• 한국가정과교육학회지
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• 제24권3호
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• pp.175-189
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• 2012

본 연구는 여고생들의 연예인 모방유형에 따라 외모관리행동 즉, 교복 변형행동, 헤어스타일 관리행동, 화장 관리행동 등에 미치는 영향을 조사하였다. 이를 위해 전북에 거주하는 여자고등학생 379명의 데이터가 사용되었고 신뢰도분석, 요인분석, 군집분석, 일원배치분산분석, 교차분석을 사용하여 분석하였다. 본 연구를 통하여 전북지역 여고생들은 연예인 모방유형에 따라 적극적 수행형, 심리적 욕구형, 연예인 호감형으로 분류되었다. 연예인 모방행동과 모방욕구의 평균이 가장 높았던 적극적 수행형 여고생들은 교복변형 경험이 가장 높았으며, 드라마속 연예인이 입고 나오는 교복스타일을 따라해 보고 싶어하고, 연예인 교복스타일로 교복을 변형한 경험이 있는 등 연예인 교복스타일에 많은 영향을 받았다. 또한 최신 유행헤어스타일을 인식하고 연예인의 헤어스타일을 선호하는 등 헤어스타일 관리행동에 더 적극적이었다. 그리고 매일 기초화장을 하고, 화장법을 배우고 싶어하는 등 화장 관리행동에 더 적극적임을 알 수 있었다. 반면 연예인 모방 행동과 모방욕구의 평균이 가장 낮았던 연예인 호감형 여고생들은 교복변형행동, 헤어스타일 관리행동, 화장 관리행동 등에 소극적임을 알 수 있었다. 따라서 청소년에게 바람직한 매스미디어에 관한 체계적인 교육을 실시하고, 교사들은 청소년들에게 합리적인 모방활동을 할 수 있도록 교육한다면 의생활지도에 있어서 효율적인 교육성과를 거둘 수 있을 것으로 보인다.

• 한국정보과학회논문지:시스템및이론
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• 제29권2호
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• pp.65-74
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• 2002

병렬 처리 시스템의 상호연결 네트워크로써 스타 그래프 구조간 그간 널리 사용되어 왔던 하이퍼규브에 비해 지름 및 차수 등의 특성에 우수한 성능을 보임으로 인해 최근 많은 연구자들의 관심을 받고 있다. 스타 그래프 네트워크에서 여러가지 통신문제들이 연구되어 지고 있는데 그러한 통신 문제 중 에 가장 기본이 될수있는 문제 중의 하나가 브로드캐스팅이다. 본 논문에서는 윕홀라우팅을 지원하는 스타 그래프 네트워크 시스템에서의 브로드캐스팅 문제를 다룬다. 윔홀라우팅을 사용하는 네트워크에서는 전송 노드간의 거리보다 전송 시 링크 충돌을 최소화하는 것이 전체 통신 시간을 줄이는 중요한 요소가 되는 데 본 논문에서는 스타 그래프 네트워크에서의 해밀 토니안 경로를 이용하여 링크 충돌이 없이 n 차원 스타 네트워크$([long_n n!]+1)$ 통신스텝이 전체 브로드캐스팅이 완료되는 알고리즘을 제시한다. 이는 이론 절 하한값 $([long_n n!]+1)$ 에 근접한 결과로 기존의 n-1 통신 스텝이 걸리는 알고리즘 보다 향상된 결과이다.

• 천문학논총
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• 제19권1호
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• pp.27-31
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• 2004

Through time-series CCD photometry using a 155mm refractor, we found a new $\delta$ Scuti type variable star, HD 235428, near a known bright $\delta$ Scuti type star, DQ Cep. We performed follow-up observations using a 61cm telescope at Sobaeksan Optical Astronomy Observatory. Four frequencies have been derived by multiple-frequency analysis, which are 15.804, 5.498, 15.351 and 24.516cycle $day^{-1}$, respectively. V-amplitude of HD 235428 is ${\Delta} V$ = 0.026.

• 유통과학연구
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• 제17권12호
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• pp.95-103
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• 2019

Purpose : Promoting startups has increased in importance in labor market policies since the economic crisis. In Korea, the Ministry of SMEs and Startups is also seeking to revitalize youth startups and traditional markets by moving young stores into idle spaces in traditional markets through 'Project to Support the Activation of Youth Mall'. Research into startups in traditional markets is very limited. Therefore, this study looks at the differences between the management performance of young merchants and senior merchants, and looks at the impact of the business period. Research design, data and methodology : It was divided into youth startup and senior startup based on the age of 40 and startup and nonstartup. Based on these criteria, the company intends to compare and analyze sales and margin rates by setting the sales and margin rates with the management performance of the startup and senior startups. In particular, to look at the feasibility of government funded projects for young merchants, the company will look at the changes in sales and margin rates of young merchants and senior merchants over the period of operation. In this study, the analysis was based on the raw data of the Statistics of traditional market in 2017, and the ANCOVA was used. Results : First of all, the sales volume of stores operated by young merchants, was higher than those operated by senior merchants. Next, the margin ratio does not differ from that of stores that are for young people and those. These findings suggest that the profit structure of stores in traditional markets is similar between young merchants and senior merchants. Third, if you look at the performance of new startups based on one year of business period in more detail, it turns out that young startups have improved in sales and margin rates since startups, while senior startups have no difference. Conclusions : While it means that management performance can be improved through support for young startups, it suggests that there is a limit to supporting senior startups. Therefore, this research indicates that the government support projects centered on youth can contribute to the revitalization of traditional markets.

• 한국통신학회논문지
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• 제31권9B호
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• pp.811-820
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• 2006

본 논문에서는 IEEE 802.15.4 MAC 프로토콜을 사용하는 스타 센서 네트워크에서 각각의 센서 노드에서 소모되는 전력을 분석 파라미터별로 연관성과 전력소모에 미치는 영향을 분석하였다. 성능분석을 위하여 데이터 전송과정에 소요되는 시간과 평균 송수신 전력랑으로 센서 노드 전력소모랑을 수식으로 전개하였으며, CSEM에서 제작한 WiseNET 시스템 측정값을 활용하였다. 모의실험결과 단일 센서 네트워크보다 10개의 센서 노드로 이루어진 센서 네트워크에서 전력소모가 평균 20% 증가 했으며, 비콘 신호 주기가 0.1초일 때 up-link가 down-link 보다 평균 2.5배 전력소모가 많았다. 비콘 신호 주기가 1초일 때 센서 노드 수가 100개로 증가하거나, 센싱 데이터가 100 byte로 증가하면 전력소모량이 약 2.3배 증가 하였으며, 868/915 MHz가 2.4 GHz보다 $6{\sim}12$배 전력소모량이 많았다.

• 천문학회보
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• 제40권2호
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• pp.40.3-41
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• 2015

We performed simultaneous observations of H2O and SiO masers toward VX Sgr using the Korean VLBI Network (KVN) and Source Frequency Phase Referencing (SFPR) method. The observations were carried out at 5 epochs from 2014 February to 2015 June. The relative locations of the SiO with respect to the H2O maser emission were determined at two epochs by SFPR for the first time. The H2O masers show well developed asymmetric outflow features which are spread up to ~300 mas in diameter. On the other hand, the SiO masers show a ring-like structure close to the central star with ~ 30 mas diameter. The SFPR observational results at two epochs (${\varphi}=0.83$ and 0.99) provide similar relative locations of H2O and SiO maser features. These superposed maps of H2O and SiO masers lead us to investigate the development of outflow motions from relatively spherical SiO maser regions close to central star to aspherical H2O maser regions according to optical phase of stellar pulsation together with the prediction of the position of central star.

• 천문학회보
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• 제39권1호
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• pp.84.1-84.1
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• 2014

We report the spatial distribution of early-type stars and pre-main-sequence (PMS) stars around the starburst type young open cluster Westerlund 2. The early-type were selected from UBVI photometric data, while the PMS members were identified from their X-ray emission and mid-infrared excess. The northern clump of the cluster is composed mainly of PMS stars detected in both optical and X-ray and seems to be coeval to the cluster, while PMS stars in the bright bridge region are highly obscured in optical wavelength. The bright bridge appear to be an on-going star forming region possibly triggered by the strong radiation field from both sides-massive stars in Westerlund 2 and WR 20b. We also found that there are many early-type stars not only in the cluster but also farther from the cluster up to several times of the cluster radius. These early-type stars are well aligned from east to southwest of the cluster. We conclude these early-type stars are members of an OB association in the RCW 49 nebula. This report indicates there is a complex star formation history in Westerlund 2 and its surrounding H II region, the RCW 49 nebula.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2009년도 한국우주과학회보 제18권2호
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• pp.29.3-29.3
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• 2009

Recent observations for the Galactic globular clusters (GCs) have shown that a number of GCs have characteristic features of multiple stellar populations, such as multiple main-sequences (MSs), splits in sub-giant branch (SGB), bimodal and/or extended horizontal branches (HBs). Based on the population synthesis models, we investigate star formation histories of the GCs with multiple populations, $\omega$ Cen, M54, NGC 1851, NGC 6388, NGC 6441, and NGC 2808, by comparing synthetic model color-magnitude diagrams (CMDs) with observations. We adopt most up-to-date Yonsei-Yale (Y2) stellar evolutionary tracks and isochrones from MS to post-HB, as well as improved color-temperature transformations from the recent stellar atmosphere libraries. Our models show that the observed features can be naturally explained by assuming the presence of helium-enhanced subpopulations.

• 천문학회지
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• 제29권2호
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• pp.107-117
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• 1996

We have studied the star forming activities and dust properties of Lynds 1251, a dark cloud located at relatively high galactic latitude. Eleven IRAS point sources identified toward Lynds 1251 are discussed. Estimate of stellar masses, and far-infrared lumnosities of the young stars associated with two prominent IRAS point sources imply that these are T-Tauri stars with masses smaller than $0.3 M_\bigodot$. The low dust temperature of 27 K and low ratio of FIR emission to hydrogen column density are probably due to the lack of internal heating sources. Presumably two low mass young stars do not have enough energy to heat up the dust and gas associated. The dust heating is dominated by the interstellar heating source, and the weaker interstellar radiation field can explain the exceptionally low dust temperatures found in Lynds 1251. The estimated dust mass of Lynds 1251 is just $\~1M_\bigodot$, or about 1/1000 of gas mass, which implies that there must be a substantial amount of colder dust. The infrared flux at $100{\mu}m$ is matching well with $^{13}CO$ peak temperature, while the $^{12}CO$ integrated intensity is matching with the boundary of dust emission. Overall, the dust properties of Lynds 1251 is similar to those of normal dark clouds even though it does have star forming activities.

• 천문학회보
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• 제46권2호
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• pp.37.3-38
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• 2021

One of the key questions on star formation is how the organic molecules are synthesized and delivered to the planets and comets since they are the building blocks of prebiotic molecules such as amino acid, which is thought to contribute to bringing life on Earth. Recent astrochemical models and experiments have explained that complex organic molecules (COMs; molecules composed of six or more atoms) are produced on the dust grain mantles in cold and dense gas in prestellar cores. However, the chemical networks and the roles of physical conditions on chemistry are not still understood well. To address this question, hot (> 100 K) cores in high mass young stellar objects (M > 8 Msun) are great laboratories due to their strong emissions and larger samples than those of low-mass counterparts. In addition, CH₃OH masers, which have been mostly found in high mass star forming regions, can provide constraints due to their very unique emerging mechanisms. We investigate twelve high mass star forming regions in ALMA band 6 observation. They are associated with 44/95 GHz Class I and 6.7 GHz Class II CH3OH masers, implying that the active accretion processes are ongoing. For these previously unresolved regions, 66 continuum peaks are detected. Among them, we found 28 cores emitting COMs and specified 10 cores associated with 6.7 GHz Class II CH3OH masers. The chemical diversity of COMs is found in cores in terms of richness and complexity; we identified up to 19 COMs including oxygen- and nitrogen-bearing molecules and their isotopologues in a core. Oxygen-bearing molecules appear to be abundant and more complex than nitrogen-bearing species. On the other hand, the COMs detection rate steeply grows with the gas column density, which can be attributed to the effective COMs formation in dense cores.