• The Bulletin of The Korean Astronomical Society
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• v.36 no.2
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• pp.146.1-146.1
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• 2011

최근의 관측에 의하면 우리 은하의 헤일로내 field에 위치한 subdwarf B 항성이 헬륨이 증가된 구상성단의 푸른 수평계열성 ( Extreme Blue Horizontal Branch ) 과 동일한 기원을 가질 것으로 예측된다. 초기 우주 환경과 비슷한 헬륨 함량을 보이는 환경에서는 Building Block 내부 이외에는 헬륨이 충분히 증가된 가스를 공급할 수 없기 때문에 이러한 기원을 가지는 sdB 항성의 개수를 예측함으로써 우리 은하의 초기 Building Block으로 부터 얼마나 많은 수의 항성이 헤일로에 뿌려졌는지 예측할 수 있다. 우리는 우리 은하내 나이가 많은 항성들로 이루어진 헤일로와 Bulge 내에 이러한 기원을 가지는 sdB 항성의 개수를 예측한 결과, 초기 Building Block으로 부터 유입된 sdB 항성이 최소 8만 여개 이상일 것으로 추정하였다. 이 개수는 우리 은하 구상 성단 중 은하 Building Block의 잔재로 생각되는 성단에 존재하는 헬륨이 증가된 수평계열성의 총 합의 10배 이상의 규모에 해당한다. 이는 이들 성단이 은하 생성 초기에는 현재의 질량 규모보다 최소 10배 이상 무거웠을 것이라는 가정과 일치하는 결과이다.

• The Bulletin of The Korean Astronomical Society
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• v.35 no.1
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• pp.54.1-54.1
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• 2010

최근 이루어진 구상성단내 다중항성종족의 발견은 항성계의 형성 및 진화, 더 나아가 우리 은하의 형성 등에 획기적인 변혁을 필요로 하는 중요한 사건이다. 본 발표에서는 항성종족이론이 현재 직면한 문제점들과 해결 방안들을 대한 검토와 KGMT시대에 대비한 전망을 토의할 것이다.

• The Bulletin of The Korean Astronomical Society
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• v.39 no.2
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• pp.85.2-85.2
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• 2014

최근 10년 동안의 측광 및 분광관측을 통하여 우리은하 내 구상성단들 중 대부분이 적어도 2개 이상의 항성종족을 갖는다고 밝혀졌다. 현재까지 이루어진 대부분의 구상성단의 항성종족 연구에서는 관측된 색등급도와 항성종족 합성모델 사이에 eye-fitting을 함으로써 항성종족 파라미터, 즉 중원소함량, 나이, 헬륨함량 등을 추정해왔다. 우리는 구상성단의 항성종족을 분석하기 위해 ${\chi}^2$-Minimization에 의거하여 구상성단과 항성종족 합성모델의 Hess Diagram을 비교하고, 수치계산 기법을 도입하여 최적의 파라미터를 추정하는 알고리즘을 개발하였다. 이 연구에서는 가상으로 만든 성단에 대하여 Recovery Test를 수행함으로써 이 알고리즘의 Self-Consistency를 검증하였고, 실제 관측결과를 사용하여 이 연구의 적용 가능성을 조사하였다.

• Journal of Astronomy and Space Sciences
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• v.23 no.1
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• pp.11-18
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• 2006

We have modeled dust envelopes around silicate carbon stars using optical properties for a mixture of amorphous carbon and silicate dust grains paying close attention to the infrared observations of the stars. The 4 stars show various properties in chemistry and location of the dust shell. We expect that the objects that fit a simple detached silicate dust shell model could be in the transition phase of the stellar chemistry. For binary system objects, we find that a mixed dust chemistry model would be necessary.

• Korean Journal of Environmental Agriculture
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• v.32 no.3
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• pp.231-239
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• 2013

BACKGROUND: The disease resistant (OsCK1) rice was generated by inserting choline kinase (CK1) and phosphinothricin acetyltransferase (PAT) genes isolated from Oriza sativa and Streptomyces hygroscopicus into the genome of rice (Nakdongbyeo). With the potential problems of safety, the non-target organism evaluation is required as an essential element for the environmental risk assessment of genetically modified (GM) crops. In present study, we studied the effects on survival of Misgurnus anguillicaudatus and Cyprinus carpio, commonly used as a model organism in ecotoxicological studies. METHODS AND RESULTS: The M. anguillicaudatus and C. carpio were fed on disease resistant (OsCK1) rice and non-genetically modified (non-GM) rice (Nakdongbyeo) to 0, 10, 100, 1,000 and 5,000 mg/L, as treatment concentration respectively. The OsCK1 rice used for the test was confirmed to have the OsCK1/PAT gene expression by the PCR and ELISA analysis. Feeding test showed that no significant differences in cumulative immobility and abnormal response of M. anguillicaudatus and C. carpio fed on between OsCK1 rice and non-GM rice. The 96hr-$LC_{50}$ values showed no difference between OsCK1 rice (>5,000 mg/L) and non-GM rice (>5,000 mg/L). CONCLUSION(S): The results of this study suggested that there was no significant difference in toxicity for M. anguillicaudatus and C. carpio between OsCK1 rice and non-GM counterparts.

• Journal of the Korean earth science society
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• v.38 no.3
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• pp.209-221
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• 2017

We investigate the star formation rate, stellar mass, and gas-phase metallicity of local starburst galaxies with different star formation time scales based on their optical spectra. The observation is made using the longslit spectrograph attached to the 4K CCD on the Bohyunsan Optical Astronomy Observatory 1.8m telescope, targeting 21 Wolf-Rayet galaxies as young starbursts and 13 UV excess galaxies as slightly older starbursts. A Baldwin-Phillips-Terlevich diagram analysis shows that 50% of the observed targets are pure star-forming galaxies while only 15% are classified as Active Galactic Nuclei. Fraction of galaxies that reside in composite region is higher in UV excess galaxies than in Wolf-Rayet galaxies, suggesting that the AGN development requires extra time after the onset of the star formation. Most of the observed starburst galaxies have stellar masses of $10^{9-11}M_{\odot}$ and stellar formation rates of $0.01-100M_{\odot}yr^{-1}$, and their star formation rates are consistent with that of the SDSS star forming main sequence galaxies of similar stellar mass. There is no significant difference between Wolf-Rayet galaxies and UV excess galaxies in terms of the stellar mass and star formation rate. We also see a mass-metallicity relation for local starbursts with slightly lower metallicity for a given stellar mass, which implies the existence of a strong feedback activity due to the star formation in these galaxies.

• Journal of Astronomy and Space Sciences
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• v.11 no.1
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• pp.107-114
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• 1994

This paper describes a method for the determination of wind parameters as mass-loss rate, wind velocity, stochastic velocity in Zeta Aurigae type binaries. We have modified the Baade's (1989) computer code to analyze the wind parameters of Zeta Aurigae type binaries according to the least squares criterion. The modified program adjusts the wind parameters by the method of differential corrections. We have appled this method to the IUE observations of 32 Cygni. We have fitted a theoretical line profile to the IUE observations of Fe II resonance line at various phases. The mass-loss rate, wind velocity and stochastic velocity of 32 Cygni obtained in this paper are $2.18{\times}10^{-8}M_{\odot}/yr$, 132.14km/s, 39.82km/s, respectively.

• Journal of Astronomy and Space Sciences
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• v.12 no.1
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• pp.14-20
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• 1995

We calculated the wind velocities for 32 Cyg in order to understand how influence a damping length on the wind of supergiant driven by Alfven waves. Four cases, $\lambda$=0.9, 1.0, 5.0, the ratio of the damping length to the supergiant's radius, and the damping length increasing linearly with the distance from the star, were compared. The results showed the forces by Alfven waves gave the major contribution to the wind velocity but the forces by the pressure and gravitation did little. The model for the damping length with the linear relation showed the rapid increased due to short damping length near the surface of the star.

• Journal of Dental Rehabilitation and Applied Science
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• v.36 no.2
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• pp.61-69
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• 2020

Purpose: Zirconia fixed partial dentures with mandibular 2^nd premolar and 2^nd molar as abutments are fabricated and then the effects of inter-abutment distance on fracture resistance of zirconia fixed partial dentures is studied. Materials and Methods: The materials used in this study are Cameleon S zirconia block and S2 zirconia block, which are divided into CS Group and S2 Group applying different inter-abutment distance for each material, and the sintered zirconia fixed partial denture was luted to the epoxy resin die using a temporary luting cement, and then the fracture resistance was measured by placing a 6 mm diameter hardened steel ball on the occlusal surfaces of the pontics and applying pressure at a cross head speed of 1.0 mm/min on a universal testing machine with a load cell of 5.0 kN. Results: The fracture resistance of zirconia fixed partial dentures is not significantly affected by inter-abutment distance The fracture resistance of zirconia fixed partial dentures in CS Group was significantly higher in 15 mm of inter-abutment distance than in 13 mm and 17 mm of inter-abutment distance (P < 0.05). The fracture resistance of zirconia fixed partial dentures in S2 Group was not significantly different between the three groups (P > 0.05). Conclusion: The fracture resistance of zirconia fixed partial dentures with mandibular 2^nd premolar and 2^nd molar as abutments does not significantly affected by the inter-abutment distance.

• Journal of Astronomy and Space Sciences
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• v.16 no.2
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• pp.255-264
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• 1999

We calculate the theoretical line profiles in order to investigate the influence of various velocity parameters. Line profiles are calculated by using the exponential velocoty law with two acceleration regions for orbital phases $\phi$ = 0.07 and $\phi$ = 0.06. From this compttation we find that the influence of the wind velocity gradient on a giant star is more important in the region near the star than in the region away from the star. The observed lines show stronger emission than the calculated line profiles and we interpret the difference is caused by the inhomogeniety in the atmosphere of 32 Cyg.