• The Bulletin of The Korean Astronomical Society
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• v.37 no.2
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• pp.240.1-240.1
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• 2012

We performed simultaneous observations of SiO v=1, 2, $^{29}SiO$ v=0, J=1-0 and $H_2O$ $6_{16}-5_{23}$ maser lines toward 252 OH/IR stars using the Korean VLBI Network 21m telescopes. The observations were carried out from 2011 November to 2012 July for studying SiO and $H_2O$ maser properties associated with the evolutionary stages of OH/IR stars. Both $H_2O$ and SiO masers were detected from 49 sources, one-side maser of SiO and $H_2O$ was detected from 109 and 11 sources, respectively. Mutual relations between SiO and $H_2O$ maser properties are investigated based on statistical analyses. We also investigate these maser properties in the IRAS two-color diagram related with stellar evolutionary sequence.

• Proceedings of the KIEE Conference
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• 1996.11a
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• pp.285-288
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• 1996

The electronic operation of the gas discharge tube is controlled by the electrical energy as sinusoidal waveform in arbitrary frequency range, or as a sequence of pulses at a wide range of duty cycle, the gas composition, the kind of electrode and the vessel geometry. In this paper, the pulsed mode operated gas discharge tube is composed with mixed gas of IIg-Ne ( 10 Torr ), in the tube of 15.0 mm outer diameter and has variable color from red to blue with changing frequency and pulse width in high voltage. As increasing pulse width and frequency in the gas discharge tube, the phenomenons that the electron temperature in the positive column increases and the radiation from atoms of higher upper state energy levels increases, exist. The color have the locus from red (0.4972, 0.3128) to blue (0.2736, 0.2619) in CIE chromacity diagram with increasing pulse width and frequency. The changing method of pulse width and frequency has been shown to be suitable for the luminous color control.

• 한국IT서비스학회:학술대회논문집
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• 2006.11a
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• pp.177-184
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• 2006

시스템의 동적 요소를 기술하고 분석하기 위해 C&C view 아키텍처를 주로 사용하지만 시스템의 실행 순서나 상태에 대한 정보가 부족하기 때문에 단지 C&C view 아키텍처로만 시스템의 동적 요소를 분석하기가 어렵다. FSP model은 시스템의 동작을 표현하기 위한 모델링 언어로써 시스템의 동작을 모델링 할 뿐만 아니라 LTSA라는 FSP 검증 툴을 이용하여 시스템의 특성을 자동으로 파악하기에도 용이한 특성을 가지고 있어 시스템 동적 요소 분석에 도움을 준다. 하지만 관련 정보를 얻기 어려워 FSP model을 구현하는데 어려움이 있다. 이 논문은 C&C view 아키텍처와 요구 사항(Use Case Scenario 혹은 Sequence diagram)을 근간으로 시스템의 동적 요소를 FSP로 모델링 하는 방법을 정의한다. 또한 LTSA 툴을 이용하여 자동적으로 시스템의 특성을 검증할 수 있고, 이를 통해 시스템 구현 전에 시스템의 에러를 찾아내고 해결하는 도움을 줄 수 있다. C&C view 아키텍처는 시스템의 컴포넌트와 커넥터에 대한 정보를 제공하여 주고 요구 사항은 소프트웨어 시스템의 행동에 대한 정보를 제공하여 줄 수 있다. 만약 우리가 컴포넌트와 커넥터에 대한 정보가 있고 시스템 동적 요소에 대해 알고 있다면 우리는 이것을 기반으로 메시지 흐름도를 구현할 수 있다. 메시지 흐름도는 Harel, Kugler 와 Pnueli에 의해 개발된 Synthesized 알고리즘을 이용하여 Statechart로 만들어지고 이것은 바로 FSP model로 변환될 수 있다. 우리가 소프트웨어 시스템에 대한 FSP model을 가지고 있다면 이것을 기반으로 시스템 행동 특성을 체크할 수 있으며 이는 향후 발생할 수 있는 결함을 미리 찾아내는데 유용한 도움이 될 수 있다. 우리는 간단한 예제를 통해 본 논문의 이론을 수립하였으며 이를 기반으로 실제 어플리케이션에 적용하여 그 효용성을 검증하였다.

• Journal of the Korean Society for Railway
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• v.11 no.5
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• pp.433-440
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• 2008

Virtual construction methodology enables to construct project facility from design phase to construction phase in 3D virtual environment. It is a technique that can solve problems of construction in virtual construction process. This study suggests some methodologies of virtual construction and developed a system for a railway station in Honam express railway project based on suggested methodologies. This study developed layout review and layer simulation functions. Those functions can improve the effectiveness of 3D simulation and the virtual construction system can be used as a verification tool for construction process of various construction projects.

• Proceedings of the Korea Information Processing Society Conference
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• 2012.11a
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• pp.1567-1570
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• 2012

기존 연구에서는 순차적, 상태, 엑티브 다이어그램 기반의 테스트케이스 추출을 초점을 두고 있다. 하지만 현재 최신의 모델링 언어인 UML2.4.1(Unified Modeling Language) 기반으로 한 테스트케이스 추출 메커니즘은 없다. 그래서 본 논문은 UML2.4.1 기반에 기존의 원인-결과 다이어그램의 접목을 통해 테스트케이스 추출 메커니즘을 제안 한다. 이를 위해 UML2.4.1 의 메시지-순차적 다이어그램에 ECA Rule(Event Condition Action)기법을 적용하고, 제안한 접목 알고리즘을 통해 확장된 메시지-순차적 다이어그램을 원인-결과 다이어그램과 접목한 후, 결정 테이블화로 테스트케이스를 발생한다. 이러한 절차를 통해 모델링 기반에서 테스트케이스 추출 가이드가 제공된다. 본 논문에서는 복잡한 메시지-순차적 다이어그램을 통해 테스트케이스 발생 사례연구로서 자동차 와이퍼 시스템을 적용한다.

• Journal of the Semiconductor & Display Technology
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• v.16 no.3
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• pp.71-77
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• 2017

As the automobile industry has shifted to software, the Automotive SPICE standard has been established to ensure efficient product development process and quality. In the assessment model, the HIS Scope is the minimum standard for small and medium automotive electric companies to meet OEM requirements. However, in order to achieve the HIS Scope, the output of each process stage that meets the verification criteria of Automotive SPICE must be created. In particular, the test phase takes a lot of resources, which is a big burden for small and medium-sized companies. In this paper, we propose a methodology for creating test cases of software integration test phase based on UML sequence diagram, which is a software design phase of Automotive SPICE HIS Scope, by applying behavior model based testing method. We also propose a tool chain for automating the creation process. This will reduce the resources required to create a test case.

• Informatization Policy
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• v.22 no.4
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• pp.22-44
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• 2015

With the growing interest being reflected in the FinTech industry, much attention has been paid to mobile easy payment services as well. In the era of mobile commerce, the core advantage of using mobile easy payment services(simplifying complex payment procedures and thus facilitating user convenience and reducing the chance of giving up payment) are being more emphasized. Mobile easy payment service market not only includes mobile easy payment service providers but also users, non-users, affiliates, banks, and credit card companies as main stakeholders. Exploring those stakeholders is thus important to thoroughly understand such market. However, extant literature on mobile easy payment services mostly focuses on examining adoption intention of users or non-users. This study, an exploratory research based on interviews, thus aims to extract driving as well as inhibiting factors of mobile easy payment service use from six different perspectives (i.e., social platform, bank, credit card company, affiliate, user, and non-user) and analyze a sequence of cause and effect for each factor. For this, the causal loop diagram was developed to deduce key issues and propose an alternative. Theoretical and practical implications of this study will also be discussed.

• Journal of the Korean earth science society
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• v.27 no.5
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• pp.557-568
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• 2006

We present CCD UBVI photometry for more than 10,000 stars in $20'.5{\times}20'.5$ field of the halo globular cluster M30. From a color-magnitude diagram, main sequence turnoff was obtained when $V_{TO},\;(B-V)_{TO},\;and\;(V-I)_{TO}\;are\;8.63{\pm}0.05,\;0.44{\pm}0.05\;and\;0.63{\pm}0.05$, respectively. From a (U-B)-(B-V) diagram, reddening parameter, E(B-V) equals $0.05{\pm}0.01$ and a UV color excess ${\delta}(U-B)\;is\;0.27{\pm}0.01$. The abundance is derived, where [Fe/H] equals $-2.05{\pm}0.09$ according to the photometric method and spectroscopic data. The observed luminosity function of M30 shows an excess in the number of red giants relative to the number of turnoff stars, when comparing with the predictions of canonical models. Using the Hipparcos parallaxes for subdwarfs, we estimate distance modulus, $(m-M)_o\;as\;14.75{\pm}0.12$. Using the R and R' method, we find helium abundances, Y(R) as $0.23{\pm}0.02$, Y(R') as $0.29{\pm}0.02$, respectively. Finally, the cluster' sage dispersion was deduced from 10.71 Gyr to 17 Gyr.

• Journal of The Korean Astronomical Society
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• v.49 no.6
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• pp.261-288
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• 2016

We present the results of simultaneous monitoring observations of $H_2O$ $6_{1,6}-5_{2,3}$ (22GHz) and SiO J=1-0, 2-1, 3-2 maser lines (43, 86, 129GHz) toward five post-AGB (candidate) stars, using the 21-m single-dish telescopes of the Korean VLBI Network. Depending on the target objects, 7 - 11 epochs of data were obtained. We detected both $H_2O$ and SiO maser lines from four sources: OH16.1-0.3, OH38.10-0.13, OH65.5+1.3, and IRAS 19312+1950. We could not detect $H_2O$ maser emission toward OH13.1+5.1 between the late OH/IR and post-AGB stage. The detected $H_2O$ masers show typical double-peaked line profiles. The SiO masers from four sources, except IRAS 19312+1950, show the peaks around the stellar velocity as a single peak, whereas the SiO masers from IRAS 19312+1950 occur above the red peak of the $H_2O$ maser. We analyzed the properties of detected maser lines, and investigated their evolutionary state through comparison with the full widths at zero power. The distribution of observed target sources was also investigated in the IRAS two-color diagram in relation with the evolutionary stage of post-AGB stars. From our analyses, the evolutionary sequence of observed sources is suggested as OH65.5+1.3${\rightarrow}$OH13.1+5.1${\rightarrow}$OH16.1-0.3${\rightarrow}$OH38.10-0.13, except for IRAS 19312+1950. In addition, OH13.1+5.1 from which the $H_2O$ maser has not been detected is suggested to be on the gateway toward the post-AGB stage. With respect to the enigmatic object, IRAS 19312+1950, we could not clearly figure out its nature. To properly explain the unusual phenomena of SiO and $H_2O$ masers, it is essential to establish the relative locations and spatial distributions of two masers using VLBI technique. We also include the $1.2-160{\mu}m$ spectral energy distribution using photometric data from the following surveys: 2MASS, WISE, MSX, IRAS, and AKARI (IRC and FIS). In addition, from the IRAS LRS spectra, we found that the depth of silicate absorption features shows significant variations depending on the evolutionary sequence, associated with the termination of AGB phase mass-loss.

• Journal of The Korean Astronomical Society
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• v.49 no.5
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• pp.199-208
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• 2016

We present photometric results of the δ Sct star V1162 Ori, which is extensively monitored for a total of 49 nights from mid-December 2014 to early-March 2015. The observations are made with three KMTNet (Korea Microlensing Telescope Network) 1.6 m telescopes installed in Chile, South Africa, and Australia. Multiple frequency analysis is applied to the data and resulted in clear detection of seven frequencies without an alias problem: five known frequencies and two new ones with small amplitudes of 1.2-1.7 mmag. The amplitudes of all but one frequency are significantly different from previous results, confirming the existence of long-term amplitude changes. We examine the variations in pulsation timings of V1162 Ori for about 30 years by using the times of maximum light obtained from our data and collected from the literatures. The O − C (Observed minus Calculated) timing diagram shows a combination of a downward parabolic variation with a period decreasing rate of (1/P)dP/dt = −4.22 × 10⁻⁶ year⁻¹ and a cyclic change with a period of about 2780 days. The most probable explanation for this cyclic variation is the light-travel-time effect caused by an unknown binary companion, which has a minimum mass of 0.69 M_⊙. V1162 Ori is the first δ Sct-type pulsating star of which the observed fast period decrease can be interpreted as an evolutionary effect of a pre-main sequence star, considering its membership of the Orion OB 1c association.