• 천문학회보
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• 제44권1호
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• pp.69.2-69.2
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• 2019

Recent high resolution IR observations reveal that molecular clouds are filamentary and such a structure is ubiquitous over various star-forming environments, and it is clear that filaments play a crucial role in the formation of cores and stars. However, the formation process of dense cores in the filaments are still unknown. To investigate this issue in detail, we have carried out TRAO FUNS (TRAO survey of nearby Filamentary molecular clouds, the Universal Nursery of Stars) toward various star forming filamentary molecular clouds. In this presentation, we will report the first look results of filaments and dense cores in MCLD 123.5+24.9 and IC 5146, which are known as a quiescent, non-star-forming region and an active, high-mass star forming region, respectively. By comparing the kinematic properties of filaments and dense cores in different star forming environments, we verified the formation scenario of filaments and dense core, i.e., gravoturbulent fragmentation via supersonic motions.

• 천문학회보
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• 제43권2호
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• pp.51.2-51.2
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• 2018

Star clusters are important in understanding star formation. In star-forming regions, the number of stars with mass forms with an initial mass function (IMF), i.e. Chabrier, Salpeter, Kroupa, etc. In our simulations, initially sub-virial fractal star clusters evolve to become surviving sub-regions in strong tidal fields. We investigate the slope of the mass function (MF) of these sub-regions with time near the Galactic centre (GC). These sub-regions would appear to have a top-heavy IMF at ~ 2 Myr. Therefore, although our star-forming region near the GC has a normal IMF, stars in surviving 'clusters' can have a top-heavy 'IMF' due to the violent environment.

• 대한수학회지
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• 제56권3호
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• pp.645-667
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• 2019

It has been little known when an Artinian point quotient has the strong Lefschetz property. In this paper, we find the Artinian point star configuration quotient having the strong Lefschetz property. We prove that if ${\mathbb{X}}$ is a star configuration in ${\mathbb{P}}^2$ of type s defined by forms (a-quadratic forms and (s - a)-linear forms) and ${\mathbb{Y}}$ is a star configuration in ${\mathbb{P}}^2$ of type t defined by forms (b-quadratic forms and (t - b)-linear forms) for $b=deg({\mathbb{X}})$ or $deg({\mathbb{X}})-1$, then the Artinian ring $R/(I{\mathbb_{X}}+I{\mathbb_{Y}})$ has the strong Lefschetz property. We also show that if ${\mathbb{X}}$ is a set of (n+ 1)-general points in ${\mathbb{P}}^n$, then the Artinian quotient A of a coordinate ring of ${\mathbb{X}}$ has the strong Lefschetz property.

• 대한수학회지
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• 제58권2호
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• pp.283-308
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• 2021

In [30] the author finds a graded minimal free resolution of the 2-nd order symbolic power of a star configuration in ℙn of any codimension r. In this paper, we find that of any m-th order symbolic power of a star configuration in ℙn of codimension 2, which generalizes the result of Galetto, Geramita, Shin, and Van Tuyl in [15, Theorem 5.3]. Furthermore, we extend it to the m-th order symbolic power of a star configuration in ℙn of any codimension r for m = 3, 4, which also generalizes the result of Biermann et al. in [1, Corollaries 4.6 and 5.7]. We also suggest how to find a graded minimal free resolution of the m-th order symbolic power of a star configuration in ℙn of any codimension r for m ≥ 5.

• Kyungpook Mathematical Journal
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• 제61권1호
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• pp.23-32
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• 2021

Let D be an integral domain with quotient field K, X an indeterminate over D, ∗ a star operation on D, and Cl∗ (D) be the ∗-class group of D. The ∗w-operation on D is a star operation defined by I∗w = {x ∈ K | xJ ⊆ I for a nonzero finitely generated ideal J of D with J∗ = D}. In this paper, we study two star operations {∗} and [∗] on D[X] defined by A{∗} = ∩P∈∗w-Max(D) ADP [X] and A[∗] = (∩P∈∗w-Max(D) AD[X]P[X]) ∩ AK[X]. Among other things, we show that Cl∗(D) ≅ Cl[∗](D[X]) if and only if D is integrally closed.

• 한국우주과학회:학술대회논문집(한국우주과학회보)
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• 한국우주과학회 2011년도 한국우주과학회보 제20권1호
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• pp.19.2-19.2
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• 2011

In 1861 Nam Byeong-Gil published a book called as "Seonggyeong" which contains a star catalogue (NBGC) with the positions, magnitudes, and star maps for 1449 stars. The NBGC lists only the traditional Chinese stars selected from "the sequel to the Qing Dynasty Star Catalogue and Star Map." To identify each star from the NBGC with modern counterpart, we correct the positions of the Hipparcos stars brighter than 6.5 mag for proper motion, then precess the coordinates to the epoch of the NBGC. For each star in the NBGC, we find the nearest counterpart in the Hipparcos Catalogue (HC). If a much brighter star is at a slightly larger angular distance, we select that star as the secure counterpart. As a result, 95.5% of the stars in the NBGC were identified. We find a very good overall agreement of our results with a previous analysis by Ahn et al. (1996, Journal of the Korean History of Science Society, vol. I). For securely identified stars, we analyse its accuracy on the basis of comparison with data from the HC. The correlation of the errors between right ascensions and declinations is significantly deviated from spherical distribution. The magnitudes recorded in the NBGC correlate well with modern values. The accuracy of position decreases slowly with magnitude. Right ascensions and declinations have error distributions with ${\sigma}$ = 2.0' for the former while the latter with ${\sigma}$ = 1.6', but with much more errors >5' than expected for a Gaussian distribution.

• 컴퓨터교육학회논문지
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• 제13권5호
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• pp.91-102
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• 2010

스타 그래프는 노드 대칭성, 최대 고장 허용도, 계층적 분할 성질을 갖고, 하이퍼큐브보다 망 비용이 개선된 널리 알려진 상호 연결망이다. 본 연구에서는 스타 그래프와 그의 변형된 그래프들 상호 간의 임베딩 방법을 제안한다. 버블정렬 그래프가 팬케익 그래프와 스타 그래프에 각각 연장율 3, 확장율 1로 임베딩 가능함을 보이고, 팬케익 그래프가 버블정렬그래프에 임베딩 하는 연장율 비용이 O($n^2$)임을 보인다. 그리고 스타 그래프가 팬케익 그래프에 연장율 4, 확장율 1로 임베딩 가능함을 보인다. 또한 스타그래프를 버블정렬 그래프에, 팬케익 그래프를 스타 그래프에 임베딩 하는 연장율 비용이 각각 O(n)임을 보인다.

• 한국멀티미디어학회논문지
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• 제9권9호
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• pp.1173-1183
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• 2006

행렬-스타그래프와 팬케익 및 RFM 그래프는 스타 그래프가 갖는 좋은 성질을 가지면서 하이퍼큐브보다 망 비용이 적은 값을 갖는 상호연결망이다. 행렬-스타그래프는 스타그래프를 기본 모듈로 하여 노드 대칭성, 최대고장허용도, 계층적분할 성질을 갖고 스타그래프보다 망비용이 개선된 상호연결망이다. 본 논문에서는 그래프의 에지 정의를 이용하여 행렬-스타그래프, 팬케익그래프, RFM그래프 사이의 임베딩 방법을 제시한다. 행렬-스타그래프 $MS_{2,n}$은 팬케익그래프 $P_{2n}$에 연장율 4, 확장율 1, $RFM_{n}$그래프는 팬케익그래프 $P_n$에 연장율 2, 확장율 1, 그리고 행렬-스타그래프 $MS_{2,n}$을 $RFM_{2n}$으로 평균연장율 3에 임베딩 가능함을 보인다.

• 천문학회보
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• 제36권2호
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• pp.65-65
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• 2011

Early-type galaxies represent the end point of galaxy evolution and, despite pervasive residual star formation, are generally considered "red and dead", that is composed exclusively of old stars with no star formation. Here, their molecular gas content is constrained and discussed in relation to their evolution, supporting the continuing importance of minor mergers and/or cold gas accretion. First, as part of the Atlas3D survey, the first complete, large, volume-limited survey of CO in normal early-type galaxies is presented. At least of 23% of local early-types possess a substantial amount of molecular gas, the necessary ingredient for star formation, independent of mass and environment but dependent on the specific stellar angular momentum. Second, using CO synthesis imaging, the extent of the molecular gas is constrained and a variety of morphologies is revealed. The kinematics of the molecular gas and stars are often misaligned, implying an external gas origin in over a third of all systems, more than half in the field, while external gas accretion must be shot down in clusters. Third, many objects appear to be in the process of forming regular kpc-size decoupled disks, and a star formation sequence can be sketched by piecing together multi-wavelength information on the molecular gas, current star formation, and young stars. Fourth, early-type galaxies do not seem to systematically obey all our usual prejudices regarding star formation (e.g. Schmidt-Kennicutt law, far infrared-radio continuum correlation), suggesting a greater diversity in star formation processes than observed in disk galaxies and the possibility of "morphological quenching". Lastly, a first step toward constraining the physical properties of the molecular gas is taken, by modeling the line ratios of density- and opacity-sensitive molecules in a few objects. Taken together, these observations argue for the continuing importance of (minor) mergers and cold gas accretion in local early-types, and they provide a much greater understanding of the gas cycle in the galaxies harbouring most of the stellar mass. In the future, better dust masses and dust-to-gas mass ratios from Herschel should allow to place entirely independent constraints on the gas supply, while spatially-resolved high-density molecular gas tracers observed with ALMA will probe the interstellar medium and star formation laws locally in a regime entirely different from that normally probed in spiral galaxies.

• 한국지구과학회:학술대회논문집
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• 한국지구과학회 2010년도 춘계학술발표회 논문집
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• pp.118-119
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• 2010

별탄생에 관한 연구는 최근 천문학 영역에서 활발히 진행되고 있으며, 별이 실제로 동역학적 과정을 거쳐 형성되고 분자운의 난류적 특성에 강하게 영향을 받는다는 것을 보여주고 있다. 별탄생 과정에 관한 관측적 영역에서 상당한 진전이 있음에도 불구하고, 별탄생의 초기단계는 여전히 해결되고 있지 않다. 따라서, 별 탄생의 복잡한 역학적 특성으로 인해 컴퓨터 시뮬레이션은 별탄생 연구의 중요한 도구로 사용된다. 우리는 SPH 시뮬레이션을 활용하여 낮은 질량의 별 탄생 과정을 제시하였고, 가장 진보된 dragon code를 사용하였다. 질량과 난류, 중심 밀도 등의 값을 변화시키면서 내부 특성의 변화를 살펴보고, 어떻게 진화하는지에 대해 알아보고자 한다. (질량범위는 0.1$5\;M{\odot}$) 이 결과에 근거하여 그들의 환경조건과 특성 그리고 성간운에서 낮은 질량의 별이 탄생하는 동안 어떻게 진화하는지에 대해 논의하고자 한다.