• International Union of Geodesy and Geophysics Korean Journal of Geophysical Research
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• v.26 no.1
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• pp.15-29
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• 1998

The numerical simulation of heavy precipitation event occurred in the central Korean Peninsula on July 26-28, 1996 was performed using the fine mesh model. ARPS (Advanced Regional Prediction System) developed by the CAPS (Center for Analysis and Prediction of Storms). Usually, the heavy rainfalls occurred at late July in the Korean Peninsula were difficult to predict, and showed very strong rainfall intensity. As results, they caused a great loss of life and property. As it usual, this case was unsuccessful to predict the location of rain band and the precipitation intensity with the coarse-mesh model. The same case was, however, simulated well with fine-mesh storm-scale model, ARPS. Moisture band at 850 hPa appeared along the Changma Front in the area of China through central Korea passed Yellow Sea. Also the low-level jet at 700 hPa existed in the Yellow Sea through central Korea and they together offered favorable condition to induce heavy rainfall in that area. The convective activities developed to a meso-scale convective system were observed at near the Yangtze River and moved to the central Korean Peninsula. Furthermore, the intrusion of warm and moist air, origninated from typhoon, into the Asia Continent might result in heavy rainfall formation through redistribution of moisture and heat. In the vertical circulation, the heavy rainfall was formed between the upper- and low-level jets, especially, the entrance region of the upper-level jet above the exit the region of the low-level jet. The low level convergence, the upper level divergence and the strong vertical wind were organized to the very north of the low level jet and concentrated on tens to hundreds km horizontal distance. These result represent the upper- and low-level jets are one of the most important reasons on the formation of heavy precipitation.

• Anxiety and mood
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• v.20 no.1
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• pp.8-16
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• 2024

Objective : The purpose of this study is to compare the signal obtained from the frontal 2-electrodes EEG with that obtained from the temporal, central, and parietal 2 electrodes. Methods : EEGs were recorded in a total of 67 patients with major depressive disorder (MDD), 104 patients with schizophrenia (SCZ), and 29 patients with Alzheimer's disease (AD). For each disease group, there were healthy controls (HC) that were paired accordingly (HC1=69, HC2=104, HC3=27). The following measurements were compared across electrodes: band power, alpha peak frequency (APF), APF power, alpha asymmetry (AA), and Kolmogorov complexity (KC). Results : Statistically significant differences were found in band power measured from frontal electrodes compared to electrodes placed in other locations. Specifically, the power of theta waves was measured higher in the temporal electorodes, alpha 1 and alpha 2 waves in the parietal, beta 1 and beta 2 in the central, and gamma waves in the temporal electrodes. Both SCZ and AD patients showed increased theta power in all electrodes. In SCZ patients, APF decreased in the central and temporal electrodes, but the APF power analysis showed no difference between the patients and controls. Additionally, AD patients exhibited increased AA in the central EEG, while SCZ patients showed decreased KC in the parietal and temporal electrodes. Conclusion : Depending on the electrode location, sensitive EEG frequencies differed. Compared with signals from other electrodes, frontal EEG in MDD patients revealed generally constant signal values, though the temporo-parieto-central electrodes appeared to be more reliable in SCZ and AD patients.

• Journal of the korean academy of Pediatric Dentistry
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• v.32 no.3
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• pp.525-530
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• 2005

Maxillary median diastema is the term used when there is spacing between maxillary central incisors. The space between maxillary central incisors are often observed during ugly duckling stage. In most of the cases, as maxillary permanent canines erupt, it gradually disappears. Maxillary median diastema needs to be treated when there is up to 2mm of space between the incisors even after eruption of permanent canines or when there is 3mm of space, at least, before the eruption of the canines. Particulary, for the latter case, orthodontic treatment is recommended because not only the esthetic point of view but also to regain the eruption space for maxillary lateral incisors and canines. The appliance used for orthodontic treatment are removable appliances, using finger spring and etc, and fixed appliances, using rubber elastics and coil spring. If rubber band alone was used to treat median diastema without any other appliance such as band, tube or bracket, it will gradually move downward along the root surface. Then it will destroy the peridontal ligament and causes tooth mobility, extrusion, and avulsion. This report presents cases of damaged tooth due to improper use of rubber band when treating maxillary median diastema.

• Publications of The Korean Astronomical Society
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• v.32 no.1
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• pp.73-75
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• 2017

Debris disks are important observational clues to understanding on-going planetary system formation. They are usually identified by significant mid-infrared excess on top of the photospheric emission of a central star on the basis of prediction from J-, H-, and Ks-band fluxes and the stellar model spectra. For bright stars, 2MASS near-infrared fluxes suffer large uncertainties due to the near-infrared camera saturation. Therefore we have performed follow-up observations with the IRSF 1.4 m near-infrared telescope located in South Africa to obtain accurate J-, H-, and Ks-band fluxes of the central stars. Among 754 main-sequence stars which are detected in the AKARI $18{\mu}m$ band, we have performed photometry for 325 stars with IRSF. As a result, we have successfully improved the flux accuracy of the central stars from 9.2 % to 0.5 % on average. Using this dataset, we have detected $18{\mu}m$ excess emission from 57 stars in our samples with a $3{\sigma}$ level. We find that some of them have high ratios of the excess to the photospheric emission even around very old stars, which cannot be explained by the current planet-formation theories.

• Clinics in Shoulder and Elbow
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• v.24 no.4
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• pp.253-260
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• 2021

Background: To suggest a reasonable isometric point based on the anatomical consistency of interosseous membrane (IOM) attachment in association with topographic characteristics of the interosseous crests, the footprints of the central band (CB) of the IOM on the radial and ulnar interosseous crests (RIC and UIC) were measured. Methods: We measured the distance from the CB footprints from each apex of both interosseous crests in 14 cadavers and the angles between the forearm axis of rotation (AOR) and the distal slopes of the RIC and UIC in 33 volunteers. Results: The CB footprints lay on the downslope of both interosseous crests with its upper margin on average 3-mm proximal from the RIC's apex consistently in the radial length, showing normality (p>0.05), and on average 16-mm distal from the UIC's apex on the ulna without satisfying normality (p<0.05). The average angle between the UIC's distal slope and the AOR was 1.3°, and the RIC's distal slope to the AOR was 14.0°, satisfying the normality tests (p>0.05), and there was no side-to-side difference in both forearms (p<0.05). Conclusions: The CB attached to the downslope just distal to the RIC's apex constrains the radius to the UIC that coincides with the AOR of the forearm circumduction, maintaining itself both isometrically and isotonically.

• The Korean Journal of Zoology
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• v.30 no.3
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• pp.261-271
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• 1987

계배 중추신경계의 분화에 따른 단백질 합성 양상을 SDS-PAGE와 2차원 전기영동으로 분석하였다. 약 24∼26개의 band가 densitomete떼 의해 기록되었고, 주요 band들의 분자량은 90K에서 lIft 범위에 분포하였다. 대뇌, 시엽 및 소뇌에서 가장 현저한 band는 분자량이 44.7K로 actin으로 사료되었다. 대뇌의 85.5광 및 47.9K, 시엽의 85.5K, 71.6K 및 34.9K 소뇌의 47.9K 및 34.9K band들은 부화전까지 는 증가하다가 부화후 감소하였다. 기록된 약 300개의 polypeptide중 약 9%가 분화가 진행됨에 따라 그들의 합성율에 변화를 보였으며, 대뇌의 spot 19(Mr, 63K; pl, 6.95)와 소뇌의 spot 22(Mr, 43K; pI, 6.5) 는 부화후 4일배에서 새로이 합성되었다.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.2
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• pp.43.1-43.1
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• 2018

Young pulsar wind nebulae, powered by energetic central pulsars, are often observed as bright extended sources in the X-ray band. They are believed to accelerate electrons and positrons to very high energy and can possibly explain the positron excess observed by Fermi and AMS. The electron distribution in these PWNe can be best studied by X-ray satellites because emission in the X-ray band is produced by direct synchrotron radiation of the electrons and positrons. We present NuSTAR studies of PWNe and discuss the implication. Future studies to help further our understanding of particle acceleration will be briefly discussed.

• The Korean Journal of Food And Nutrition
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• v.36 no.3
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• pp.202-208
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• 2023

FT-IR, GC/MS, and ATR-FT-IR analyses were performed to confirm the physicochemical characteristics of saw palmetto fruit (SPF) extract. FT-IR analysis of the standard product showed that the band corresponding to the carbonyl bond of free fatty acid was stronger than the band of acyl-glyceride. Sample E was identified as having the same trend as the standard sample. Fatty acid composition analysis revealed that the main fatty acids in the standard sample were lauric acid and oleic acid. The content of lauric acid ranged from approximately 30% to 38% in samples B, C, D, and E, while the content of oleic acid ranged from approximately 29% to 34%. The GC/MS analysis confirmed that the standard SPF extract consisted of fatty acids and fatty acid ethyl esters. Sample E demonstrated a similar pattern to the standard samples in terms of oleic acid, lauric acid, and fatty acid esters. ATR-FT-IR analysis indicated that only sample E was predicted to contain 100% saw palmetto extract. Therefore, these study findings can be considered fundamental data for analyzing the physicochemical characteristics of the composition of SPF extract.

• Journal of The Korean Astronomical Society
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• v.52 no.6
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• pp.235-244
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• 2019

We present the results of near-infrared imaging observations of the galaxy overdensity around the z = 1.44 radio-loud active galactic nucleus (AGN) 6CE1100+3505, which was carried out with the purpose of sampling the redshifted Hα emission from the actively star-forming galaxies that could constitute the overdensity. The existence of the structure around this AGN was spectroscopically confirmed by previous grism observations which are however limited to the central region. Using the CH4Off narrow/medium-band and H broad band filters in the Wide Infrared Camera (WIRCam) on the Canada-France-Hawaii Telescope (CFHT), we constructed a sample of objects that show a flux excess in the CH4Off band due to line emission. The emission line flux is ~ 4.9 × 10^-16 erg s^-1 cm^-2, corresponding to a star formation rate (SFR) of ~ 50 M_⊙ yr^-1 for galaxies at redshifts z ~ 1.4. None of the galaxies with medium-band flux excess is located within 1 Mpc from the central AGN, and there is no evidence that the selected galaxies are associated with the proposed cluster. Along with the star formation quenching near the center that was found from the previous grism observations, the lack of extreme starbursts in the structure suggests that at z ~ 1.4, overdense regions are no longer favorable locations for vigorous star formation.

• Journal of the Korean Society of Tobacco Science
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• v.28 no.2
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• pp.94-99
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• 2006

AFLP(Amplified Fragment Length Polymorphism) analysis was conducted to cultivars of tobacco, Nicotiana tabacum in order to select the cultivar-specific markers. AFLP results using 12 primer sets revealed genetic diversity among 12 field grown tobacco cultivars. Polymorphic fragments amplified by PCR was purified and cloned to identify their nucleotide sequences. From the sequences of them, 40 primer sets were designed to select cultivar-specific markers. When genomic DNA isolated from tobacco were used as PCR template, a set of primers, BrSF/BrSR showed Burley-specific band patterns. The results indicate that AFLP technique used in this experiments is useful for identifying tobacco cultivars in a rapid manner.