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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 12, Issue 2 - Dec 1995
Volume 12, Issue 1 - Jun 1995
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MODEL DUST ENVELOPES FOR ASYMPTOTIC GIANT BRANCH STARS. I. OH/IR STARS
Suh, Kyung-Won ;
Journal of Astronomy and Space Sciences, volume 12, issue 2, 1995, Pages 157~167
OH/IR stars are the most massive and youngest subclass in asymptotic giant branch stars which pass through sporadic superwind phases. We have modeled the dust envelopes around OH/IR stars with close attention to the evolution of the structure of the dust shells. We use various dust density distributions to take account the effect of the superwind due to the helium shell flash by adding a density increased region. Depending on the position and quality of the density increased region, the model results are different from the results with conventional density distribution. The new results fit the observations of some OH/IR stars better. Especially, the OH/IR stars with excessive 30-100
m emission can be better explained by the new results. The IR two-color diagrams comparing the results of the superwind models and IRAS observation of 95 OH/IR stars have been made. The new results can explain much wider regions on the IR two-color diagrams.
MODEL DUST ENVELOPES FOR ASYMPTOTIC GIANT BRANCH STARS. II. CARBON STARS
Suh, Kyung-Won ; Kwoun, Hee-Joung ;
Journal of Astronomy and Space Sciences, volume 12, issue 2, 1995, Pages 168~178
We have modeled the dust envelopes around carbon stars with close attention to the evolution of the structure of the dust shells. We use various dust density distributions to take account the effect of the superwind due to the helium shell flash by adding a density increased region. Depending on the position and quality of the density increased region, the model results are different from the results with conventional density distribution. The new results fit the observations of some carbon stars better. The IR two-color diagrams comparing the results of the super wind models and IRAS observation of 252 carbon stars have been made. The new results can explain much wider regions on the IR two-color diagrams.
PERIOD VARIATIONS OF RT PERSEI
Kim, Chun-Hwey ;
Journal of Astronomy and Space Sciences, volume 12, issue 2, 1995, Pages 179~195
RT Per has been known as a close binary of which the orbital period has unpredictably varied so far. Although there are no agreements with the working mechanism for the changes of the period, two interpretations have been suggested and waiting for to be tested: 1) light-time effects due to the unseen 3rd and 4rd bodies (Panchatsaram 1981), 2) Abrupt period-changes, due to internal variations of the system (e.g. mass transfer or mass loss) superimposing to the light-time effect by a 3rd body (Frieboes-Conde & Herczeg 1973). In the point of view that the former interprepation models could predict the behavior of the changes of the orbital period theoretically, we checked whether the recent observed times of minimum lights follow the perdictions by the first model or not. We confirmed that the observed times of minimum lights have followed the variations calculated by the light-times effects due to the 3rd and 4rd bodies suggested by Panchatsatam. In this paper a total of 626 times of minimum lights were reanalyzed in terms of the light-time effects by the 3rd and 4rd bodies. We concluded that the eclipsing pair in SVCam system moves in an elliptic orbit about center of mass of the triple system with a period of about
, while the mass center of the triplet is in light-time orbit about the center of mass of the quadruple system with a period of
. The mean masses deduced for the 3rd and 4rd bodies were
LIGHT CURVE ANALYSIS OF A SHORT PERIOD ECLIPSING BINARY SW LYNCIS
Journal of Astronomy and Space Sciences, volume 12, issue 2, 1995, Pages 196~203
The UBV light curves of a close eclipsing binary SW Lyn were obtained with the observations made at the Sobaeksan Astronomy Observatory during 7 nights from September 1983 to March 1987. These light curves show asymmetry to the secondary minimum light and the asymmetry is larger at the shorter wavelength light curve. Assuming that the star sport makes the asymmetry, we employed the WD code to make the B and V light curves solution. We confirmed that SW Lyu has near contact(semi-detached) Roche configuration and has the Case A evolution.
STUDY OF THE EVOLUTION OF SL-9 IMPACT SITES ON JUPITER WITH THE KYUNGHEE UNIVERSITY 30 INCH TELESCOPE
Journal of Astronomy and Space Sciences, volume 12, issue 2, 1995, Pages 204~215
We observed SL-9 impact sites on Jupiter with a CCD and a R filter on the KyungHee University 30-inch telescope between July 17 and September 3, 1994. We identified impact sites of A, C, E, G, H, K, L, Q1, W and G-group, We calculated the moving velocity relative to System II and rotation period of the G, L sites to be from -8.0 to 8.8m/s, and
, respectively. The diameters of G and L sites in our first observation were
, respectively. In particular, we investigated the evolution of the impact sites by calculating the diffusing rates of the impact clouds.
THE ELECTROMAGNETIC CHARACTERISTICS OF THE POLAR IONOSPHERE DURING A MODERATELY DISTURBED PERIOD
Journal of Astronomy and Space Sciences, volume 12, issue 2, 1995, Pages 216~233
The distributions of the ionospheric conductivities, electric potential, ionospheric currents, field-aligned currents, Joule heating rate, and particle energy input rate by auroral electrons along with the characteristics of auroral particle spectrum are examined during moderately disturbed period by using the computer code developed by Kamide et al. (1981) and the ionospheric conductivity model developed by Ahn et al. (1995). Since the ground magnetic disturbance data are obtained from a single meridian chain of magnetometers (Alaska meridian chain) for an extended period of time (March 9 - April 27, 1978), they are expected to present the average picture of the electrodynamics over the entire polar ionosphere. A number of global features noted in this study are as follows: (1) The electric potential distribution is characterized by the so-called two cell convection pattern with the positive potential cell in the morning sector extending into the evening sector. (2) The auroral electrojet system is well developed during this time period with the signatures of DP-1 and DP-2 current systems being clearly discernable. It is also noted that the electric field seems to play a more important role than the ionospheric conductivity the conductivity over the poleward half of the westward electrojet in the morning sector while the conductivity enhancement seems to be more important over its equatorward half. (3) The global field-aligned current distribution pattern is quite comparable with the statistical result obtained by Iijima and Potemra (1976). However, the current density of Region 1 is much higher than that of Region 2 current at pointed out by pervious studies (e.g.; Kamide 1988). (4) The Joule heating occurs over a couple of island-like areas, one along the poleward side of the westward electrojet region in the afternoon sector. (5) The maximum average energy of precipitating electrons is found to be in the morning sector (07∼08 MLT) while the maximum energy flux is registered in the postmidnight sector (02 MLT). Thus auroral brightening and enhancement of ionospheric conductivity during disturbed period seem to be more closely associated with enhancement of particle flux rather than hardening of particle energy.
CHARACTERISTICS OF THE CONTAMINATED LANGMUIR PROBE
Journal of Astronomy and Space Sciences, volume 12, issue 2, 1995, Pages 234~243
Korea's third rocket, which is currently under development for launch in 1997, is expected to reach as high as 160km and thus, it will provide a good opportunity for the direct measurement of the plasmas in the E-region ionosphere of the Korean peninsula. Langmuir probe techniques, which are the basic tools of the plasma experiment, may yield inaccurate results if they are applied in the conventional form as they are used in the laboratory experiments because of the contamination. In the present paper we study the contamination problem by performing the ground experiments in the vacuum chamber using the contaminated probe. The result show that the contamination effect is reduced when the plasma density is low or when the frequency of the sweep voltage is fast. We propose a modified Langmuir probe based upon our experiments which is suitable for the rocket experiments.
THE SELECTION OF ALTITUDE AND INCLINATION FOR REMOTE SENSING SATELLITES
Journal of Astronomy and Space Sciences, volume 12, issue 2, 1995, Pages 244~255
The success of a satellites mission is largely depended upon the choice of an appropriate orbit. In the case of a remote sensing satellite which observes the Earth, there exits an optimum solar elevation angle depending on the mission. Therefore a sun-synchronous orbit is suitable for a remote sensing mission. The second-order theory for secular perturbation due to non-symmetric geopotential was described. To design a sun-synchronous orbit, a constraint condition on regression of node was derived. A algorithm to determine the altitude and the inclination was introduced using this constraint condition. As practical examples, the altitudes and the inclinations of four remote sensing satellites were calculated. The ground tracks obtained by the orbit propagator were used to verify the resulting sun-synchronous orbital elements.
PROTOTYPE DEVELOPMENT OF THE STAR SENSOR FOR THE KITSAT-3
Journal of Astronomy and Space Sciences, volume 12, issue 2, 1995, Pages 256~264
This report presents the development procedure and the results of a prototype star sensor which can be used as one of the attitude sensors of the KITSAT-3. The star sensor is a major attitude sensor that can determine the 3-axis attitude information, by comparing between star corrdinates in the star catalog and the measured corrdinates. The 2 dimensional CCD camera is used for measuring the star corrdinates and the DSP(Digital Signal Processor) technology is applied to the image and signal processing. Using the prototype star sensor with thermoelectri cooling technique, we have succesfully obtained the star images around 4th magnitude at Sobaeksan Astronomy Observatory minimizing night sky effect.
MONTE CARLO ANALYSIS FOR STATION ACQUISITION ERROR CORRECTION OF SATELLITE
Journal of Astronomy and Space Sciences, volume 12, issue 2, 1995, Pages 265~274
The purpose of perigee kick motor firing is to place a satellite into transfer orbit and that of apogee kick motor firing is to place the satellite into geosynchonous orbit in order to increase the semi-major axis of the transfer orbit and reduce the inclination of the transfer orbit. Because apogee motor firing is always accompanied with injection errors, the satellite is not placed into geosynchonous orbit but into a near-geosynchonous orbit, also knows as a drift orbit. Thus, the orbital maneuver to correct drift orbit into gteosynchonous orbit is required, this maneuver is called the station acquisition. For reduction of expenditure and performance of mission, we estimate
V budget and required fuel allowance for station acquisition. As the uncertainty of drift orbit by injection error of perigee and apogee kick motor firing prevents us from obtaining exact
V budget, statistical Monte Carlo simulation technique is used in order to get optimal
V budget and required fuel allowance with a probability of 99%. With respect to Korea satellite launched by Delta-2 launch vehicle in 1995, Monte Carlo analysis is used in order to get various orbital parameters,
V budget and required fuel allowance for station acquisition with a probability of 99%.