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REFERENCE LINKING PLATFORM OF KOREA S&T JOURNALS
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Journal of Astronomy and Space Sciences
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The Korean Space Science Society
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Volume 8, Issue 2 - Dec 1991
Volume 8, Issue 1 - Jun 1991
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TIME-DEPENDENT DUST FORMATION IN NOVAE
Suh, Kyung-Won ;
Journal of Astronomy and Space Sciences, volume 8, issue 1, 1991, Pages 1~10
The dust formation processes in novae are investigated with close attention to recent infrared observations. Using mainly the classical nucleation theory, we have calculated the time scales of dust formation and growth in the environments of novas. Those time scales roughly the typical observations. We have classified the dust-forming novae into three classes according to their explosion properties and the thermodynamic properties of dust grains. Oxygen grains form much later than carbon grains because of their thermodynamic properties. The effect of grain formation to the efficiency of stellar winds to drive the material outward is tested with newly obtained Planck mean values of dust grains.
THE DYNAMICAL EVOLUTION OF GLOBULAR CLUSTERS WITH STELLAR MASS LOSS
Kim, Chang-Hwan ; Chun, Mun-Suk ; Min, Kyung-W. ;
Journal of Astronomy and Space Sciences, volume 8, issue 1, 1991, Pages 11~23
The dynamical evolution of globular clusters is studied using the orbit-averaged multicomponent Fokker-Planck equation. The original code developed by Cohn(1980) is modi-fied to include the effect of stellar evolutions. Plommer's model is chosen as the initial density distribution with the initial mass function index
=0.25, 0.65, 1.35, 2.35, and 3.35. The mass loss rate adopted in this work follows that of Fusi-Pecci and Renzini(1976). The stellar mass loss acts as the energy source, and thus affects the dynamical evolution of globular clusters by slowing down the evolution rate and extending the core collapse time Tcc. And the dynamical length scale
is also extended. This represents the expansion of cluster due to the stellar mass loss.
SPECTROSCOPIC STUDY OF 31 CYGNI
Song, Hye-Kyeong ; Chun, Mun-Suk ;
Journal of Astronomy and Space Sciences, volume 8, issue 1, 1991, Pages 25~51
The spectra of 31 Cygni were taken at the Asiage Observatory in Italy. Reduction was made using the 2nd and 4th order non-linear least square method. Spectral lines which were relatively sharp or strong were identified within the wavelength regions from 3800 to 5100
. Radial velocities and equivalent widths were calculated from the Gaussian Fitting Method for this star. The measured mean radial velocity of 31 Cygni is + 0.5km/sec.
IUE ARCHIVAL SPECTRA OF 31 CYGNI
Kang, Young-Woon ;
Journal of Astronomy and Space Sciences, volume 8, issue 1, 1991, Pages 53~61
UV light curve of 31 Cygni has been made from the IUE high dispersion specta. The depth of primary minimum of the light curve is 5.2 magnitudes because the B4 star's steep spectral gradient. The light curve has been analyzed by the method of Wilson and Devinney Differential Correction (WD). The radial velocities have been measured using the Mg II h lines. The spectroscopic elements have been determined by the method of WD. The change of the Mg II resonance doublet has been investigated based on the eight representative spectra taken at well distributed orbital phases.
THE WIND VELOCITIES DRIVEN BY ALFVEN WAVES IN 31 CYG
Journal of Astronomy and Space Sciences, volume 8, issue 1, 1991, Pages 63~72
THE PHOTOMETRIC STUDY FOR THE LONG PERIOD INTERACTION CLOSE BINARY AQ CAS
Journal of Astronomy and Space Sciences, volume 8, issue 1, 1991, Pages 73~83
UBV light curves of an early type close binary AQ Cas are made with the observations obtained at Yonsei University from 1982 to 1989. Light losses in U are shown at the phase around 0.55 and 0.90 which might be produced by the stream of mass transfer. Four times of minimum light derived from our observations. With the collected minima including ours, new light elements are determined. Phtometric solution with B and V light curves is made by using Wilson-Devinney codes.
ATTITUDE CONTROL OF SMALL SCIENTIFIC SATELLITE USING GEOMAGNETISM
Journal of Astronomy and Space Sciences, volume 8, issue 1, 1991, Pages 85~98
Geomagnetism was used to control the attitude of the small scientific satellite at low altitude in sun-synchronous orbit. First, we analyzed the telemetry data. The rotation state of the satellite, can be known from the magnitude and variations of the magnetic field which is measured from the 3 axis magnetometer. In axisymmetric case, it is possible to control the attitude of the satellite by changing the rotation velocity of each 3 axis. The algorithm and the program were developed to calculate the supply time of the current operating the magnetorquer. This attitude control can be applied when the satellite is in tumbling motion and after passive control is attained by the Gravity gradient boom.
A STUDY ON THE TRACKING AND POSITION PREDICTIONS OF ARTIFICIAL SATELLITE(II) - A Study on the Orbit Prediction -
Journal of Astronomy and Space Sciences, volume 8, issue 1, 1991, Pages 99~113
We developed a software system called IODS(ISSA Orbit Determination System), which can predict the orbit of arbitary artificial satellite using the numerical method. For evaluating the orbit prediction accuracy of IODS, the orbital data predicted for the meteorological satellite NOAA-11 and the stationary satellite INTELSAT-V are intercompared with those tracked at the Central Bureau of Meterology and the Kum-San Satellite Communication Station. And the Perturbations affecting the orbit of these artificial satellites are quantitatively analyzed. The orbital variation and the eclipse phenomina due to the shadow are analyzed for a hypothetical geostationary satellite called KORSAT-1 which is assumed to be located in longitude
AN ANALYSIS OF THE AUTOMATCHING USING LANDSAT TM DATA AND ASTRONOMICAL APROACH
Journal of Astronomy and Space Sciences, volume 8, issue 1, 1991, Pages 115~123
Automatching algorithm is suitable for cross-correlation, which showed correlation surface about maximal correlation coefficient. The size of the window area must be determined empirically, whereas window size generally chosen as a compromise between speed and accuracy. It is possible that epipolar transform prevented from mismatching and decreased search space. In application of the astronomical fields, automatching algorithm mainly used to planet surface recovery in satellite image.