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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 & Issues
Volume 11, Issue 2 - Dec 1994
Volume 11, Issue 1 - Jun 1994
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MAGNETOSPHERIC STRUCTURE OF THE INTERMEDIATE POLAR
Kim, Yong-Gi ;
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 1~12
The structure of the magnetic funnel element in the intermediate polar is considered in terms of an important site for the X-ray absorption and the reemission of the X-ray as the optical light. In this paper the column density and the optical depth vary with the filling factor, which is introduced to characterize the structure of matter in the magnetic funnel element. The results of the energy dependence of the X-ray spectrum and the modulation depth of the X-ray light curve are discussed.
THE SPECTROSCOPIC STUDIES OF THE LONG PERIOD ECLIPSING BINARY AZ CAS
Cheon, Mun-Seok ; Sohn, Young-Jong ;
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 13~20
Spectroscopic observations of the long period eclipsing binary AZ Cas were made using 122cm telescope/Image Tube. From the relatively sharp and strong spectral FeI lines we can calculate the mean radial velocity as -39.7km/sec. The estimated equivalent widths of some atomic lines are well fitted to the phase of the AZ Cas.
UBV PHOTOMETRY AT THE OUTSIDE ECLIPSE PHASE OF AZ CASSIOPEIAE
Nha, Il-Seong ;
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 21~30
VV Cep-type long period spectroscopic-eclipsing binary AZ Cas has been observed for five years, 1985 Oct~1990 Feb, UBV at the Ilsan Station of Yonsei University Observatory. A total of 431 observations (U=129, B=142 and V=160) are made for 86 nights. Instrumental differential UBV and B-V light curves made with these observations cover phases nearly a half of one period. There is no appreciable light variation in V but in other two passbands a gradual decrease of the brightness is clearly noticed. The loss of light in B resulted in a reddening in
by + 0.06 at phases between 0.4~0.5 as compared with that of at phase ~0.1. This intrinsic reddening arouses a question why at the orbital phase of the transit of a hot star in front of a cool M supergiant the heating of the facing hemisphere of M supergiant by the strong radiation from the B stat is absent. With regard to this unusual situation we propose a hypothesis that a large amount of gas stream of low temperature ejected from the surface of M supergiant component towards the B star dominates the brightness of B star and the reflection effect.
UV ENERGY DISTRIBUTION OF AZ CASSIOPEIAE
Kang, Young-Woon ;
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 31~40
The IUE low dispersion spectra of AZ Cas have been analyzed for line identifications and energy distribution in ultraviolet region. Highly ionized atoms, SiIV and CIV are identified. We could infer a temperature range of the B star between 15,000K and 20,000K. The energy density distribution shows a hump between IUE short wavelength and long wavelength regions. Photometric and spectroscopic elements were revised based on the Florkowisk photeelectric observations and collected radial velocities. The temperature of both stars were reduced as 16,000K and 3,800K. The radii of both stars are
. The eccentricity and longitude of periastron are 0.61 and
NEW DESIGN CONCEPT FOR UNIVERSAL CCD CONTROLLER
Han, Won-Yong ;
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 41~52
Currently, the CCDs are widely used in astronomical observations either in direct imaging use or spectroscopic mode. However according to the recent technical advances, new large format CCDs are rapidly developed which have better performances with higher quantum efficiency and sensitivity. In many cases, some microprocessors have been adopted to deal with necessary digital logic for a CCD imaging system. This could often lack the flexibility of a system for a user for to upgrade with new devices, especially if it is a commercial product. A new design concept has been explored which could provide the opportunity to deal with any format of devices from any manufactures effectively for as tronomical purposes. Recently available PLD (Programmable Logic Devices)technology makes it possible to develop such digital circuit design, which can be integrated into a single component, instead of using micrprocessors. The design concept could dramatically increase the efficiency and flexibility of a CCD imaging system, particularly when new or large format devices are available and to upgrade the performance of a system. Some variable system control parameters can be selected by a user with a wider range of choice. The software can support such functional requirements very conveniently. This approach can be applied not only to astronomical purpose, but also to some related fields, such as remote sensing and industrial applications.
OZONE MEASUREMENTS IN THE STRATOSPHERE FROM KSR420S-1 AND -2
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 53~70
The Korean sounding rockets(KSR420S-1, -2) equipped with ozone detectors have b3en launched at An-heung, Chungchungnam-do, on June 4 and September 1, 1993, respectively. The ozone detector is used to measure the attenuation of solar UV radiation for various frequency bands in the stratosphere, to obtain vertical profiles of the ozone number density in the stratosphere. They confirm that the maximum ozone densities occur near 25 km, which is quite consistent with the mean value in the mid-latitude region. Our results from KSR420S-1 and -2 are compared with the other observation data from the Dobson spectrophotometer at Yonsei Univ., the LIDAR at Kyunghee Univ., the SBUV from Nimbus satellite, and the TOVS from NOAA satellite, which were performed simultaneously with the sounding rocket experiments.
THE MEASUREMENT OF THE IONOSPHERIC TOTAL ELECTRON CONTENT USING P-CODE OF GPS
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 71~80
It is generally known that the measurement of the ionospheric total electron content(TEC) by GPS can more accurately monitor the broader area of the ionosphere than other current methods. \Ve measured the TEC along a slant path considering the arrival time differences of P-code which is transmitted from GPS satellites with the modulation on two L-band carrier frequencies, L1 (1574.42MHz) and L2 (1227.60MHz). Under the assumptions that the ionosphere is uniformly distributed and its average height is 350km, we transformed the slant TEC to the vertical TEC at the point that the line-of-sight direction to GPS satellite cut across the average height of the ionosphere. Because there is no dual frequency P-code GPS receiver in Korea, we used the data observed at the TAIW GPS station (
) in Taiwan which is one of the core stations in International GPS and Geodynamics Services (IGS). The TEC values obtained in this work showed a typical daily variation of the ionosphere which is high in the daytime and low in the nighttime. Our results are found to be consistent with the SOLAR-DAILY data of NOAA and the Klobuchar's model for the ionospheric correction of GPS. In addition, in the cornparision with SOLAR-DAILY data, we estimated the precision of our TEC measurement as 2 TEC.
GLOBAL MAPPING OF NEAR-EARTH MAGNETIC FIELDS MEASURED BY KITSAT-1 AND KITSAT-2
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 81~92
The magnetic field measurements from the KitSat-1 and KitSat-2 were tested by comparing with the IGRF model. The magnetic data have been collected by a three-axis fluxgate magnetometer on each satellite at an latitude of 1,325 km and 820 km, respectively. To avoid highly variable magnetic disturbances at the polar region, the field map has been within the limits of 50 degrees in latitude. Each data is averaged over the square of
degrees in both latitude and longitude. In these results, the relatively quiet periods were selected and the sampling rate was 30 seconds. It is shown that the results from these measurements are consistent with the IGRF map over the global surface map.
EFFECTS OF THE RING CURRENT ON ULF WAVES IN THE MAGNETOSPHERE
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 93~106
A three-dimensional box model has been developed to study the MHD wave coupling in the magnetosphere. In this model, the effects of the ring current are included by assuming the pressure gradients in the MHD equations. It is found that the axisymmetric ring current may play an important role in producing spectral noises in compressional waves, while field line resonances have no such disturbances. These results may explain the current observational characteristics that compressional cavity modes hardly appear in the satellite experiment, while field line resonances often occur. Our numerical resluts also suggest that any discrete spectral peaks such as the global cavity modes can hardly occur where the pressure distribution of the ring current becomes important. The continuous band of transverse waves is found to be unperturbed until the ring current becomes significantly asymmetric with respect to the dipole axis. In addition, our results in the absence of the pressure gradient are found to be consistent with the previous results from the box-like and dipole models.
DETERMINATION OF WIND PARAMETERS BY THE METHOD OF DIFFERENTIAL CORRECTIONS
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 107~114
This paper describes a method for the determination of wind parameters as mass-loss rate, wind velocity, stochastic velocity in Zeta Aurigae type binaries. We have modified the Baade's (1989) computer code to analyze the wind parameters of Zeta Aurigae type binaries according to the least squares criterion. The modified program adjusts the wind parameters by the method of differential corrections. We have appled this method to the IUE observations of 32 Cygni. We have fitted a theoretical line profile to the IUE observations of Fe II resonance line at various phases. The mass-loss rate, wind velocity and stochastic velocity of 32 Cygni obtained in this paper are
, 132.14km/s, 39.82km/s, respectively.
ON THE FIFTH FORCE AND THE STRUCTURE OF NEUTRON STAR
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 115~130
In the framework of Thomas-Fermi equation, we have examined the properties of neutron star by assuming the existence of a new intermediate force which is composition dependent. We have found that the structure, size and mass of neutron star are affected by the strength and range of this new force. In the ultrarelativistic limit, we have also confirmed that Chandraseknar mass,
is determined by the constants of classical physical laws, which take part in the selfgravitating processes on neutron star as well as the constant of hypothetical fifth force. In the experimental limits of the fifth force, the changes of size and mass of a neutron star are in the order of strength parameter
CRE ECPERIMENT OF KITSAT-1
Journal of Astronomy and Space Sciences, volume 11, issue 1, 1994, Pages 131~145
The Cosmic Ray Experiment (CRE) is one of the modules flown on board the KITSAT-1 satellite and consistes of two sub-systems: the Total Dose Experiment (TDE) and the Cosmic Particl Experiment(CPE). The purpose of CRE is to characterize the space radiation environment as encountered by an Earth-orbiting spacecraft. KITSAT-1 orbit is dominated by the inner Van Allen radiation belt. This region has a large population of high energy protons which contributes significantly to both long-term and transient radiation effects. The data shows that the inner Van Allen radiation belt is very stable and the solar activity influences the CPE, TDE data and SEU(Single Event Upset) rates. The result also shows that much larger high energy particle flux is recorded than the predictions of the CREME code.