. <TEX>$A\;\gamma\;Cas$</TEX> type variable, V1322 Cyg, which has been known as a member of M29, did not show any light variations during the period of present observations, indicating that it passed the steady phase without the eruption during our observing runs.
818
- CHEN ROSIE CHANG-HUI
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.135-136
- 1996
- 원문 바로보기
We present a new photometric study of the globular cluster NGC288 in Stromgren u, v, b, y, and H<TEX>$\beta$</TEX> system. This cluster is known to have an intermediate metallicity but its color-magnitude diagram has a pure blue horizontal branch, which is a signature of metal poor stellar population. We compare our dataset with Bergbusch's (1993) in both field size and CMD to see whether different photometry system would determine the same physical parameters of a cluster. Demarque and Yi's isochrones (1996, private communication) were applied to Bergbusch's dataset, and we obtained distance modulus of (m - M) = 14.9 <TEX>$\pm$</TEX> 0.2, color excess of E(B - V) = 0.03, and age of 1.5<TEX>$\pm$</TEX>3 Gyr. Vandenberg's (1985) isochrones for Stromgren system were also applied to Bergbusch's and our data. We find that the isochrone fits to different photometric systems give rather in consist ant solutions. The source of this discrepancy may become clear when the Demarque and Yi's isochrones for Johnson system are converted to those of Stromgren system. We note that Kurucz model atmospheres provide a useful ground for this conversion work as well as theoretical study of Stromgren characteristics of globular cluster stars.
819
- SUBRAMANIAN K.
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.155-158
- 1996
- 원문 바로보기
Magnetic fields correlated on several kiloparsec scales are seen in spiral galaxies. Their origin could be due to the winding up of a primordial cosmological field or due to amplification of a small seed field by a turbulent galactic dynamo. Both options have difficulties: There is no known battery mechanism for producing the required primordial field. Equally the turbulent dynamo may self destruct before being able to produce the large scale field, due to excess generation of small scale power. The current status of these difficulties is discussed. The resolution could depend on the nature of the saturated field produced by the small scale dynamo. We argue that the small scale fields do not fill most of the volume of the fluid and instead concentrate into intermittent ropes, with their peak value of order equipartition fields, and radii much smaller than their lengths. In this case these fields neither drain significant energy from the turbulence nor convert eddy motion of the turbulence on the outer scale to wave like motion. This preserves the diffusive effects needed for the large scale dynamo operation.
820
- KIM BONG GYU
- Journal of the Korean astronomical society = 천문학회지
- 29, n.suppl1
- pp.193-194
- 1996
- 원문 바로보기
A large scale <TEX>$^{13}CO$</TEX>(J=1-0) survey was made for CMa OB1/R1 region in <TEX>$220^{\circ}{\le}{\iota}{\le}230^{\circ}$</TEX> and <TEX>$-10^{\circ}{\le}b{\le}10^{\circ}$</TEX> with a 8' spacing by using the 4 m radio telescope of Nagoya University. 34 isolated clouds were identified in this survey. Among them, two clouds were firstly identified by us. The observed LSR velocity indicate that almost of the all clouds are located in the Local arm, except two extreme velocity. The mass spectrum of the clouds in the Local arm is best fitted by a power-law index of 1.6.