• Proceedings of the PSK Conference
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• 2000.10a
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• pp.242.2-242.2
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• 2000

• Proceedings of the PSK Conference
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• 2000.10a
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• pp.247.2-247.2
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• 2000

• Proceedings of the Korean Magnestics Society Conference
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• 2002.04a
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• pp.24-25
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• 2002

No Abstract, See Full Text

• Proceedings of the Korea Air Pollution Research Association Conference
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• 1999.10a
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• pp.428-429
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• 1999

잘 알려져 있듯 광화학 오존 생성의 첫 단계는 N $O_2$가 자외선을 받아 NO와 O로 해리되는 과정이다. N $O_2$ ＋ h$\upsilon$ $\longrightarrow$ NO ＋ O 일반적으로 이러한 광해리 반응을 정량화하기 위하여 아래의 식과 같이 광해리 상수, $J_{NO2}$를 정의한다.(중략)략)

• Publications of The Korean Astronomical Society
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• v.30 no.2
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• pp.217-218
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• 2015

In this work, we present the result of our follow-up observations of SDSS J092741.73+332959.1 and SDSS J130733.49+215636.7 using the 2.35 m Thai National Telescope and ULTRASPEC instrument. Both systems are listed among the recently found white dwarf main sequence binaries from the Sloan Digital Sky Survey. SDSS J092741.73+332959.1 is a new PCEB with a period of 2.3 days, the longest orbital period known to date for white dwarf binaries. SDSS J130733.49+215636.7 is confirmed to be an eclipsing system with a period of 0.21 days from the Catalina Survey's light curve, however the parameters for the white dwarf are still uncertain. Our goal is to determine precise parameters for both systems using the Binary Maker 3 software. The observation for SDSS J0927+3329 was done on 9 January 2014 in the SDSS r' filter while the data for SDSS J1307+2156 were taken in the z' filter on 27 April 2014. Our models show that the red dwarf companions in both systems are well constrained inside their Roche Lobes. We find that the binary M2/M1 ratio in SDSS J0927+3329 is close to 0.5, with white dwarf and M-dwarf temperatures of 12000 K and 3300 K, respectively. Our preliminary result for SDSS J1307+2156 show that this system has an extreme mass ratio of 0.3. The white dwarf in this system has a temperature of 7500 K and the companion star has an effective temperature of 3150 K.

• Transactions of the Korean Society of Mechanical Engineers A
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• v.27 no.1
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• pp.119-125
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• 2003

A way to measure the second parameter $A_2$of CT specimens is described. The displacement $\delta$$_{5}$ which is measured continuously from visual images of the lateral surface during crack growth is used to calculate the A, as a function of crack growth. The crack length is measured by DCPD(Direct Current Potential Drop) method and the J-resistance curve is determined according to ASTM standard E1737-96. To prove the validity of this method, three dimensional finite element analyses were performed, and variations of the displacements $\delta$$_{5}$ and $A_2$along the thickness were explored. As the result, it has been shown that the $\delta$$_{5}$ measured from the visual images of the lateral surface and the corresponding $A_2$can be regarded as the average through the thickness for 1T and 1/2T specimens of SA106Gr.C steel.steel.

• Proceedings of the KSRS Conference
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• 2008.10a
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• pp.285-288
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• 2008

We analyzed evaporation data in the Japanese Ocean Flux Data Sets with Use of Remote Sensing Observations (J-OFURO) Ver.2. There exists huge evaporation in Gulf Stream, Kuroshio Extension, the ocean dessert and the southern part of the Indian Ocean. The temporal variation of evaporation is overwhelmingly large, of which the standard deviation is more than 120(mm), in the Kuroshio Extension region. Also, the result of harmonic analysis gives that this large variation is closely related to annual variation. In addition, the first EOF mode shows long-term variation showing the maximum amplitude between 1992 and 1994 and remarkable decrease after 1994, and large amplitude in the equatorial region and northeast of Australia. The second and third modes were strongly influenced by El Nino. Moreover, we compared J-OFURO2 evaporation product with other products. We used six kinds of data sets (HOAPS3 and GSSTF2 of satellite data, NRA1, NRA2, ERA40 and JRA25 of reanalysis data) for comparison. Most products show underestimation in the most regions, in particular, in the northern North Pacific, mid-latitudes of the eastern South Pacific, and high-latitudes of the South Pacific compared with J-OFUR02. On the other hand, JRA25 and NRA2 show large overestimation in the equatorial regions. RMS difference between NRA2 and J-OFURO2 in the Kuroshio Extension was significantly large, more than 120(mm).

• Proceedings of the Korean Powder Metallurgy Institute Conference
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• 2006.09b
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• pp.1165-1166
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• 2006

An experiment was carried out to investigate the effect of Ba Stearate as a reducing agent on the magnetic and physical properties of anisotropic $BaFe_2-W$ type ferrite magnets. It was found that the magnetic properties of $BaO{\cdot}8.5Fe_2O_3$ were improved by adding 0.3 wt% of Ba Stearate, 0.5 wt% of $SiO_2$, and 0.5 wt% of CaO together. The optimum conditions for making magnets were as follows; semisintering condition: $1350^{\circ}C{\times}4.0$ h in nitrogen gas atmosphere, drying condition: $180^{\circ}C{\times}2.0$ h in air, sintering condition: $1160^{\circ}C{\times}1.5$ h in nitrogen gas atmosphere. Magnetic and physical properties of a typical sample were $J_m$ = 0.46 T, $J_r$ = 0.43 T, $H_{cJ}$ = 182.3 kA/m, $H_{cB}$ = 177.2 kA/m, $(BH)_{max}$ = 33.8 kJ/$m^3$, $T_C$ = $495^{\circ}C$ and $K_A$ = $2.65{\times}10^5\;J/m^3$ and $H_A$ = 1332 kA/m.

• The Bulletin of The Korean Astronomical Society
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• v.44 no.1
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• pp.67.2-67.2
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• 2019

We present the results of KVN and ALMA observations toward WX Psc (IRC+10011) which is a long-period variable OH/IR star. The SiO masers of v=1 and v=2, J=5-4, and the SiO thermal emission of v=0, J=5-4 were observed together with H2O v2=1 (232.6 GHz) and continuum emission at ALMA Band 6 in October 2017 (Cycle 5). This observation aims to investigate the physical association between the inner and outer parts of the circumstellar envelope (CSE) swept by the stellar winds, which is very crucial to understand the asymmetric outward motions developed during the evolutionary phases from the asymptotic giant branch (AGB) stars to the planetary nebulae (PNe). The strong SiO maser features and thermal emissions are detected together with the continuum emission in ALMA observation, which imply the elongated morphology of the CSE of WX Psc. While the spatial resolution of about 20 mas in ALMA observation cannot clearly resolve the detailed characteristics of the inner part of the CSE, the Korean VLBI Network (KVN) observations show the spatial distributions of the v=1 J=1-0, J=2-1, J=3-2 SiO masers emitted from the inner regions of CSE, which are the complementary to the ALMA results. Therefore, we expect these results reveal how the bipolar features of the 22 GHz H2O maser are connected to the innermost region of CSE through the dust condensation region, which is closely related to the enormous mass ejection of the evolved stars.

• The Bulletin of The Korean Astronomical Society
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• v.43 no.2
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• pp.52.1-52.1
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• 2018

Orion Molecular Clouds Complex(OMC) 분자운에는 별 생성은 없으면서 은하면 방향으로 누워있는 큰 규모($10^{\circ}{\times}0.5^{\circ}$)의 필라멘트 구조가 있다. 본 연구는 북쪽 필라멘트(이하 NF)를 대상으로 12CO (J = 1-0) 선 관측 데이터를 이용하여 필라멘트의 운동학적 연구를 수행함으로서 은하면과의 상관관계를 알아보고자 하였다. 관측은 공간분해능은 2 arcmin인 SRAO(Seoul Radio Astronomy Observatory)의 6m 밀리미터 망원경이 사용되었고 큰 규모로 인해 은하면으로부터 먼 순서로 NF1, NF2, NF3 세 곳으로 관측 지역이 정해졌다. 연구결과 필라멘트는 매우 낮은 수준의 12CO (J = 2-1)과 티끌 분포에서 자기장을 따라 은하면 방향으로 연계되어 보였다. 밀도 분포에서는 SRAO 12CO (J = 1-0) 적분강도와 Planck 위성의 12CO (J = 2-1)과 티끌 자료를 이용했을 때, 12CO와 성간 티끌은 주로 은하면에 수직인 방향에서 밀도가 높았다. 속도 분포와 위치 속도 분석을 통해 NF는 단일 구조의 분자운 형태이고 NF2 하단에서는 회전 운동의 가능성이 확인되었다. NF3는 자기장에 의해 생성된 나선형 회전을 하고 있으며, NF2와 NF3를 따라 은하면을 향하여 12CO (J = 1-0)를 비롯한 물질이 흐르고 있음도 확인되었다. 하지만 은하면을 향하여 물질이 흐르는 원인을 제공하는 천체가 무엇인지와 NF1과 NF2 상단의 회전 운동은 확인 할 수 없었으며 이들 지역에 대한 상세한 관측이 요구된다.