• 대한교통학회지
• /
• 제22권1호
• /
• pp.43-62
• /
• 2004

전통적으로 기종점 OD행렬을 추정하는 방법은 가구통행조사나 노측면접조사를 실시하여 표본조사한 자료의 전수화 과정을 거쳐 기종점 OD행렬표를 작성한다. 조사 과정에서 조사표본수가 증가함에 따라 시간과 비용 및 조사오차가 수반되는 문제로 인하여 많은 제약이 내포되어 있다. 이러한 제약을 극복하기 위해 관측교통량을 이용하여 기종점 OD행렬을 추정하는 기법을 연구해 오고 있다 관측교통량으로 기종점 OD행렬을 추정하는 기법 중 gradient 모형은 가장 일반적으로 많이 이용하는 기법중의 하나다. 그러나 gradient모형을 이용하여 관측교통량으로 기종점 OD행렬을 추정한 결과 관측교통량과 추정교통량의 오차는 최소화시키면서 기종점 OD행렬을 추정하지만 사전(prior) 기종점 OD행렬의 OD행렬 구조를 유지하지 못할 경우가 많다. 즉 사전 기종점 OD행렬의 통행특성을 변경시키는 단점이 있다. 따라서 본 연구에서는 추정된 기종점 OD행렬은 사전 기종점 OD행렬의 OD행렬 구조를 반영하면서 관측교통량과 추정교통량의 오차를 최소화시켜주도록 하는 기종점 OD행렬 추정모형을 개발하기 위하여 Conjugate Gradient 알고리즘을 이용하였다. 개발된 모형을 검증하기 위하여 예제 분석가로망에서 모형의 일관성(일치성)을 분석하였다. 일관성 분석결과 모형의 상위수준(upper level)과 하위수준(lower level)이 내부적으로 유기적인 관계를 유지하고 있는 것으로 분석되었다. 또한 관측링크교통량에 관측오차를 반영하여 기종점 OD행렬의 추정력을 분석하였다. 분석결과는 관측교통량과 추정(배정)교통량의 오차는 허용오차 범위내에서 추정되는 것으로 분석되었고 추정된 기종점 OD행렬의 OD행렬 구조는 사전 기종점 OD행렬의 OD행렬 구조를 유지하는 것으로 분석되었다.른 지원이 필요하다. 이와 같은 철도화물활성화의 정책수립필요성의 배경에는 철도화물수송이 효율성과 환경친화성, 높은 안전성 등 사회적 비용을 감소시키는 장점을 가지고 때문이다. 철도화물운송회사도 현재의 수송기능과 함께 포워더로서의 기능을 가져야 할 것이며, 운임인하노력과 속도향상을 위한 노력을 계속하여야 할 것이다.적 대안경로 집합을 역추적 생성하는 과정을 단계별로 추가 설명하였다.을 받지 않은 시추공의 자료는 사용하였다 이러한 온천 주변 지역이라 하더라도 실제는 온천의 pumping 으로 인한 대류현상으로 주변 일대의 온도를 올려놓았기 때문에 비교적 높은 지열류량 값을 보인다. 한편 한반도 남동부 일대는 이번 추가된 자료에 의해 새로운 지열류량 분포 변화가 나타났다 강원 북부 오색온천지역 부근에서 높은 지열류량 분포를 보이며 또한 우리나라 대단층 중의 하나인 양산단층과 같은 방향으로 발달한 밀양단층, 모량단층, 동래단층 등 주변부로 NNE-SSW 방향의 지열류량 이상대가 발달한다. 이것으로 볼 때 지열류량은 지질구조와 무관하지 않음을 파악할 수 있다. 특히 이러한 단층대 주변은 지열수의 순환이 깊은 심도까지 가능하므로 이러한 대류현상으로 지표부근까지 높은 지온 전달이 되어 나타나는 것으로 판단된다.의 안정된 방사성표지효율을 보였다. $^{99m}Tc$-transferrin을 이용한 감염영상을 성공적으로 얻을 수 있었으며, $^{67}Ga$-citrate 영상과 비교하여 더 빠른 시간 안에 우수한 영상을 얻을 수 있었다. 그러므로 $^{99m}Tc$-transierrin이 감염 병소의 영상진단에 사용될 수 있을 것으로 기대된다.리를 정량화 하였다. 특히 선조체에서의 도파민 유리에 의한 수용체 결합능의

• 한국초등과학교육학회지:초등과학교육
• /
• 제37권3호
• /
• pp.323-338
• /
• 2018

The aims of this study are to develop the STEAM program focused '3D printing for respiratory system' and to ascertain its influence on elementary student's science process skills, creative problem solving abilities and scientific interest. The developed STEAM program was applied to 5th grade students of O elementary school located in J city. As a result of applying the STEAM program, the experimental group of the STEAM program class improved significantly in creative problem solving abilities and scientific interest than the control group of the theoretical class. The result of learner satisfaction survey of the STEAM program was high. Meanwhile, there was no significant difference in science process skills between the two groups. Therefore, the STEAM program class with the theme of '3D printing for respiratory system' could be meaningful works to encourage students' interest as well as their creative problem solving ability and scientific interest. In future, continuous and systematic studies on STEAM programs focused on 'structure and function of our body' are needed for elementary students' cognitive and affective developments.

• 한국주거학회:학술대회논문집
• /
• 한국주거학회 2008년도 춘계학술발표대회 논문집
• /
• pp.382-385
• /
• 2008

The purpose of this study is to analyse design characteristics of the boutique hotel guestrooms to formalize their internal design concepts, and to evaluate the emotional response to these concepts, focusing on the response of consumers to the current trend of designs. It seems to be important, therefore, that this study are able to provide basic information necessary to establish a successful design strategy from the viewpoint of design marketing. This study was carried out with the guestrooms of 'O' Hotel, located at Paju, Gyeonggi-do Province, Korea, that is considered to fully introduce the concepts of 'Boutique Hotel.' A preliminary survey was performed by taking pictures and visiting the field from the 17th to 19th day of January 2008. Based on its results, a questionnaire survey as a major survey was conducted using a slide show according to Semantic Differential Scale on March 5, 2008. The collected data was evaluated by 50 students who majored in interior architectural design at D college, and was analysed using the SPSS Package

• 천문학논총
• /
• 제30권2호
• /
• pp.99-101
• /
• 2015

Massive stars are some of the most influential objects in the Universe, shaping the evolution of galaxies, creating chemical elements and hence shaping the evolution of the Universe. However, the processes by which they form and how they shape their environment during their birth processes are not well understood. We use $NH_3$ data from "The $H_2O$ Southern Galactic Plane Survey" (HOPS) survey to define the positions of dense cores/clumps of gas in the southern Galactic plane that are likely to form stars. Then, using data from "The Millimetre Astronomy Legacy Team 90 GHz" (MALT90) survey, we search for the presence of infall and outflow associated with these cores. We subsequently use the "3D Molecular Line Radiative Transfer Code" (MOLLIE) to constrain properties of the infall and outflow, such as velocity and mass flow. The aim of the project is to determine how common infall and outflow are in star forming cores, and therefore to provide valuable constraints on the timescales and physical process involved in massive star formation. Preliminary results are presented here.

• 천문학논총
• /
• 제30권2호
• /
• pp.211-214
• /
• 2015

We investigated the period variation for 79 eclipsing binary systems using 20 years (1990-2009) of EROS, Macho, and OGLE survey observations. We discovered 9 apsidal motions, 8 mass transfers, 5 period increasing and decreasing systems, 12 light-travel-time effects, 5 eccentric systems and 40 other systems showing no period variations. We select 3 representative eclipsing binary systems; EROS 1052 for apsidal motion, EROS 1056 for mass transfer, and EROS 1037 for the light-travel-time effect. We determine the period variation rate (dP/dt), orbital parameters of the 3rd body (e3, ${\omega}_3$, $f(m_3)$, $P_3$, $T_3$), apsidal motion parameters ($d{\omega}/dt$, U, Ps, Pa, e) and apsidal motion period by analyzing the light curves and O-C diagrams.

• 천문학회보
• /
• 제44권2호
• /
• pp.51.1-51.1
• /
• 2019

At the commissioning phase of KVN from 2009 to 2013, single-dish survey and monitoring observations were performed toward about 1000 evolved stars and about 60 relatively strong SiO and H2O maser sources respectively. Based on these single-dish results and VLBI feasibility test observations at K/Q/W/D bands in 2014, KVN Key Science Project (KSP) has started from 2015 and will be completed in 2019 as KSP phase I. Here we present the overview of observational studies on evolved stars using KVN. In KSP phase I, we have focused on nine KSP sources which show a successful astrometrically registered maps of SiO and H2O masers using the source frequency phase referencing method. We aim at investigating the spatial structure and dynamical effect from 43/42/86/129 GHz SiO to 22 GHz H2O maser regions associated with a stellar pulsation and development of asymmetry in circumstellar envelopes. Using the combined network KaVA (KVN+Japanese VLBI network VERA), KaVA Large Program titled on "Expanded Study on Stellar Masers: ESTEMA Phase I" was performed from 2015 to 2016. Based on ESTEMA Phase I, EAVN Large Program titled on "EAVN Synthesis of Stellar Maser Animations: ESTEMA Phase II" was also performed from 2018. The ESTEMA II project aims to publish composite animations of circumstellar H2O and SiO masers, which taken from up to 6 long-period variable stars with a variety of the pulsation periods (333-1000 days). The animations will exhibit the three-dimensional kinematics of the maser gas clumps with complexity caused by stellar pulsation-driven shock waves and anisotropy of clump ejections from the stellar surface. Adding three EAVN telescopes (Tianma 65m, Nanshan 26m and NRO 45m telescopes) with KaVA always secures the high quality of the maser image frames through the monitoring program.

• 천문학회보
• /
• 제42권2호
• /
• pp.79.2-79.2
• /
• 2017

To dynamically and chemically understand how filaments, dense cores, and stars form under different environments, we are conducting a systematic mapping survey of nearby molecular clouds using the TRAO 14 m telescope with high ($N_2H^+$ 1-0, $HCO^+$ 1-0, SO 32-21, and $NH_2D$ v=1-0) and low ($^{13}CO$ 1-0, $C^{18}O$ 1-0) density tracers. The goals of this survey are to obtain the velocity distribution of low dense filaments and their dense cores for the study of their origin of the formation, to understand whether the dense cores form from any radial accretion or inward motions toward dense cores from their surrounding filaments, and to study the chemical differentiation of the filaments and the dense cores. Until the 2017A season, the real OTF observation time is ~760 hours. We have almost completed mapping observation with four molecular lines ($^{13}CO$ 1-0, $C^{18}O$ 1-0, $N_2H^+$ 1-0, and $HCO^+$ 1-0) on the six regions of molecular clouds (L1251 of Cepheus, Perseus West, Polaris South, BISTRO region of Serpens, California, and Orion B). The cube data for $^3CO$ and $C^{18}O$ lines were obtained for a total of 6 targets, 57 tiles, 676 maps, and $7.1deg^2$. And $N_2H^+$ and $HCO^+$ data were added for $2.2deg^2$ of dense regions. All OTF data were regridded to a cell size of 44 by 44 arcseconds. The $^{13}CO$ and $C^{18}O$ data show the RMS noise level of about (0.1-0.2) K and $N_2H^+$ and $HCO^+$ data show about (0.07-0.2) K at the velocity resolution of 0.06 km/s. Additional observations will be made on some regions that have not reached the noise level for analysis. To identify filaments, we are using and testing programs (DisPerSE, Dendrogram, FIVE) and visual inspection for 3D image of cube data. A basic analysis of the physical and chemical properties of each filament is underway.

• Ocean and Polar Research
• /
• 제26권2호
• /
• pp.199-205
• /
• 2004

$SiO_2$ and CaO are added to decrease the smelting temperature in the reduction-smelting method for manganese nodule processing. These elements are components of the manganese nodules and might be very important controlling factors in the processing due to the locally variable content. The 707 chemical data of manganese nodules acquired from 1994 to 2001 in KODOS(Korea Deep Ocean Survey) area were used for the hierarchical cluster analysis. The chemical data were classified by the morphological types, and the averages of the chemical data for each station were classified by the facies groups and the localities. All data are plotted on the $SiO_2-CaO-MnO$ phase diagram at $1773^{\circ}K$ to compare with the best compositional area in the nodule smelting. Variations and distributions of $SiO_2$ and CaO in KODOS nodules were also reviewed. The mineral phases assigned by the cluster analysis are CFA(Carbonate Fluorapatite), Fe-oxide, Al-silicate, and Mn-oxide. MnO contents are generally higher than $SiO_2$ contents in most of the morphological types except for the Is- and It-type. The Dt- and Tt-type show wider range and the E-types show high anomaly in their CaO contents. The stations which belong to facies group A and B show generally higher MnO contents than $SiO_2$ contents, however, the stations of facies group C and D show wide range in their MnO and $SiO_2$ contents. It seems to be very important to control the $SiO_2$ contents in the processing because of the wide range in the northern area. The additions of approximately 10 wt.% CaO and 10 wt.% $SiO_2$ are recommended for the northern area, whereas, the additions of approximately 10 wt.% CaO and 20 wt.% $SiO_2$ are recommended for the southern area.

• 천문학회보
• /
• 제42권1호
• /
• pp.32.1-32.1
• /
• 2017

To dynamically and chemically understand how filaments, dense cores, and stars form under different environments, we are conducting a systematic mapping survey of nearby molecular clouds using the TRAO 14 m telescope with high ($N_2H^+$ 1-0, $HCO^+$ 1-0, SO 32-21, and $NH_2D$ v=1-0) and low ($^{13}CO$ 1-0, $C^{18}O$ 1-0) density tracers. The goals of this survey are to obtain the velocity distribution of low dense filaments and their dense cores for the study of their origin of the formation, to understand whether the dense cores form from any radial accretion or inward motions toward dense cores from their surrounding filaments, and to study the chemical differentiation of the filaments and the dense cores. Until Feb. 2017, the real OTF observation time is 460 hours. We have almost completed mapping observation with four molecular lines ($^{13}CO$ 1-0, $C^{18}O$ 1-0, $N_2H^+$ 1-0, and $HCO^+$ 1-0) on the five regions of molecular clouds (L1251 of Cepheus, Perseus west, Polaris south, BISTRO region of Serpense, California, and Orion B). The maps of a total area of $7.38deg^2$ for both $^{13}CO$ and $C^{18}O$ lines and $2.19deg^2$ for both $N_2H^+$ and $HCO^+$ lines were obtained. All OTF data were regridded to a cell size of 22 by 22 arcseconds. The $^{13}CO$ and $C^{18}O$ data show the RMS noise level of about 0.22 K and $N_2H^+$ and $HCO^+$ data show about 0.14 K at the velocity resolution of 0.06 km/s. Additional observations will be made on some regions that have not reached the noise level for analysis. We are refining the process for a massive amount of data and the data reduction and analysis are underway. This presentation introduces the overall progress from observations to data processing and the initial analysis results to date.

• 한국수학교육학회지시리즈E:수학교육논문집
• /
• 제24권2호
• /
• pp.385-413
• /
• 2010

본 연구는 2007년 개정 수학과 교육과정의 목표에 새롭게 부각된 수학적 의사소통에 대한 중요성을 바탕으로 우리나라 초등학교에서 구현 가능한 수학적 의사소통 목표를 설정하기 위한 것이다. 구현 가능하도록 하기 위해 교사들이 이해하기 쉽도록 수학적 의사소통 유형을 전달방식에 따라 담화, 표현, 조작, 복합으로 구분하였으며, 학생 수준에 따른 수준별 교수 학습이 가능하도록 수학적 의사소통 유형별로 저 중 고학년에 따른 성취요소와 목표를 설정하였다. 성취요소와 목표 설정에 있어 타당성을 높이고자 전문가와 현장 교사들의 의견을 수렴하였다. 전문가와 교사 집단의 의견 중 각각 10%이상 부적절하다고 응답한 경우 판단 이유를 파악하여 삭제하거나 수정하였으나, 일부 특정 요소의 경우 국제적 동향이나 선행연구를 토대로 이상적인 목표로 문제가 없다고 판단될 경우 그대로 두거나 학년 이동만 한 것도 있다. 본 연구에서 설정된 초등학교 수학적 의사소통 성취요소와 목표는 수학교실에서 실질적으로 학생들의 다양한 수학적 의사소통을 돕고, 학생 수준을 파악하는데 큰 도움이 되길 기대한다.