• 전자통신동향분석
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• 제8권4호
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• pp.143-156
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• 1993

ISDN 을 구축하기 위한 망구조로 ISDN 의 다양한 서비스 수용 관점에서 Single Star 형 망구조가 가장 잠재력이 우수한 구조로 평가되고 있으며 Single Star 형 구조로 구축될 때 High Count Optical Fiber Cable 과 광커넥터 (단심, 다심) 가 요구된다. 그중 광커넥터는 광 가입자 망의 구축을 위해 필수적인 부품으로서 기술 추세는 다심화, 복합 기능화, 소형화, 저가격화, 고성능화, 고신뢰성화의 방향으로 진행되고 있다. 본 고에서는 향후 국내에서 적용 가능한 광케이블용 다심 광커넥터 개발을 위하여 외국에서 개발되어 있는 제품의 정렬원리, 정렬 구조 및 제조기술을 분석하였으며 또한 국내의 수요를 분석하였다. 수요 분석은 과거의 생산 실적 자료가 없는 이유로 정량적 분석법보다는 전화 가입자 수요 자료와 가입자 선로의 광케이블 계획, 그리고 광 CATV 가입자 예측 자료를 이용한 정성적인 방법을 적용하였다.

• 천문학회보
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• 제41권1호
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• pp.70.1-70.1
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• 2016

NGC 4402 is a spiral galaxy located in the Virgo cluster. It is undergoing active HI gas stripping due to the strong ICM pressure, showing evidence for recent quenching of star formation. Its CO disk is also highly disturbed as HI, yet unlike HI disk, no sign of significant molecular gas stripping is found. Aiming to better understand how atomic gas stripping and disturbed molecular gas result in star formation quenching, we probe properties of molecular gas in the densest forms. As a pilot study, we observed HCN (1-0) and HCO+ (1-0) in the center of NGC 4402 using one of the Korean VLBI Network (KVN) antennas located at Yonsei site. In this work, we present the result from the KVN single-dish observations and discuss its implications.

• 천문학회지
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• 제54권6호
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• pp.171-182
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• 2021

The lack of short baselines, referred to as the short-spacing problem (SSP), is a well-known limitation of the performance of radio interferometers, causing a reduction of the flux detected from source structure on large angular scales. The very large number of antennas operated in the Atacama Large Millimeter/sub-millimeter Array (ALMA) generates situations for which the impact of the SSP takes a complex form, not simply measurable by a single number, such as the maximal recoverable scale. In particular, extended antenna configurations, complemented by a small group of closeby antennas at the centre of the array, may result in a double-humped baseline distribution with a significant gap between the two groups. In such cases one should adopt as the effective maximal recoverable scale the one associated with the extended array and use only the central array to recover missing flux, as one would do with single dish or ACA (Atacama Compact Array) observations. The impact of the missing baselines can be very important and may easily be underestimated, or even overlooked. The present study uses ALMA archival data of the ²⁹SiO(8-7) line emission of the AGB star W Hydrae for a demonstration. A critical discussion of the reliability of the observations away from the star is presented together with comments of a broader scope. Properties of the circumstellar envelope of W Hya within ~15 au from the star, many of which are not mentioned in the published literature, are briefly described and compared with R Doradus, an AGB star having properties very similar to W Hya.

• 한국전산구조공학회:학술대회논문집
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• 한국전산구조공학회 2000년도 봄 학술발표회논문집
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• pp.85-91
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• 2000

The smallest value of the load when the equilibrium condition becomes to be unstable is defined as the buckling load. The primary objective of this paper is to analyse stability boundaries for star dome under combined loads and is to investigate the iteration diagram under the independent loading parameter In numerical procedure of the geometrically nonlinear problems, Arc Length Method and Newton-Raphson iteration method is used to find accurate critical point(bifurcation point and limit point). In this paper independent loading vector is combined as proportional value and star dome was used as numerical analysis model to find stability boundary among load parameters and many other models as multi-star dome and arches were studied. Through this study we can find the type of buckling mode and the value of buckling load.

• 천문학회보
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• 제38권2호
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• pp.67.1-67.1
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• 2013

It has been known that HCN is one of ubiquitous high-density gas tracer, and the abundance ratio between HCN and its Isomer, HNC sensitively depends on kinetic temperature in star-forming regions. Here we investigate the molecular abundance ratio toward three different evolutionary phases of massive star formation: Infrared Dark Clouds, High-mass Protostellar Objects and Ultracompact HII Regions. We obtained the abundances of HCN and HNC using optically thin H13CN and HN13C lines observed with the KVN single-dish telescopes and MAMBO 1.2mm and SCUBA $850{\mu}m$ continuum data. According to our results, the ratio of [HCN]/[HNC] increases statistically with the evolutionary stage, indicative of the effect of temperature. We also found a strong anti-correlation between the column density of molecular hydrogen and the HNC abundance.

• 천문학논총
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• 제30권2호
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• pp.93-97
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• 2015

How high-mass stars form is currently unclear. Calculations suggest that the radiation pressure of a forming star can halt spherical infall, preventing further growth when it reaches $10M_{\odot}$. Two major theoretical models on the further growth of stellar mass have been proposed. One model suggests the merging of less massive stellar objects, and the other is through accretion, but with the help of a disk. Inflow motions are key evidence for how forming stars gain further mass to build up massive stars. Recent developments in technology have boosted the search for inflow motion. A number of high-mass collapse candidates were obtained with single dish observations, and mostly showed blue profiles. Infalling signatures seem to be more common in regions which have developed radiation pressure than in younger cores, which is the opposite of the theoretical prediction and is also very different from observations of low mass star formation. Interferometer studies so far confirm this tendency with more obvious blue profiles or inverse P Cygni profiles. Results seem to favor the accretion model. However, the evolution of the infall motion in massive star forming cores needs to be further explored. Direct evidence for monolithic or competitive collapse processes is still lacking. ALMA will enable us to probe more detail of the gravitional processes.

• 천문학회보
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• 제40권2호
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• pp.58.4-59
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• 2015

We have performed single dish and VLBI monitoring observations of $H_2O$ and SiO masers toward the semi-regular variable star R Crateris using the Korean VLBI Network(KVN) 4 band receiving system. In the case of VLBI observations at 3 epochs, successful superposed maps of $H_2O$ and SiO masers were obtained on 2015 May by adopting the Source Frequency Phase Referencing(SFPR) method. These results enable us to investigate the development of outflow and asymmetric motions from SiO maser to $H_2O$ maser regions according to stellar pulsation which are closely related with a mass-loss process. Single dish monitoring observations were carried out from 2009 June to 2015 May. Intensity variations between $H_2O$ and SiO masers were investigated according to stellar phases together with peak velocity variations. We will compare the VLBI results with those of single dish.

• KSII Transactions on Internet and Information Systems (TIIS)
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• 제10권3호
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• pp.1052-1070
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• 2016

Wireless Body Area Networks (WBANs) have received a lot of attention as a promising technology for medical and healthcare applications. A WBAN should guarantee energy efficiency, data reliability, and low data latency because it uses tiny sensors that have limited energy and deals with medical data that needs to be timely and correctly transferred. To satisfy this requirement, many multi-radio multi-channel MAC protocols have been proposed, but these cannot be implemented on current off-the-shelf sensor nodes because they do not support multi-radio transceivers. Thus, recently single-radio multi-channel MAC protocols have been proposed; however, these methods are energy inefficient due to data duplication. This paper proposes a TDMA-based single-radio, multi-channel MAC protocol that uses the Unbalanced Star+Mesh topology to satisfy the requirements of WBANs. Our analytical analysis together experiments using real sensor nodes show that the proposed protocol outperforms existing methods in terms of energy efficiency, reliability, and low data latency.

• 천문학회보
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• 제41권1호
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• pp.43.1-43.1
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• 2016

With the Korean VLBI Network (KVN), both single dish and VLBI monitoring observations of H2O and SiO masers were performed toward the semi-regular variable star R Crateris. In the case of 11 VLBI monitoring observations from Jan. 5, 2014 to Jan. 7, 2016, successful superposed maps of H2O and SiO masers were obtained at 7 epochs by adopting the Source Frequency Phase Referencing (SFPR) method. These results enable us to investigate the development of outflow and asymmetric motions from SiO maser to H2O maser regions according to stellar pulsation which are closely related with a mass-loss process. Single dish monitoring observations of H2O and SiO masers were also carried out from 2009 June to 2016 Feb. Intensity variations between H2O and SiO masers were investigated according to stellar optical phases together with peak velocity variations with respect to the stellar velocity. We will compare the VLBI results among different maser transitions with those of single dish.

• 천문학회보
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• 제41권2호
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• pp.46.3-46.3
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• 2016

We present the ALMA Cycle 2 results "Two New SiO Maser Sources in High-Mass Star-Forming Regions" which was published in the Astrophysical Journal (Vol. 826, P157, 2016). Silicon monoxide (SiO) masers are rare in star forming regions, with the exception of five known SiO maser sources. However, we detected two new SiO maser sources from infrared loud clumps of the high-mass star forming regions G19.61-0.23 and G75.78+0.34 using the KVN single dish. High angular resolution observations with ALMA and JVLA toward G19.61-0.23 suggest that the deeply embedded young stellar object (YSO) of SMA 1 is powering the SiO masers. In addition, the SiO v=1, J=1-0 line shows four spike features while the v=2 maser shows combined features of one spike and broad wing components, implying energetic activities of the YSO of SMA 1 in the G19.61-0.23 hot molecular core. The SiO v=0, J=2-1 emission shows bipolar outflows in NE-SW direction with respect to the center of the SiO maser source. A high angular resolution map of the SiO v=1, J=2-1 maser in G75.78+0.34 shows that the SiO maser is associated with the CORE source at the earliest stage of high-mass star formation. Therefore, the newly detected SiO masers and their associated outflows will provide good probes for investigating this early high-mass star formation.