• 천문학회보
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• 제44권2호
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• pp.35.3-35.3
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• 2019

The new era of multi-messenger astronomy (MMA) has arrived in 2017 with the detection of the binary neutron star merger in both gravitational wave (GW) and electromagnetic radiation (EM). Now, the new run of GW detectors are providing numerous GW events and the number GW events are expected to increase dramatically in future as the GW sensitivities improve. When the GW studies are combined with EM counterpart observations, a great synergy is expected in many areas of study such as the physical process following the compact object merger, the environment of such events (and galaxy evolution), and cosmology, Therefore, it has now become crucial to identify and characterize these GW events in optical/IR EM. In the past, we have been performing optical/NIR observation of GW events using a worldwide network of more than 10 telescopes, and are getting more actively involved in MMA of GW sources. In this talk, we will present our network of telescopes, the EM follow-up observation results of GW events including GW170817 and the O3 events in 2019, and the current issues in MMA. We will also give the future prospects of MMA, showing the forecast for the GW events and the outlook of EM MMA observations.

• 천문학회보
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• 제46권1호
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• pp.27.4-28
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• 2021

Since the first direct detection of the gravitational waves in 2015, more than 50 events coming from the merging of compact binaries composed of black holes and neutron stars have been observed. The simultaneous detection of gravitational waves and electromagnetics waves from the merging of neutron stars opened up multi-messenger astronomy. The forthcoming observations with better sensitivity by the network of ground based detectors will enrich the gravitational wave source populations and provide valuable information regarding stellar evolution, dynamics of dense stellar systems, and star formation history across the cosmic time. The precision of the Hubble constant from the distance measurement of gravitational sources will improve with more binary neutron star events are observed together with the aftweglows. I will also briefly cover the expected scientiic outcomes from the future detectors that are sensitive to much lower frequenies than current detectors.

• Journal of Astronomy and Space Sciences
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• 제12권1호
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• pp.21-29
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• 1995

$\beta$ Lyrae형 식쌍성 AW Cam을 UBV 세파장 영역에서 광전 관측하여 얻은 UBV 광도곡선을 Wilson and Devinney 쌍성 모델의 2가지 mode( mode 2와 mode 5)로 분석하였다. 이는 Russo and Milano (1983)가 산출한 측광 질량비(q=0.21)와 Mammano et al. (1967)의 분광질량비(q=0.43)가 일치하지 않는 모순-AW Cam 계의 남아 있는 문제인-올 해결하기 위한 것이다. Mode 2로 구한 측광학적 해가 mode 5로 구한 해보다 관측된 광도곡선을 더 잘 반영하는 것으로 계산되었다. 이는AW Cam이 정상준분리형계가 아나라 분리형 쌍성계임을 제시하는 것으로 해석될 수 있다. 또한 산출한 질량비 (q=0.43)로 계산한 AW Cam계의 삼차원 로쉬 모형을 보면 가벼운 반성은 안쪽 로쉬 한계면에 잘 들어 있는 반연 더 무거운 주성이 로쉬 한계면에 거의 접촉하고 있다. 로쉬 기하, 공전주기의 일정성, 그리고 다른 측광학적 증거들로 부터 AW Cam은 Giuricin and Mardrossian (1981)이 제안한 ‘접촉이 깨진 상태’에 있는 진화된 분리형 쌍성계가 아니라, ‘접촉 상태’로 가고 있는case A 진화 상 태에 있는 덜 진화된 분리형 쌍성계로 잠정적으로 결론짓는다

• 분석과학
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• 제9권2호
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• pp.161-167
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• 1996

이성분계 첨가물을 이용한 카드뮴 석출과 수소 생성의 상대족인 속도를 조절할 수 있는 가능한 방법에 대하여 조사하였다. 수소를 발생하는 물의 전기환원을 억제하는 소수성 필름을 형성할 수 있는 벤질 알코올을 첨가제 중의 하나로 선택하였다. 다른 한 가지 첨가제는 카드뮴(II) 이온의 친수성을 약화시킴으로써 소수성 벤질 알코올 필름층을 쉽게 가로질러 환원극에 전착시킬 수 있는 것을 선택하였다. 전압 전류 효율 연구로부터 이온쌍과 착물 첨가제가 벤질 알코올 필름 존재하에서 카드뮴의 환원을 촉진시킬 수 있다는 것을 확인하였다. 벤질 알코올 필름은 나트륨 이온과 카드뮴의 염화착물을 형성하는 이온쌍을 얻기에 충분하도록 전극 주위의 유전상수를 낮추고, 카드뮴의 환원을 촉진시킨다. 이러한 환원의 촉진은 염화물이 존재하지 않는 황산염 용액에서는 일어나지 않는다. 왜냐하면 카드뮴은 본래 아쿠아 착물과 이온쌍으로 존재하여 카드뮴의 환원을 촉진시키지 못하고 환원을 방해시키기 때문이다.

• 정보보호학회논문지
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• 제23권5호
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• pp.885-896
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• 2013

사람이 개입할 필요 없이 기기 및 사물들을 셀룰러 망(cellular network)으로 연결하여 언제 어디서나 다양한 서비스를 제공하는 MTC(Machine Type Communications)는 차세대 통신의 주요 이슈로 고려되고 있다. 현재, 다수의 MTC 단말들이 동시적으로 망에 접속하려고 하면 각 MTC 단말들은 독립적인 접근 인증 절차를 수행해야 된다. 이로 인해 LTE-Advanced 네트워크에서 인증 시그널링(authentication signaling) 혼잡(congestion)과 부하(overload)의 문제가 야기된다. 본 논문은 그룹 기반의 인증 프로토콜과 키 관리 프로토콜을 제안한다. 그룹 단위로 MTC 단말들을 관리하기 위해 제안하는 프로토콜은 그룹 리더(leader)를 선출하고, 리더만이 코어 망(core network)과의 인증에 참여한다. 인증이 완료된 후, 그룹 리더는 이진트리(binary tree)를 구성하여 나머지 구성원(member)들과 MME(Mobility Management Entity)를 관리한다. 마지막으로 제안 프로토콜 분석은 제안하는 프로토콜이 MTC 단말들과 코어 망 사이에서 발생되는 인증 시그널링을 줄여줄 수 있을 뿐만 아니라 효율적으로 MTC 단말들을 관리할 수 있음도 보여준다.

• 천문학논총
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• 제30권2호
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• pp.585-586
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• 2015

4U 1323-62, a low mass X-ray binary with an orbital period of 2.94 hr, exhibits periodic X-ray dips, which are due to absorption by the bulge of the outer accretion disk. The purpose of this study is to search for orbital period changes using archived X-ray data over a time span of 20 years. We present our preliminary results from analyzing light curves observed by RXTE, BeppoSAX, XMM-Newton and Suzaku. We used the method proposed by Hu et al. (2008) to estimate dip center time and adopted the Observed - Calculated method to measure changes in period. We obtained an orbital period of 2.941917(36) hr and a period derivative of $\dot{P}_{orb}/P_{orb}=(-9.9{\pm}3.5){\times}10^{-7}yr^{-1}$. The F-test result shows that the quadratic ephemeris is describes the evolution of the dip phases better than the linear ephemeris at a greater than 95% confidence level. More X-ray data collected from the early 80s will be included to further refine the orbital ephemeris.

• 천문학논총
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• 제30권2호
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• pp.605-607
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• 2015

The development of time-frequency analysis techniques allow astronomers to successfully deal with the non-stationary time series that originate from unstable physical mechanisms. We applied a recently developed time-frequency analysis method, the Hilbert-Huang transform (HHT), to two non-stationary phenomena: the superorbital modulation in the high-mass X-ray binary SMC X-1 and the quasi-periodic oscillation (QPO) of the AGN RE J1034+396. From the analysis of SMC X-1, we obtained a Hilbert spectrum that shows more detailed information in both the time and frequency domains. Then, a phase-resolved analysis of both the spectra and the orbital profiles was presented. From the spectral analysis, we noticed that the iron line production is dominated by different regions of this binary system in different superorbital phases. Furthermore, a pre-eclipse dip lying at orbital phase ~0:6-0:85 was discovered during the superorbital transition state. We further applied the HHT to analyze the QPO of RE J1034+396. From the Hilbert spectrum and the O-C analysis results, we suggest that it is better to divide the evolution of the QPO into three epochs according to their different periodicities. The correlations between the QPO periods and corresponding fluxes were also different in these three epochs. The change in periodicity and the relationships could be interpreted as the change in oscillation mode based on the diskoseismology model.

• 천문학회지
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• 제50권3호
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• pp.51-59
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• 2017

The presence of blue stragglers pose challenges to standard stellar evolution theory, in the sense that explaining their presence demands a complex interplay between stellar evolution and cluster dynamics. In the meantime, mass transfer in binary systems and stellar collisions are widely studied as a blue straggler formation channel. We explore properties of the Galactic open clusters where blue stragglers are found, in attempting to estimate the relative importance of these two favored processes, by comparing them with those resulting from open clusters in which blue stragglers are absent as of now. Unlike previous studies which require a sophisticated process in understanding the implication of the results, this approach is straightforward and has resulted in a supplementary supporting evidence for the current view on the blue straggler formation mechanism. Our main findings are as follows: (1) Open clusters in which blue stragglers are present have a broader distribution with respect to the Z-axis pointing towards the North Galactic Pole than those in which blue stragglers are absent. The probability that two distributions with respect to the Z-axis are drawn from the same distribution is 0.2%. (2) Average values of $log_10(t)$ of the clusters with blue stragglers and those without blue stragglers are $8.58{\pm}0.232$ and $7.52{\pm}0.285$, respectively. (3) The clusters with blue stragglers tend to be relatively redder than the others, and are distributed broader in colors. (4) The clusters with blue stragglers are likely brighter than those without blue stragglers. (5) Finally, blue stragglers seem to form in condensed clusters rather than simply dense clusters. Hence, we conclude that mass transfer in binaries seems to be a relatively important physical mechanism of the generation of blue stragglers in open clusters, provided they are sufficiently old.

• Smart Structures and Systems
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• 제15권5호
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• pp.1373-1392
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• 2015

Placing sensors at appropriate locations is an important task in the design of an efficient structural health monitoring (SHM) system for a large-scale civil structure. In this paper, a hybrid optimization algorithm called virus monkey algorithm (VMA) based on the virus theory of evolution is proposed to seek the optimal placement of sensors. Firstly, the dual-structure coding method is adopted instead of binary coding method to code the solution. Then, the VMA is designed to incorporate two populations, a monkey population and a virus population, enabling the horizontal propagation between the monkey and virus individuals and the vertical inheritance of monkey's position information from the previous to following position. Correspondingly, the monkey population in this paper is divided into the superior and inferior monkey populations, and the virus population is divided into the serious and slight virus populations. The serious virus is used to infect the inferior monkey to make it escape from the local optima, while the slight virus is adopted to infect the superior monkey to let it find a better result in the nearby area. This kind of novel virus infection operator enables the coevolution of monkey and virus populations. Finally, the effectiveness of the proposed VMA is demonstrated by designing the sensor network of the Canton Tower, the tallest TV Tower in China. Results show that innovations in the VMA proposed in this paper can improve the convergence of algorithm compared with the original monkey algorithm (MA).

• 천문학논총
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• 제30권2호
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• pp.175-178
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• 2015

Due to the lack of an accretion disk in a polar (magnetic cataclysmic variable, MCV), the material transferred from the secondary is directly accreted onto the white dwarf, forming an accretion stream and a hot spot on the white-dwarf component. During the eclipses, different light components can be isolated. Therefore, the monitoring of eclipsing polars could provide valuable information on several modern astrophysical problems, e.g., CVs as planetary hosting stars, mass transfer and mass accretion in CVs, and the magnetic activity of the most rapidly rotating cool dwarfs. In the past five years, we have monitored about 10 eclipsing polars (e.g., DP Leo and HU Aqr) using several 2-m class telescopes and about 100 eclipse profiles were obtained. In this paper, we will introduce the progress of our research group at YNOs. The first direct evidence of variable mass transfer in a CV is obtained and we show that it is the dark-spot activity that causes the mass transfer in CVs. Magnetic activity cycles of the cool secondary were detected and we show that the variable mass transfer is not caused by magnetic activity cycles. These results will shed light on the structure and evolution of close binary stars (e.g., CVs and Algols).