• 대한소아치과학회지
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• 제42권1호
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• pp.22-29
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• 2015

본 연구는 최근 12년간 하악 소구치에 발생한 함치성 낭을 가진 환자에 대하여 조대술을 시행한 후 해당 치아의 맹출 양상과 이에 영향을 미칠 수 있는 매복치의 깊이, 경사도, 매복치 치근의 발달 정도 등과의 관계를 평가하였다. 조대술을 시행 한 후 93%의 하악 소구치가 자발적으로 맹출 했으며, 낭종에 이환된 소구치는 이환되지 않은 대조군보다 조대술 후 더 빠르게 맹출 되었고 각도 변화도 더 크게 나타났다(p < 0.05). 이환된 소구치의 치근 발육정도가 낮을수록 맹출 속도가 빠르게 나타났고(p < 0.05), 치축각 변화량은 커지는 경향을 보였으나 통계학적으로 유의하지 않았다(p > 0.05). 대부분의 경우 맹출 속도와 치축각의 변화는 조대술 후 6개월 이내에 나타났다. 이 연구의 결과를 통해 함치성 낭에 이환된 치아의 조대술 후 자발적인 맹출 유도양상에 대한 정보를 제공하여 적절한 진단을 통해 바람직한 치료계획을 수립하는데 도움을 줄 것이다.

• 천문학회보
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• 제39권1호
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• pp.74.2-74.2
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• 2014

We have presented a classic two-ribbon filament eruption occurred in the east side of NOAA active region 11850 at 21:00 UT on 29 September 2013. Interestingly, this filament eruption was not accompanied by any flares and just there was a slight brightening in X-rays, C1.2, associated with the eruption. An accompanying huge CME was appeared at 22:12 UT in the LASCO C2 field of view and it propagates into the interplanetary space with a speed of about 440 km/s. And the related solar proton event (S2) started at 05:05 UT and peaked at 20:05 UT on 30 September 2013. The CME arrival was recorded by the ACE spacecraft around 01:30 UT on 2 October 2013. Around the CME arrival time, the solar-wind speed reached at about 640 km/s and IMF Bz showed southward component (-27 nT). Finally, the filament eruption and the CME cause geomagnetic storm (G2) at 03:00 UT on 2 October 2013. We described the detailed evolution of the filament eruption and its related phenomena such as CME, proton event, geomegnetic storm and so on. In addition, we will discuss about the activation mechanism of the filament eruption without flares.

• 천문학회보
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• 제38권2호
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• pp.90.2-90.2
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• 2013

Filament eruptions are one of the energetic phenomena on the solar surface with flares and coronal mass ejections (CMEs). We observed the whole process of filament eruption that occurred in AR 11305 in association with a C5.6 flare on 2011 September 29th using the Fast Imaging Solar Spectrograph (FISS) and the Solar Dynamics Observatory (SDO). The eruption consists of a slow phase with a transverse speed of ~10 km $s^{-1}$ in 16 minutes and a fast phase with a transverse speed of ~200 km $s^{-1}$ in 3 minutes. Near the beginning of slow phase eruption, preflare brightening occurred beneath the filament in $H{\alpha}$ and some EUV images. The preflare brightening region is associated with a blue-shifted $H{\alpha}$ feature with a speed of ~60 km $s^{-1}$. It appears that this is the outflow from magnetic reconnection which may have occurred at relatively low atmosphere. Our result support the notion that the preflare brightening is a process of magnetic reconnection playing an important role in triggering the filament eruption by deformative the magnetic field lines under the eruptive filament.

• 대한소아치과학회지
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• 제30권3호
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• pp.373-384
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• 2003

사춘기 전 아동에서 흔히 발생되는 함치성 낭을 조대술로 치료한 후 낭에 이환된 치아의 맹출에 영향 미치는 제반요인을 분석하여 이환된 치아의 외과적 또는 교정적 치료 유무의 기준을 마련하고자 본 연구를 시행하였다. 하악 소구치 부위가 함치성 낭으로 이환되어 있으며 조대술 실시 후 8개월 이내에 촬영된 파노라마 관찰사진이 있는 5-12세 아동 총 22명의 증례를 대상으로 하였다. 초진과 재진 시의 관찰기간 동안에 촬영 한 파노라마 사진으로 트레이싱 용지에 필요한 구조물과 치아를 모두 그렸으며 사진 상의 수직, 수평적인 상의 확대 및 축소의 보상을 위하여 초진사진의 제1대구치 치관크기를 기준으로 모든 사진을 표준화시켰다. 각 사진 상에서 낭에 이환된 부위를 실험군, 동일 악궁의 반대측 부위를 대조군으로 설정하여 교두깊이, 각의 크기, 낭의 크기, 교두점 위치지수를 계측하여 측정값을 얻은 후, 각 치아의 발육단계, 이환치아의 경사도, 위치의 변위율, 낭종의 면적 감소량과 치아의 맹출과의 관계를 분석하고자 맹출 속도, 각의 변화율, 낭면적의 감소율, 실험군 내의 조대술 후의 평균 기간(month)을 산정하여 다음의 결론을 얻었다. 낭에 이환된 부위의 영구치의 맹출 속도는 비이환측에 비해 평균 3.5배 빨랐으며 치축의 변화는 평균 $2.7^{\circ}/month$였다. 치근의 성장 단계에 따른 변화에서는 치근의 성장단계가 낮을수록 더욱 빠른 맹출 성향을 보였으며 각의 변화에서도 치근의 성장이 1/4이하 군에서 현저히 높게 나타났으며 낭종내 이환치의 변위에 따른 변화에서는 교두점 위치지수 차이가 30%될 때까지는 맹출 속도가 증가하다가 그 이상에서는 다시 감소하는 경향을 보였다. 낭의 면적 감소율이 $80mm^2/month$이상 감소하는 경우 현저하게 높은 맹출 속도를 보였고 이환된 치아가 근심 변위한 경우 원심 변위한 치아보다 맹출 속도는 낮았지만 각의 변화율은 크게 나타났다. 이환된 치아의 각도 변위가 작을수록 맹출의 속도는 증가하였으며 $15^{\circ}$ 이하의 경우 각도 변화도 높게 나타났다. 조대술 후 대부분의 경우 급격한 맹출 속도와 치축 각의 변화는 6개월 이내에 일어났다.

• 문화기술의 융합
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• 제8권3호
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• pp.493-499
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• 2022

본 논문은 제주도의 화산이 폭발 시에 얼마만한 속도로 폭발했으며, 폭발 후에 생기는 튜물러스와 한라산 중턱에서 폭발된 현무암이 바다까지 밀려온 결과를 보고한다. 현무암 지하 마그마가 약 절대온도 1000K로 지상의 중성대를 뚫고 1950m 상공에서 절대온도 1200K로 폭발하면서 나올 때의 속도에 대해 분석했다. 부력(浮力)에 의한 화염 기둥의 열기류인 Plume 화산 폭발로 인한 주변의 공기보다 연소가스의 밀도가 작아져 부력이 발생하고 상승 기류가 형성된다. 화염 기둥은 연속, 간헐, 부력 화염 영역으로 분류된다. 한라산(1950m) 화염 기둥의 속도는 상승한 최고점에서 낙하함으로 위치에너지가 운동에너지로 변환되어 유체흐름에 의해 이 두 식을 같게 놓아 풀면 화산 폭발 속도87.5m/s를 얻었다. 이때 마그마의 밀도는 온도에 반비례한다. 거문오름(456m)은 폭발 속도는 42.6m/s로 계산했다.

• 한국측량학회지
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• 제34권4호
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• pp.357-372
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• 2016

Augustine volcano, located along the Aleutian Arc, is one of the most active volcanoes in Alaska and nearby islands, with seven eruptions occurring between 1812 and 2006. This study monitored the surface displacement before and after the most recent 2006 eruption. For analysis, we conducted a time-series analysis on data observed at the permanent GPS(Global Positioning System) observation stations in Augustine Island between 2005 and 2011. According to the surface displacement analysis results based on GPS data, the movement of the surface inflation at the average speed of 2.3 cm/year three months prior to the eruption has been clearly observed, with the post-eruption surface deflation at the speed of 1.6 cm/year. To compare surface displacements measurement by GPS observation, ENVISAT(Environmental satellite) radar satellite data were collected between 2003 and 2010 and processed the SBAS(Small Baseline Subset) method, one of the time-series analysis techniques using multiple InSAR(Interferometric Synthetic Aperture Radar) data sets. This result represents 0.97 correlation value between GPS and InSAR time-series surface displacements. This research has been completed precise surface deformation using GPS and time-series InSAR methods for a detection of precursor symptom on Augustine volcano.

• 천문학회보
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• 제35권2호
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• pp.50.1-50.1
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• 2010

The New Solar Telescope (NST) at Big Bear Solar Observatory (BBSO) is the recently constructed world largest 1.6 m optical solar telescope on the ground. We took an observation of the north polar limb in H-alpha line center wavelength on 2009 August 26 with the instrument at Nasmyth focus of the NST and found a remarkable small-scale H-alpha eruption from 18:20 UT and 18:45 UT. The eruption occurred with a relatively slow speed of about 10 km/s in early stage and a slight acceleration up to 20-30 km/s in later stage. We also found that the eruption shows a deflection along the pre-existing magnetic field as well as several interesting features such as bifurcation, rotation, horizontal oscillation, and direction and thickness change of its structure during the eruption. In this talk, we will report the observational properties of the small-scale eruption observed by the NST and discuss their implication on magnetic reconnection.

• Journal of the Korean Association of Oral and Maxillofacial Surgeons
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• 제36권6호
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• pp.528-532
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• 2010

Introduction: There are few reports on tooth eruption through Bio-Oss grafts. To our knowledge, there are no reports on whether teeth can erupt normally through the grafts. The aim of this study was to examine the effect of Bio-Oss grafts on tooth eruption in a canine model. Materials and Methods: In five 10-week-old dogs, the deciduous third mandibular molars in one jaw quadrant of each animal were extracted and the fresh extraction sockets were then filled with Bio-Oss particles (experimental side). No such treatments were performed on the contralateral side (control side). A clinical and radiological evaluation was carried out every other week to evaluate the eruption level of the permanent third mandibular premolars and compare the eruption levels between the two sides. Results: At week 4 after the experiment, the permanent third premolars began to erupt on both sides. At week 12, the crown of the permanent third premolar emerged from the gingiva on both sides. At week 20, the permanent third premolars on both sides erupted enough to occlude the opposing teeth. No significant differences were found between the control and experimental sides in terms of the eruption speed of the permanent third molars. Conclusion: These findings demonstrate that the grafting of Bio-Oss particles into the alveolar bone defects does not affect tooth eruption.

• 천문학회지
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• 제37권1호
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• pp.41-53
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• 2004

It has been a big mystery what drives filament eruptions and flares. We have studied in detail an X1.8 flare and its associated filament eruption that occurred in NOAA Active Region 9236 on November 24,2000. For this work we have analyzed high temporal (about 1 minute) and spatial (about 1 arcsec) resolution images taken by Michelson Doppler Imager (MDI) onboard the Solar and Heliospheric Observatory, Hoc centerline and blue wing ($-0.6{\AA}$) images from Big Bear Solar Observatory, and 1600 ${\AA}$ UV images by the Transition Region and Corona Explorer (TRACE). We have found that there were several transient brightenings seen in H$\alpha$ and, more noticeably in TRACE 1600 ${\AA}$ images around the preflare phase. A closer look at the UV brightenings in 1600 ${\AA}$ images reveals that they took place near one end of the erupting filament, and are a kind of jets supplying mass into the transient loops seen in 1600 ${\AA}$. These brightenings were also associated with canceling magnetic features (CMFs) as seen in the MDI magnetograms. The flux variations of these CMFs suggest that the flux cancellation may have been driven by the emergence of the new flux. For this event, we have estimated the ejection speeds of the filament ranging from 10 to 160 km $s^{-1}$ for the first twenty minutes. It is noted that the initiation of the filament eruption (as defined by the rise speed less than 20 km $s^{-1}$) coincided with the preflare activity characterized by UV brightenings and CMFs. The speed of the associated LASCO CME can be well extrapolated from the observed filament speed and its direction is consistent with those of the disturbed UV loops associated with the preflare activity. Supposing the H$\alpha$/UV transient brightenings and the canceling magnetic features are due to magnetic reconnect ion in the low atmosphere, our results may be strong observational evidence supporting that the initiation of the filament eruption and the preflare phase of the associated flare may be physically related to low-atmosphere magnetic reconnection.

• 천문학회보
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• 제37권1호
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• pp.89.1-89.1
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• 2012

We have investigated a coronal jet observed near the limb on 2010 June 27 by the Hinode/X-Ray Telescope (XRT), EUV Imaging Spectrograph (EIS), and Solar Optical Telescope (SOT), and the SDO/Atmospheric Imaging Assembly (AIA), Helioseismic and Magnetic Imager (HMI), and on the disk by STEREO-A/EUVI. From EUV (AIA and EIS) and soft X-ray (XRT) images we have identified both cool and hot jets. There was a small loop eruption in Ca II images of the SOT before the jet eruption. Using high temporal and multi wavelength AIA images, we found that the hot jet preceded its associated cool jet by about 2 minutes. The cool jet showed helical-like structures during the rising period. According to the spectroscopic analysis, the jet's emission changed from blue to red shift with time, implying helical motions in the jet. The STEREO observation, which enabled us to observe the jet projected against the disk, showed that there was a dim loop associated with the jet. We have measured a propagation speed of ~800 km/s for the dimming front. This is comparable to the Alfven speed in the loop computed from a magnetic field extrapolation of the HMI photospheric field measured 5 days earlier and the loop densities obtained from EIS Fe XIV line ratios. We interpret the dimming as indicating the presence of Alfvenic waves initiated by reconnection in the upper chromosphere.