• 천문학회지
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• 제47권6호
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• pp.259-277
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• 2014

G192.8-1.1 has been known as one of the faintest supernova remnants (SNRs) in the Galax until the radio continuum of G192.8-1.1 is proved to be thermal by Gao et al. (2011). Yet, the nature of G192.8-1.1 has not been fully investigated. Here, we report the possible discovery of faint non-thermal radio continuum components with a spectral index ${\alpha}{\sim}0.56(S_{\nu}{\propto}{\nu}^{-{\alpha}})$ around G192.8-1.1, while of the radio continuum emission is thermal. Also, our Arecibo $H_I$ data reveal an $H_I$ shell, expanding with an expansion velocity of $20-60km\;s^{-1}$, that has an excellent morphological correlation with the radio continuum emission. The estimated physical parameters of the $H_I$ shell and the possible association of non-thermal radio continuum emission with it suggest G192.8-1.1 to be an~0.3 Myr-old SNR. However, the presence of thermal radio continuum implies the presence of early-type stars in the same region. One possibility is that a massive star is ionizing the interior of an old SNR. If it is the case, the electron distribution assumed by the centrally-peaked surface brightness of thermal emission implies that G192.8-1.1 is a "thermal-composite" SNR, rather than a typical shell-type SNR, where the central hot gas that used to be bright in X-rays has cooled down. Therefore, we propose that G192.8-1.1 is an old evolved thermal-composite SNR showing recurring emission in the radio continuum due to a nearby massive star. The infrared image supports that the $H_I$ shell of G192.8-1.1 is currently encountering a nearby star forming region that possibly contains an early type star(s).

• 대한조선학회논문집
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• 제31권2호
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• pp.1-6
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• 1994

선박의 개념설계를 지원하는 전산시스템은 창조적인 설계를 지원할 수 있을뿐만 아니라, 작업환경의 변화에 유연하게 대처할 수 있는 기능이 필요하다. 본 연구에서는 기존의 개념설계시스템의 기능을 확장한 유연화된 개념설계시스템을 개발하였다. 시스템을 구성하는 각 모듈들은 독립적인 수행이 가능하도록 개발되었으며, 수퍼 어플리케이션 개념을 이용하여 상위레벨에서 각 모듈들을 제어하는 기능을 추가하였다. 수퍼 어플리케이션 개념의 제어 프로그램을 SUN SPARC Work-station의 UNIX C Shell 환경하에서 개발하였다.

• 천문학회보
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• 제37권1호
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• pp.72.2-72.2
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• 2012

We present the results of HI 21 cm line observations to explore the nature of the high-velocity (HV) HI gas at - 173${\circ}$, which appears as faint, wing-like, Hi emission that extends to velocities beyond those allowed by Galactic rotation in the low-resolution surveys. We designate this feature as Forbidden Velocity Wing (FVW) 172.8+1.5. Our high-resolution Arecibo HI observations show that FVW 172.8+1.5 is composed of knots, filaments, and ring-like structures distributed over an area of a few degrees in extent. These HV HI emission features are well correlated with the HII complex G173+1.5, which is composed of five Sharpless HII regions distributed along a radio continuum loop of size 4.4${\times}$3.4, or -138 pc ${\times}$ 107 pc, at a distance of 1.8 kpc. G173+1.5 is one of the largest star-forming regions in the outer Galaxy. The HV HI gas and the radio continuum loop seem to trace an expanding shell. Its derived HI parameters including large expansion velocity (55 km/s) imply the SNR interpretation. Hot xray emission is detected within the HII complex, which also supports its SNR origin. The FVW172.8+1.5 is most likely the products of a supernova explosion(s) within the HII complex, possibly in a cluster that triggered the formation of these HII regions.

• 천문학회지
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• 제28권2호
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• pp.255-264
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• 1995

The HII region S140 and the associated molecular cloud L1204 have been observed with 10 molecular transitions, CO (1-0), $^{13}CO$ (1-0), $C^{18}O$ (1-0), CS (2-1), $HCO^+$ (1-0), HCN (1-0), SO (${2_2}-{1_1}$), $SO_2(2_{20}-3_{13})$, OCS (8-7), and $HNCO\;(4_{04}-3_{03})$ with ${\sim}50"$ angular resolutions. More than 7,000 spectra were obtained in total. The morphology of this region shows a massive fragment (the S140 core) and the extended envelope to the northeast. Several gas condensations have been identified in the envelope, having masses of ${\sim}10^{3}M_{\odot}$ and gas number densities of ${\lesssim}10^{4}cm^{-3}$ to $3{\times}10^{5}cm^{-3}$ in their cores. The column densities of the observed molecular species toward the S140 core appear to be the typical warm clouds' abundances. It seems to be that the S140 core and L1204 have been swept up by an expanding shell called the Cepheus bubble. The large value of $L_{IR}$(embedded\;stars)/$M_{cloud}\;{\sim}\;5\;L_{\odot}$/$M_{\odot}$ of the S140 core may suggest that the star formation has been stimulated by the HII region, but the shock velocity and the pressure of the region seem to give a hint of the spontaneous star formation by the self gravity.

• 천문학회지
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• 제47권5호
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• pp.179-185
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• 2014

We study the physical and chemical properties of the molecular clump hosting a young stellar cluster, IRAS 20160+3636, which is believed to have formed via the "collect and collapse" process. Physical parameters of the UC H II region associated with the embedded cluster are measured from the radio continuum observations. This source is found to be a typical Galactic UC H II region, with a B0.5 type exciting star, if it is ionized by a single star. We derive a CN/HCN abundance ratio larger than 1 over this region, which may suggest that this clump is being affected by the UV radiation from the H II region.

• 한국패류학회지
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• 제31권2호
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• pp.83-92
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• 2015

본 연구는 북방전복 육상 수조 내 고밀도 중간양성 방법을 모색하기 위해 부착면적 확대를 위해 다단식 shelter 설치와 수조 내 중층 이상의 가두리를 설치하여 성장을 비교하고 아울러 전복류 육상 양성방법인 'shallow race way' 국내 도입 가능성을 조사하였다. Shelter 실험구는 PE (polyethylene) 재질의 shelter ($63{\times}98cm$) 1층형 (the single layer shelter, SLS), 2층형 (the double layer shelter, DLS), 3층형 (the triple layer shleter, TLS) 과 육상 가두리 양성방식 (the single layer shelter and net cage culture, SLSNC), 그리고 'shallow race way' 방식을 polyvinyl chloride (PVC)로 제작하여 고랑수로양성 (culture of the ditch raceway tank, CDRT)과 편평한 수로양성 (culture of the floor raceway tank, CFRT) 방식을 설정하였으며, 실험구는 모두 2반복으로 실시되었다. 각 실험구별 SLS 기준 60%밀도로 수용한 실험 전복 (최초 수용 시 평균각장 $25.19{\pm}0.50mm$, 중량 $1.93{\pm}0.14g$), 성장에서 각장의 절대성장율 (absolute growth rate, ARG), 일간성장율 (daily growth rate, DGR) 및 순간성장율 (specific growth rate, SGR) 과 중량의 증중률 (weight gain, WG), 일간증중률 (daily weight gain, DWG) 에서 SLSNC 제외한 모든 실험구가 유의적인 차이가 없었다. 그리고 생존율에서는 CDRT와 CFRT가 유의적으로 낮았다 (P < 0.05). 따라서 shelter를 이용하여 부착면적을 확대한 고밀도 전복치패 육상 중간육성 사육 시 단층과 다단층에서 성장과 생존율에서 차이가 없으며, 호주 등에서 사용되는 shelter 없는 'shallow race way'의 얇은 수심사육은 국내 북방전복 육상 중간양성 방식으로 도입하기에 적합하지 않는 것으로 판단된다.

• 천문학회지
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• 제50권6호
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• pp.157-165
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• 2017

$H_2O$ maser emission at 22 GHz in the circumstellar envelope is one of the good tracers of detailed physics and kinematics in the mass loss process of asymptotic giant branch stars. Long-term monitoring of an $H_2O$ maser spectrum with high time resolution enables us to clarify acceleration processes of the expanding shell in the stellar atmosphere. We monitored the $H_2O$ maser emission of the semi-regular variable R Crt with the Kagoshima 6-m telescope, and obtained a large data set of over 180 maser spectra over a period of 1.3 years with an observational span of a few days. Using an automatic peak detection method based on least-squares fitting, we exhaustively detected peaks as significant velocity components with the radial velocity on a $0.1kms^{-1}$ scale. This analysis result shows that the radial velocity of red-shifted and blue-shifted components exhibits a change between acceleration and deceleration on the time scale of a few hundred days. These velocity variations are likely to correlate with intensity variations, in particular during flaring state of $H_2O$ masers. It seems reasonable to consider that the velocity variation of the maser source is caused by shock propagation in the envelope due to stellar pulsation. However, it is difficult to explain the relationship between the velocity variation and the intensity variation only from shock propagation effects. We found that a time delay of the integrated maser intensity with respect to the optical light curve is about 150 days.

• Maxillofacial Plastic and Reconstructive Surgery
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• 제29권4호
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• pp.321-328
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• 2007

If there are problems for us to sleep, we are faced with fatigue and dizziness in the day. Snoring and OSAS (obstructive sleep apnea syndrome) during sleeping are the main cause of sleep disorder. Treatments through surgical method and sleep splint can be performed to treat snoring and OSAS. Relapse of snoring and OSAS is common after treatment by surgical method. But, Recently sleep splint is frequently applied to treat snoring and OSAS with surgical treatment, because it is convenient and conservative. Sleep splint treat snoring and OSAS by ensuring airway through nose. As first step of fabrication occlusal bite is gained at a point that patient get feeling of increased nasal breathing in supined position, and next, the bite is transfered to sleep splint. This study surveyed the effect of sleep splint by questionnaire to the out-patients (the Dept. of Oral and Maxillofacial Surgery, Chonbuk National University Hospital) weared sleep splint and their partners, secondarily measured airflow through nose by aerophone II after wearing sleep splint and finally evaluated the effect of treatment of snoring and OSAS by sleep splint. The obtained result were as follows; 1. Though 'sleep splint' couldn't eliminate fundamental problems of snoring, it could improve the symptoms when patients were selected could using the 'Nakagawa's respiration method'. 2. Patients who used the sleep splint could breathe stably when patients are sleeping stably. Wearing a 'sleep splint' improved airflow by expanding the upper airway. 3. Even though sleep splint can be made with variable materials, the patients expressed the most satisfaction on the splint with '0.75mm hard shell'. 4. The 'Herbst' may allows the mandible to move the TMJ to relax. Nevertheless, some patients experienced a discomfort or irritation. 5. In Snoring and OSAS cases, it is recommended that patients should first explore non-surgical options prior to choosing a surgical treatment.