• 천문학회보
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• 제40권2호
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• pp.39.3-40
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• 2015

The NISS (Near-infrared Imaging Spectrometer for Star formation history) onboard NEXTSat-1 is the near-infrared instrument optimized to the first small satellite of NEXTSat series. The capability of both imaging and low spectral resolution spectroscopy in the near-infrared range is a unique function of the NISS. The major scientific mission is to study the cosmic star formation history in local and distant universe. For those purposes, the main targets are nearby galaxies, galaxy clusters, star-forming regions and low background regions. The off-axis optical design of the NISS with two linear variable filters is optimized to have a wide field of view ($2deg.{\times}2deg.$) as well as the wide wavelength range from 0.95 to $3.8{\mu}m$. The mechanical structure is considered to endure the launching condition as well as the space environment. The dewar inside the telescope is designed to operate the infrared detector at 80K stage. From the thermal analysis, we confirmed that the telescope and the dewar can be cooled down to around 200K and 80K, respectively in order to reduce the large amount of thermal noise. The stray light analysis is shown that a light outside a field of view can be reduced below 1%. After the fabrications of the parts of engineering qualification model (EQM), the NSS EQM was successfully assembled and integrated into the satellite. To verify operations of the satellite in space, the space environment tests such as the vibration, shock and thermal-vacuum test were performed. Here, we report the results of the critical design review for the NISS.

• 천문학회보
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• 제41권2호
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• pp.64.3-65
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• 2016

The NISS (Near-infrared Imaging Spectrometer for Star formation history) is the near-infrared instrument optimized to the Next Generation of small satellite series (NEXTSat). The capability of both imaging and low spectral resolution spectroscopy in the near-infrared range is a unique function of the NISS. The major scientific mission is to study the cosmic star formation history in local and distant universe. For those purposes, the main observational targets are nearby galaxies, galaxy clusters, star-forming regions and low background regions. The off-axis optical design is optimized to have a wide field of view ($2deg.{\times}2deg.$) as well as the wide wavelength range from 0.95 to $3.8{\mu}m$. Two linear variable filters are used to realize the imaging spectroscopy with the spectral resolution of ~20. The mechanical structure is considered to endure the launching condition as well as the space environment. The compact dewar is confirmed to operate the infrared detector as well as filters at 80K stage. The electronics is tested to obtain and process the signal from infrared sensor and to communicate with the satellite. After the test and calibration of the engineering qualification model (EQM), the flight model of the NSS is assembled and integrated into the satellite. To verify operations of the satellite in space, the space environment tests such as the vibration, shock and thermal-vacuum test were performed. Here, we report the test results of the flight model of the NISS.

• 전자공학회논문지
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• 제53권4호
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• pp.27-34
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• 2016

철도 차량은 일렬로 연결되는 구조적 특수성이 있으므로 네트워크 토폴로지를 구성하는 경우에서도 이를 고려하여야 한다. 또한 차량 내의 장치 간 연결에서의 토폴로지와 차량 간 연결에서의 토폴로지를 구분하여야 한다. 차량 간 연결에 있어서 기존의 링, 스타, 데이지체인, 버스 등의 토폴로지 대신 이를 조합한 하이브리드 토폴로지가 제안되었다. 이는 일렬로 연결된 철도 차량을 적절한 수의 그룹으로 묶고 그룹 내에서는 스타 네트워크 토폴로지로 구성하고 그룹 간 연결은 데이지체인 네트워크 토폴로지로 구성하는 방식이다. 이를 통해 하이브리드 토폴로지는 스타 토폴로지에 비해 차량 간 연결에 필요한 케이블의 수를 절감하고도 적절한 전송 속도를 유지할 수 있다. 하이브리드 토폴로지는 스타와 데이지 체인 두 가지 토폴로지를 절충하는 방식이므로 각각의 장점을 잘 활용할 수 있도록 그룹 내 차량의 수를 적절히 선정하는 것이 중요하다. 본 논문에서는 철도차량에서 최적의 하이브리드 네트워크 토폴로지를 구하는 것을 목적으로 한다. 이를 위해 차량 별로 데이터 생성 크기와 생성 주기가 동일하다는 가정 하에 차량 간 연결에서의 최대 케이블 수와 전송 속도에 대하여 각각 가중치를 별도로 두고 가중치 별로 전체 차량 수에 따른 최적의 그룹 내 차량의 수를 도출한다.

• Journal of Astronomy and Space Sciences
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• 제33권3호
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• pp.185-196
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• 2016

New multiband BVRI light curves of NSVS 1461538 were obtained as a byproduct during the photometric observations of our program star PV Cas for three years from 2011 to 2013. The light curves indicate characteristics of a typical W-subtype W UMa eclipsing system, displaying a flat bottom at primary eclipse and the O'Connell effect, rather than those of an Algol/b Lyrae eclipsing variable classified by the northern sky variability survey (NSVS). A total of 35 times of minimum lights were determined from our observations (20 timings) and the SuperWASP measurements (15 ones). A period study with all the timings shows that the orbital period may vary in a sinusoidal manner with a period of about 5.6 yr and a small semi-amplitude of about 0.008 day. The cyclical period variation can be interpreted as a light-time effect due to a tertiary body with a minimum mass of 0.71 M_⊙. Simultaneous analysis of the multiband light curves using the 2003 version of the Wilson-Devinney binary model shows that NSVS 1461538 is a genuine W-subtype W UMa contact binary with the hotter primary component being less massive and the system shows a low mass ratio of q(m_c/m_h)=3.51, a high orbital inclination of 88.7°, a moderate fill-out factor of 30 %, and a temperature difference of ΔT=412 K. The O'Connell effect can be similarly explained by cool spots on either the hotter primary star or the cool secondary star. A small third-light corresponding to about 5 % and 2 % of the total systemic light in the B and V bandpasses, respectively, supports the third-body hypothesis proposed by the period study. Preliminary absolute dimensions of the system were derived and used to look into its evolutionary status with other W UMa binaries in the mass-radius and mass-luminosity diagrams. A possible evolution scenario of the system was also discussed in the context of the mass vs mass ratio diagram.

• 한국엔터테인먼트산업학회논문지
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• 제14권2호
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• pp.1-14
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• 2020

본 연구는 싸이 이후 더 확대된 K-Pop 시장에서 BTS의 선호요인이 특징적으로 무엇인지를 밝혀보고자 하는 관심에서 시작되었다. 본 연구의 목적을 위해 국내를 비롯해 BTS가 인기를 끌고 있는 대만, 태국, 베트남을 대상으로 설문조사를 시행하였다. 본 연구의 결과를 살펴보면 BTS 선호요인 전체에 대해 베트남과 태국이 가장 긍정적인 인식을 하는 것으로 나타났고, 가장 높은 정(+)의 영향을 미치는 요인은 BTS의 차별적 감각으로 분석되었다. 본 연구가 동남아와 한국 팬들을 대상으로 하여 폭넓은 설문조사 대상자를 통한 확대된 연구이며, BTS 선호요인에 대한 새로운 시각에서의 규명이 가능했다는 의의에도 불구하고, 팬덤효과와 구매의도에 영향을 미칠 수 있는 다양한 변수를 고려하지 못하고, 세계적으로 더 많은 팬을 확보하고 있는 미국, 유럽 지역 팬들에 대한 의식조사를 함께하지 못한 점이 본 연구의 한계가 될 수 있을 것이다.

• 천문학회보
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• 제46권1호
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• pp.57.2-57.2
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• 2021

Variability in Young Stellar Objects (YSOs) can be caused by time-dependent accretion rates, geometric changes in the circumstellar disks, the stochastic hydromagnetic interactions between stellar surfaces and inner disk edges, reconnections within the stellar magnetosphere, and hot/cold spots on stellar surfaces. We uncover ~1400 variables from a sample of ~5300 YSOs in nearby low-mass star-forming regions using mid-IR light curves obtained from the 5.5-years NEOWISE All Sky Survey. The mid-IR variability traces a wide range of dynamical, physical, and geometrical phenomenon. We classify six types of YSO variability based on their light curves: secular variability (Linear, Curved, Periodic) and stochastic variability (Burst, Drop, Irregular). YSOs in earlier evolutionary stages have higher fractions of variables at all types and higher amplitudes for the variability. Along with brightness variability, we also find a diverse range of secular color variations, which can be attributed to a competitive interplay between the variable accretion luminosity of the central source and the variable extinction by material associated with the accretion process. We compare the variability of known FUors/EXors and VeLLOs/LLSs, which represent two extreme ends (burst versus quiescent) of the episodic accretion process; FUors/EXors have a higher fraction of variables (65%) than VeLLOs/LLSs (41%). Short-term (few day) and long-term (decades) variability, as well as possible AGB contamination in the YSO catalogues, are also discussed.molecules become more complex by surface chemistry induced directly by high energy photons or by the thermal energy diffused over heated grain surface. Therefore, the ice composition is an

• 한국지구과학회지
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• 제37권7호
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• pp.389-397
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• 2016

${\delta}$ Scuti형 변광성 BO Lyn의 파장에 따른 광도곡선 차이를 알아보기 위해서 보현산천문대의 1.8m 반사망원경과 적외선 검출기 KASINICS를 이용한 측광 관측을 수행하였다. 2011년 3월 26일부터 4월 1일까지 총 7일간의 관측 자료로 J, H, Ks필터 광도곡선을 얻어 기존에 보고된 V필터에서의 광도곡선과 비교하여 주기, 극대점, 진폭, 형태에 대한 차이를 알아보았다. 적외선 광도곡선의 주기 분석 결과 단일 주파수해 $f_1=10.712cycle/day$, 주기$P=0.09335{\pm}0.00002days$의 값을 얻었으며, 파장에 따른 주기의 차이는 나타나지 않았다. 적외선에서는 $2f_1$에 해당하는 주파수가 검출되었는데, 이는 고진폭 ${\delta}$ Scuti형 변광성의 특징인 비대칭적인 광도곡선의 형태를 잘 설명해준다. 극대점의 위치를 비교한 결과 계산된 V필터의 예상 극대점보다 관측된 적외선 극대점이 전체 주기의 약 0.3에 해당하는 만큼 더 늦게 나타났다. 진폭은 ${\Delta}J/{\Delta}V=0.328$, ${\Delta}H/{\Delta}V=0.216$, ${\Delta}Ks/{\Delta}V=0.211$로 파장이 길어질수록 변광의 폭이 더 작게 나타났다. 파장에 따른 극대점의 지연과 변광폭의 차이는 맥동변광성의 밝기 변화가 주로 온도변화에 기인하기 때문인 것으로 여겨진다.

• 가정과삶의질연구
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• 제27권3호
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• pp.201-212
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• 2009

The purpose of research is to investigate patterns and diffusion of consumer participation on Internet UCC based on digital contents services. A sample survey of internet users was conducted, responses were collected from 629 respondents and consumer streaming data were analyzed. Some of the practical implications of the results are follows. Research can find out that patterns of user participation in UCC. The major genres of UCC are like daily lives of individuals, humors, parodies of star entertainers and types of contents like still pictures or images, texts are relatively highly generated comparing with multimedia UCC. Although participants have been being increased in UCC recently, the consumers as prosumers who are classified in contents generating group are ten percents at the most. In generating community-based UCC such as posting answers of questions and activities in Blog, prosumers who are in contents making group(recreational group) show more positive attitudes than simple participants(consuming only). The results of multiple regression analysis indicated that fun & entertainment, arousal, self-expression, user friendly web interface variable commonly posited a significant effect in multimedia UCC Services between two groups. Information sharing and perceived usefulness posited a significant effect in recreational group.

• Journal of Astronomy and Space Sciences
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• 제28권1호
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• pp.9-12
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• 2011

Results of an analysis of 11 nights of R-filter CCD photometry data of an intermediate polar MU Camelopardalis (MU Cam) obtained at the Korean 1.0 m telescope at Mt. Lemmon are reported. After checking the spin period with our data, $P_{spin}=0.^d01373801(59)$, we compiled the reported data of maxima timing and an O-C diagram analysis has been carried out to understand the spin period variation. A significant spin period variation was detected, and fitting the O-C points to a cubic parabola led to an ephemeris of $BJD_{max}=2453682.4178(94)+0.0137380(13)E-2.07(55){\times}10^{-11}E^2+2.28(52){\times}10^{-15}E^3$. The torque experienced by the magnetic compact star accreting in a disk is estimated as ${\tau}{\approx}1.815{\times}10^{35}gcm^2/s^2$ in a simple approximation in order to show how important monitoring the period variation is. Thus we conclude that monitoring the long-term spin period variation will help to understand the physical condition of magnetic compact stars.

• 한국조리학회지
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• 제12권3호
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• pp.201-218
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• 2006

This research has attempted to asses the relationship between trust management, the element of service discretion act, and the quality of the service. The research model and assumption have been set up based on such a theoretical research and the demonstrative analysis of the customer-encountering employees of five-star hotels in Seoul. The results of the study are as follows; First, the rationalization of management can be achieved by improving the service through having a command of trust management as a management strategy. Second, there has been significant differences between variables such as the degree of importance and accomplishment of trust management. And it tells us that it is necessary to improve the range of service discretion acts up to the level where the difference between importance and accomplishment is not in existence. Third, the variable changes according to demographic characteristics show us the necessity of providing individualized education by recognizing the differences among groups. Fourth, the trust management has a considerable effect on the quality of the service, and this indicates that the quality of the service can be improved through expanding the range of service discretion acts of customer-encountering employees.