• Journal of the Institute of Electronics and Information Engineers
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• v.54 no.3
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• pp.78-86
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• 2017

In this paper, we propose hidden object detection system using parametric array based on acoustic signal that is harmless to human body. A transmit signal of the proposed detection system uses a high directive chirp signal generated from parametric array phenomenon, which uses technique to improve a signal to noise (SNR) of a received signal and a distance resolution trough the dechirp processing. The transmit sensor array is constructed as $8{\times}2$ and has a horizontal beam width of $7^{\circ}$ and vertical beam width of $26^{\circ}$. To verify the detection and visualization of the proposed system, a 2-axis driving control system based on linear stage was constructed, and A-scan, B-scan, and C-scan experiments was addressed for hidden object. From experimental results, we detected and visualized the hidden bronze plate and pipe by cloth and the visualized shapes was confirmed. Especially, the obtained errors was $0.015m^2$ for bronze plate, and $0.046m^2$ for pipe.

• Journal of radiological science and technology
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• v.34 no.1
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• pp.43-50
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• 2011

In this study we modeled the varian 2100C/D linear accelerator head and multi-leaf collimator by simulation with the GEANT4 Monte Carlo toolkit. Then central axis percentage depth dose profiles and lateral dose profiles within homogeneous water phantom($50{\times}50{\times}50\;cm^3$) were evaluated with 6 MV photon beam. The simulations were performed in two stages. In the first stage, photon energy spectrum at the target were computed were computed. Then spectra data was directly irradiated in the water phantom using sampling techniques. The simulation data were compared with experimental data to evaluate the accuracy of the model. Results showed that two data were matched within 2% error boundary. The proposed method will be applied for simulation of dose calculation and dose distribution study.

• The Korean Journal of Pain
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• v.12 no.1
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• pp.27-35
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• 1999

Background: Fibromyalgia is a common syndrome of musculoskeletal pain and fatigue. Lacking distinctive histological or laboratory abnormality in diagnosis, it has often been considered a form of "psychogenic rheumatism". Fibromyalgia causes much distress to the affected patients and often frustrates physicians, who are unable to start rational therapy on any logical disease pathology. Methods: Growth hormone is essential for muscular homeostasis. In the present study, the notion that the stage-4 sleep anomaly typically seen in the fibromyalgia syndrome may disrupt growth hormone secretion was tested. Because growth hormone has a very short half-life, serum levels of somatomedin C were measured; somatomedin C is the major mediator of growth hormone's anabolic actions and is a prerequisite for normal muscle homeostasis. Serum levels of somatomedin C using acid-extraction procedure and two-site immunoradiome-tric assay (IRMA) and number of tender points were measured in 27 female patients with fibromyalgia from 40 to 60 years old and 27 healthy controls. Results: There were no differences in the concentration of somatomedin C between fibromyalgia patients and controls ($mean{\pm}SD$: $178.3{\pm}75.5$ ng/ml versus $166.3{\pm}76.6$ ng/ml; p=0.55). And there were no correlations between number of tender point and serum somatomedin C level by linear regression analysis. Conclusions: These findings did not support that there is a distinctive disruption of the growth hormone-somatomedin C neuroendocrine axis in a fibromyalgia syndrome. But we can not discard the hypothesis that disturbed sleep predispose to muscle pain.

• Korean Journal of Psychosomatic Medicine
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• v.6 no.2
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• pp.155-175
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• 1998

The purpose of this study was to test a reliability and validity of the Korean version of Eating Attitudes Test-26(KEAT-26). Using multi-stage sampling, we finally got 3,496 subjects(1422 males and 2074 females) who were available for analysis from target 4,400 Korean adults over 18 in the nationwide areas of9 kus, 10 middle or small cities, and 17 kuns. We tried to make T score norm of the KEAT-26 as a cutoff score and STEN score norm as a index of severity for disordered eating behaviors. For the male group, Cronhach's internal consistency was .83 and Spearman-Brown split half correlation coefficiency was .75. For the female group, each of them was .81 and .75, and .81, .75 for the grand total group respectively. Validity test was performed by construct validation analysis. By a iterated principal axis factoring, 4 factors were extracted. There were some differences in the factors of the KEAT-26 by sex. In the male group, factor I was 'self-control of eating and bulimic symptom', factor II was 'food preoccupation and dieting', factor III was 'preoccupation with being thinner', factor N was 'avoidance of sweet foods'. In contrast with the male group, factor I was 'self-control of eating and bulimic symptom', factor II was 'preoccupation with being thinner', factor III was 'food preoccupation' and factor N was 'dieting' in the female group. We used T score 65 as a cutoff score. T score 65 corresponded to raw score 19 in the male group, 22 in the female group and 21 in the grand total group. Severity of disordered eating behaviors was measured by a STEN score. In the male group, each of the score range of 0-10, 11-14, 15-18, 19-22 and over 23 represented the degree of none, subclinical, manifest, moderate and severe severity respectively. Each of the score range of 0-13, 14-17, 18-21, 22-26 and over 27 in the female group, and the score range of 0-12, 13-16, 17-20, 21-25 and over 26 in the grand total group also represented the same degree of severity as like in the male group. These results support that KEAT-26 is a reliable and valid scale for evaluating disordered eating behaviors and eating problems.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.2
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• pp.102-102
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• 2014

The NISS (Near-infrared Imaging Spectrometer for Star formation history) onboard NEXTSat-1 is the near-infrared instrument onboard NEXTSat-1 which is being developed by KASI. The main scientific targets are nearby galaxies, galaxy clusters, star-forming regions and low background regions in order to study the cosmic star formation history in local and distant universe. After the Preliminary Design Review, we have fixed major specifications of the NISS. The off-axis optical design with 15cm apertureis optimized to obtain a wide field of view ($2deg.{\times}2deg.$), while minimizing the sensitivity loss. The opto-mechanical structure of the NISS was designed to be safe enough to endure in the launching condition as well as the space environment. The tolerance analysis was performed to cover the wide wavelength range from 0.95 to $3.8{\mu}m$ and to reduce the degradation of optical performance due to thermal variation at the target temperature, 200K. The $1k{\times}1k$ infrared sensor is operated in the dewar at 80K stage. We confirmed that the NISS can be cooled down to below 200K in the nominal orbit through a radiative cooling. Here, we report the preliminary design of the NISS.

• Journal of The Korean Astronomical Society
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• v.51 no.1
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• pp.17-25
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• 2018

Detecting exoplanets around giant stars sheds light on the later-stage evolution of planetary systems. We observed the M giant HD 18438 and the K giant HD 158996 as part of a Search for Exoplanets around Northern circumpolar Stars (SENS) and obtained 38 and 24 spectra from 2010 to 2017 using the high-resolution Bohyunsan Observatory Echelle Spectrograph (BOES) at the 1.8m telescope of Bohyunsan Optical Astronomy Observatory in Korea. We obtained precise RV measurements from the spectra and found long-period radial velocity (RV) variations with period 719.0 days for HD 18438 and 820.2 days for HD 158996. We checked the chromospheric activities using Ca $\text\tiny{II}$ H and $H{\alpha}$ lines, HIPPARCOS photometry and line bisectors to identify the origin of the observed RV variations. In the case of HD 18438, we conclude that the observed RV variations with period 719.0 days are likely to be caused by the pulsations because the periods of HIPPARCOS photometric and $H{\alpha}$ EW variations for HD 18438 are similar to that of RV variations in Lomb-Scargle periodogram, and there are no correlations between bisectors and RV measurements. In the case of HD 158996, on the other hand, we did not find any similarity in the respective periodograms nor any correlation between RV variations and line bisector variations. In addition, the probability that the real rotational period can be as longer than the RV period for HD 158996 is only about 4.3%. Thus we conclude that observed RV variations with a period of 820.2 days of HD 158996 are caused by a planetary companion, which has the minimum mass of 14.0 $M_{Jup}$, the semi-major axis of 2.1 AU, and eccentricity of 0.13 assuming the stellar mass of $1.8 M_{\odot}$. HD 158996 is so far one of the brightest and largest stars to harbor an exoplanet candidate.

• Journal of the Korea institute for structural maintenance and inspection
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• v.22 no.1
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• pp.147-157
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• 2018

The basis of capacity design has been explicitly or implicitly regulated in most bridge design specifications. It is to guarantee ductile failure of entire bridge system by preventing brittle failure of pier members and any other structural members until the columns provides fully enough plastic rotation capacity. Brittle shear is regarded as a mode of failure that should be avoided in reinforced concrete bridge pier design. To provide ductility behavior of column, the one of important factors is that flexural hinge of column must be detailed to ensure adequate and dependable shear strength and deformation capacity. Eight small scale circular reinforced concrete columns were tested under cyclic lateral load with 4.5 aspect ratio. The test variables are longitudinal steel ratio, transverse steel ratio, and axial load ratio. Eight flexurally dominated columns were tested. In all specimens, initial flexural-shear cracks occurred at 1.5% drift ratio. The multiple flexural-shear crack width and length gradually increased until the final stage. The angles of the major inclined cracks measured from the vertical column axis ranged between 42 and 48 degrees. In particular, this study focused on assessing transverse reinforcement contribution to the column shear strength. Transverse reinforcement contribution measured during test. Each three components of transverse reinforcement contribution, axial force contribution and concrete contribution were investigated and compared. It was assessed that the concrete stresses of all specimen were larger than stress limit of Korea Bridge Design Specifications.

• Journal of architectural history
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• v.28 no.2
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• pp.77-90
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• 2019

The Sacheonwangsa temple in Silla was completed in 679, just after the unification of the Three Kingdoms. In recent years, we have been critically considering the history of the chronology based on the existence of 'Geumdang of the previous generation', which has emerged through the research report of the Sacheonwangsa temple. It is the one to reconsider the construction process of the Sacheonwangsa temple centering on the re-interpretation of the construction time and the character of the first stage of the foundation which was confirmed from within the Geumdang site. The results of this study are as follows : 1)The "Chang(創) of Sacheonwangsa temple" in [Three Affairs that Queen Seondeok had already known] that it is presumed that the construction of the Sacheonwangsa temple, which was designed by Anham before 640 years ago, will convey the fact that the first of the King Munmu's reign (661 ~) has been finalized after the initial discussion. 2)Although the theories after excavations are predicated on the existence of 'Geumdang of the previous generation', there is no reason to believe that a lasting predecessor building with roof and pillar walls on predecessor buildings is considered to have been built. The foundation was associated with the "build a temple out of coloured silk(以彩帛營寺)" i.e. 'Jochang(祖創)' in 670 years before the construction plan was formally finalized. However, it is presumed that the remains of the platform construction on the premise that it will be used on the construction of Geumdang. 3)The decision to 'rebuilding( ??)' based on a formal construction plan is determined to be from 670 to 672 years. The maintaining of the original cathedral axis line, to the north on the boundary of the southern limit of the foundation flat portion, the result of developing and embodied the relative position of the Geumdang in the newly determined cathedral unfold and embody, the center of the building base and Geumdang, it is presumed that the centers of them are divided into North and south. 4)The completion of the Sacheonwangsa temple in 679 is understood as the conclusion of 'rebuilding' to "build a temple out of coloured silk" i.e. 'Jochang' in 670 years. The pent roof of the Geumdang was initially considered not to be in the plan, but it is judged to be before the completion of the Sacheonwangsa temple.

• Journal of The Korean Astronomical Society
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• v.24 no.2
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• pp.217-271
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• 1991

We have observed dense core around young stellar objects, DR21, S140, Orion-KL, and L1551 using four millimeter-wave transitions of $HC_3N\;J$=4-3, J=5-4, J=10-9, and J=12-11. The spatial distribution of $HC_3N$ emission closely resembles the morphology of the previous CS observations that trace high density gas. These observations reveal the existence of $HC_3N$ dense cores around central IR source, elliptical in shape and almost perpendicular to the CO bipolar outflow axis. Small differences can be explained by that $HC_3N$ molecular line is more optically thin and is seen to be more detailed structure in the neighborhood of central IR sources. In S140 and Orion-KL, massive(${\sim}10\;M_{\odot}$), slowly rotating dense cores lie near at the central IR sources of bipolar outflows. The velocity channel maps of DR21 show that the bipolar outflow gas may have a correlation with the dense core of DR21. We analyzed intensities of the four lines to derive physical conditions in dense core from two methods, LTE and LVG. The column density of $HC_3N$, $N(HC_3N)$, between LTE and LVG calculations agree well with each other. The abundances of $HC_3N$ in each observing source have been estimated using the average values of $n(H_2)$ and $N(HC_3N)$ and assuming the size of dense core. The fractional $HC_3N$ abundances in massive dense cores of DR21, S140, and Orion-KL have a range of $(2-7){\times}10^{-10}$, while that of low mass dense core, L1551, has one order of magnitude greater value of $2{\times}10^{-9}$. This should be considered good agreement with the result by Morris et al.(1976). It may be considered that dense cores of DR21, S140, and Orion-KL may have almost same stage of chemical evolution, and their abundances have a small values relative to that of L1551. The column density $N(HC_3N)$ decreases with increasing distance from the densest part of the cloud, the central infrared source, and have the relation of $N(HC_3N){\varpropto}R^{\alpha}$, where a has a range of 0.65 to 0.89. The values of $n(H_2)$ are not varied with increasing distance from the dense core, and have almost same values. Therefore, it is considered that the dense cores in these regions probably consist of dense clumps in diffuse molecular gas medium, and $n(H_2)$ of each clump is ${\sim}10^5\;cm^{-3}$. Levels in the $T_{ex}$ increases with $n(H_2)$. It is considered that the $HC_3N$ dense cores are not completely thermalized. We examine the relationships between the luminosity of central infrared sources versus mass of the dense cores, and the luminosity of central infrared sources versus molecular hydrogen column density. Luminosities of the central IR sources show good correlation with mass and hydrogen column density of the dense core. Same has been found from CS observations. However, mass and size derived from $HC_3N$ observations are one order of magnitude smaller than those from CS. It can be interpreted that we see more central part of the cloud cores in $NC_3N$ lines than CS lines.

• Korean Journal of Ichthyology
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• v.2 no.1
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• pp.53-62
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• 1990

Morphological development from egg to juvenile stages of the trident goby, Tridentigertrigonocephalu5 were observed in the laboratory at Pusan, Korea. The ripe eggs were spherical in shape, measuring 0.49-0.62 mm in diameter. The eggs became ellipsoid shape after the insemination and measured about 1.40-1.58 mm on the long axis. Hatching began about 158 hours after insemination at water temperature of $20.5-24^{\circ}C$. The newly hatched larvae were 2.88-3.14 mm in total length(TL), with 27-28(10+ 17-18) myomeres. Many melanophore and guanophores are distributed on eye cups, gas bladder, optic vesicle, intestine and the caudal region. Three days after hatching the yolk and oil-globule was completely absorbed and the larvae attained a total length 3.26-3.62 mm. The larvae swam actively in the aquarium and fed on the rotifer. Ten days after hatching, the larvae averaged 5.20 mm in TL and the caudal notochord flexed at $45^{\circ}$. Twenty days after hatching, the larvae averaged 7.47 mm in TL and rudimental anal, second dorsal, caudal and pectoral fins were formed. The larvae attained 12.05-12.65 mm in TL thirty five days after hatching and are found to transit the bottom-life, and first dorsal and ventral fins are completely formed. The larvae reached the juvenile stage at 45-50 days after hatching and attained 15.85-16.95 mm in TL, and all scales appeared on the body.