• 한국습지학회지
• /
• 제17권3호
• /
• pp.251-263
• /
• 2015

본 연구에서는 L-moment ratio diagram 기법과 지형정보시스템(GIS)을 동시에 활용하여 우리나라의 지속기간별 연 최대강우량의 최적확률밀도함수를 판별하는 새로운 기법을 제안하고, 결과 도출과정에 있어 발견된 연최대강우량의 통계값의 흥미로운 지형학적 특성을 살펴보았다. 이를 위하여 우리나라 기상청에서 운영하는 67개의 강우관측지점에서 관측된 강우자료의 연최대강우량을 1시간, 3시간, 6시간, 12시간, 24시간 누적시간에 대하여 산출하고, L-moment ratio diagram 기법을 활용하여 이들에 대한 최적확률밀도함수를 구한 후, 이를 관측지점에 해당하는 티센 다각형에 다른 색상으로 표현하여 그 공간적 분포를 살펴보았다. 또한, 각 후보 확률밀도함수의 적합도에 대한 지도를 작성하였다. 본 연구의 결과를 요약하면 다음과 같다: (1) 강우의 극한값의 특성을 대표할 수 있는 통계값인 L-skewness와 L-kurtosis는 뚜렷한 공간적 경향을 띠고 있다. 특히 산맥을 포함한 우리나라의 지형적 특성에 큰 영향을 받았다. 이는 발생빈도가 높고 강도가 낮은 평상시의 강우사상뿐 만 아니라, 연최대강우량 또한 지형의 영향을 크게 받는다는 것을 의미한다; (2) 우리나라의 산악지역에서는 연최대강우량의 통계적 특성에 대한 고도의 영향이 비산악지역보다 더 크며, 고도가 높은 지역일수록 발생 빈도가 낮고 강도가 강한 강우사상이 더 자주 발생하며, 강우의 누적기간이 증가할수록 이러한 경향은 작아졌다; (3) 우리나라의 연최대강우량을 가장 잘 대변할 수 있는 확률밀도함수는 Generalized Extreme Value (GEV) 분포와 Generalized Logistic (GLO) 분포이다. 단, 남해안의 중앙지역에 대해서는 Generalized Pareto (GPA) 분포가 가장 적합한 것으로 나타났다.

• 천문학회지
• /
• 제48권6호
• /
• pp.343-355
• /
• 2015

There is much observational evidence that active star formation is taking place in the Hii regions Sh 2-255 – 257. We present a photometric study of this star forming region (SFR) using imaging data obtained in passbands from the optical to the mid-infrared, in order to study the star formation process. A total of 218 members were identified using various selection criteria based on their observational properties. The SFR is reddened by at least E(B −V ) = 0.8 mag, and the reddening law toward the region is normal (R_V = 3.1). From the zero-age main sequence fitting method it is confirmed that the SFR is 2.1 ± 0.3 kpc from the Sun. The median age of the identified members is estimated to be about 1.3 Myr from a comparison of the Hertzsprung-Russell diagram (HRD) with stellar evolutionary models. The initial mass function (IMF) is derived from the HRD and the near-infrared (J, J −H) color-magnitude diagram. The slope of the IMF is about Γ = −1.6 ± 0.1, which is slightly steeper than that of the Salpeter/Kroupa IMF. It implies that low-mass star formation is dominant in the SFR. The sum of the masses of all the identified members provides the lower limit of the cluster mass (169M_⊙). We also analyzed the spectral energy distribution (SED) of pre-main sequence stars using the SED fitting tool of Robitaille et al., and confirm that there is a significant discrepancy between stellar mass and age obtained from two different methods based on the SED fitting tool and the HRD.

• 한국해양공학회지
• /
• 제1권1호
• /
• pp.104-110
• /
• 1987

Fatigue tests by axial loading (R = 0.05) were carried out to investigate fatigue crack growth characteristics of small surface cracks in 2 1/4 Cr-1 Mo steel at room temperature by using flat specimens with a small artificial pit. All the data of the fatigue crack growth rate obtained in the present test are determined as a function of the stress intensity factor range about a semi-elliptical crack, so that the application of linear fracture mechanics to the surface fatigue crack growth and to the fatigue crack growth into depth, and all the data obtained from tests were discussed in comparison with the data of Type 304 stainless steel and two type of mild steel under the same test conditions. The obtained results are as follows: 1)When the cycle ratios are same, surface fatigue crack length and its depth are almost same and fall within a narrow scatter band in spite of different stress levels. 2)Relations of the surface fatigue crack growth rate (da/dN) and fatigue crack growth rate into depth (db/dN) to its stress intensity factor range ($\Delta K_{Ia}, \Delta K_{Ib}$) can be plotted as a straight line at log-log diagram without dependence of stress level and coincide with the data of part-through crack in various steels.

• 천문학회보
• /
• 제35권1호
• /
• pp.51.1-51.1
• /
• 2010

We present the interim results of simultaneous observations of SiO and H2O masers toward 401 known stellar SiO and/or H2O maser sources (166 both SiO and H2O maser sources, 83 only SiO maser sources, and 152 only H2O maser sources) using KVN_Yonsei telescope. The results of 166 known SiO/H2O maser sources will be presented by Kim et al. and the results of 83 only SiO maser sources and 152 only H2O maser sources presented here. Both SiO and H2O maser emission were detected from 30 sources giving a detection rate of 36 % toward known 83 only SiO maser sources, while they were detected from 66 sources giving a detection rate of 43 % toward known 152 only H2O maser sources at one epoch observation. Only SiO masers were detected from 42 sources toward 83 only SiO sources, while they were detected from 28 sources toward 152 only H2O sources. Characteristics of these observed sources in the IRAS two-color diagram is investigated including mutual relations between SiO and H2O maser emission. In addition, these results will be useful for statistical study of late-type stars and future VLBI observations.

• 천문학회보
• /
• 제43권1호
• /
• pp.60.2-60.2
• /
• 2018

We present the near infrared JHK photometric properties and the spatial distribution of red supergiants(RSGs) of NGC 3623, NGC 3627 and NGC 3628 in the Leo Triplet system using the data obtained with 3.8m UKIRT(United Kingdom Infra-Red Telescope) at Hawaii. We checked interaction between the three galaxies by making a spatial density map of RSGs. From (J-K,K)0 Color-Magnitude Diagram which include resolved stars in three galaxy and control field with PARSEC isochrone, we figured out the RSG candidates of the Leo triplet are at 0.9<(J-K)0<1.2, mK<17.5 and separated them from background and foreground sources. Using gaussian kernel density estimation, we drew spatial density map of RSGs in the Leo triplet with an assumption that all RSGs are an identical population. The density map shows extended features of NGC 3628 to NGC 3627 along the declination direction. The asymmetries between NGC 3627 and NGC 3628 might be evidence for that the distribution of actual star components(RSGs) follows the neutral hydrogen distribution and also for interaction between two galaxies. And the extended features along the right ascension direction might be a supporting evidence for the existence of a TDG(Tidal Dwarf Galaxy). In case of NGC 3623, we could not see any sign of interaction in density map.

• 천문학회보
• /
• 제36권2호
• /
• pp.145.2-145.2
• /
• 2011

We present the results of simultaneous observations of SiO v = 1, 2, J = 1-0, $^{29}SiO$ v = 0, J = 1-0, and $H_2O$ $6_{16}-5_{23}$ maser lines toward 152 known $H_2O$-only maser sources (the sources which are previously detected only in the 22 GHz $H_2O$ maser emission) using Yonsei and Tamna 21-m radio telescopes of the Korean VLBI Network from 2009 June to 2011 January. Both SiO and $H_2O$ maser emission were detected from 62 sources giving a detection rate of 40.8 %. SiO-only maser emission was detected from 27 sources, while $H_2O$-only maser was detected from 22 sources. We have identified 19 new detections of SiO maser emission for previous non-detection sources and 51 new detections of SiO maser for previously not observed sources. Characteristics of all observed sources in the IRAS two-color diagram is investigated including their evolutionary sequence and mutual relations between SiO and $H_2O$ maser emission. These observational results will be useful for statistical study of asymptotic giant branch (AGB) stars and future VLBI observation.

• 천문학회보
• /
• 제36권2호
• /
• pp.70.1-70.1
• /
• 2011

We have investigated properties of merging galaxies in the nearby universe, using Sloan Digital Sky Survey (SDSS) DR7. We first constructed two galaxy samples according to redshift range: Sample 1 for 0 ${\leq}$ z ${\leq}$ 0.025 and Sample 2 for 0.09 ${\leq}$ z ${\leq}$ 0.1. We then identified 118 and 184 merging galaxies among the galaxies in the Sample 1 and 2, respectively, and classified them into different merging types and stages by visual inspection of galaxy images. In the Sample 1, there are more wet mergers than dry mergers, while most merging galaxies in the Sample 2 are dry mergers. The color-magnitude diagram of the merging galaxies in our samples is comparable to that of normal galaxies. Dry mergers tend to locate in the red sequence, while wet and mixed mergers reside mostly in the blue cloud. Unlike some previous studies, we did not find a clear trend that the merger rate increases at higher redshift. However, it is difficult to make a direct comparison of the merger rate found in different studies, because it depends on the number of observed galaxies and criteria for merger classification. From the ratios of emission lines, we infer that the faction of merging galaxies with AGNs is higher in wet mergers than in other types.

• 천문학회보
• /
• 제37권2호
• /
• pp.240.1-240.1
• /
• 2012

We performed simultaneous observations of SiO v=1, 2, $^{29}SiO$ v=0, J=1-0 and $H_2O$ $6_{16}-5_{23}$ maser lines toward 252 OH/IR stars using the Korean VLBI Network 21m telescopes. The observations were carried out from 2011 November to 2012 July for studying SiO and $H_2O$ maser properties associated with the evolutionary stages of OH/IR stars. Both $H_2O$ and SiO masers were detected from 49 sources, one-side maser of SiO and $H_2O$ was detected from 109 and 11 sources, respectively. Mutual relations between SiO and $H_2O$ maser properties are investigated based on statistical analyses. We also investigate these maser properties in the IRAS two-color diagram related with stellar evolutionary sequence.

• 천문학회보
• /
• 제37권2호
• /
• pp.237.1-237.1
• /
• 2012

We report extensive statistical analyses based on the simultaneous observational results of SiO and $H_2O$ masers toward 166 known both SiO and $H_2O$ maser sources (Kim et al. 2010), 83 known SiO maser sources (Cho & Kim 2012 submitted), and 152 known $H_2O$ maser sources (Kim et al. 2012 in preparation). We investigate mutual relations between SiO and $H_2O$ maser properties (peak and total flux density ratios, full line width ratios, and velocity structures etc.) according to stellar pulsation phases and type of evolved stars. These statistical results are compared with monitoring observational results of some individual stars. In addition, a relation between the full line width of SiO/$H_2O$ masers and stellar mass loss rates is examined. For 401 observed stars, we also investigate characteristics of SiO and $H_2O$ maser properties related with evolutionary stages in the IRAS two-color diagram.

• 천문학회보
• /
• 제46권2호
• /
• pp.49.2-49.2
• /
• 2021

We present the results of long-term simultaneous monitoring observations (~ 12 years) of H²O (22 GHz) maser and several vibrationally excited lines of SiO J = 1-0, 2-1, 3-2 masers (43, 86, 129 GHz) carried out with the 21-m antennas of the Korean VLBI Network (KVN) toward a sample of three AGB stars (RT Vir, RR Aql, IRC-10151) that are believed to be semiregular variable star, Mira variable star, and OH/IR star, respectively, according to a sequential evolutionary phase of AGB star. A total 10 transitions were observed, of which we detected H²O, SiO 𝝊 = 1 and 2, J = 1-0, SiO 𝝊 = 1, J = 2-1 and J = 3-2 maser lines in all three target objects, depending on the observational epochs. In this study, we scrutinize the evolutionary traits of each target object based on the maser line profiles, flux/velocity variations, and phase lags with the optical light curves. The IRAS two color diagram and the infrared spectral energy distributions (SEDs) in the wavelength range from 1.2 to 240 ㎛ of three observed sources were also analyzed.