• Journal of Astronomy and Space Sciences
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• 제32권1호
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• pp.51-62
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• 2015

I investigated a method for drawing the star chart in the planisphere Cheonsang-yeolcha-bunyajido. The outline of the star chart can be constructed by considering the astronomical information given in the planisphere alone and the drawing method described in Xin-Tangshu; further the chart can be completed by using additional information on the shape and linking method of asterisms out of an inherited star chart. The circles of perpetual visibility, the equator, and the circle of perpetual invisibility are concentric, and their common center locates the Tianshu-xing, which was defined to be a pole star in the Han dynasty. The radius of the circle of perpetual visibility was modified in accordance with the latitude of Seoul, whereas the other circles were drawn for the latitude of $35^{\circ}$, which had been the reference latitude in ancient Chinese astronomy. The ecliptic was drawn as an exact circle by parallel transference of the equator circle to fix the location of the equinoxes at the positions recorded in the epitaph of the planisphere. The positions of equinoxes originated from the Han dynasty. The 365 ticks around the boundary of the circle of perpetual invisibility were possibly drawn by segmenting the circumference with an arc length instead of a chord length with the ratio of the circumference of a circle to its diameter as accurate as 3.14 presumed. The 12 equatorial sectors were drawn on the boundary of the star-chart in accordance with the beginning and ending lodge angles given in the epitaph that originated from the Han dynasty. The determinative lines for the 28 lunar lodges were drawn to intersect their determinative stars, but seven determinative stars are deviated. According to the treatises of the Tang dynasty, these anomalies were inherited from charts of the period earlier than the Tang dynasty. Thus, the star chart in Cheonsang-yeolcha-bunyajido preserves the old tradition that had existed before the present Chinese tradition reformed in approximately 700 CE. In conclusion, the star chart in Cheonsang-yeolcha-bunyajido shows the sky of the former Han dynasty with the equator modified to the latitude of Seoul.

• 정보처리학회논문지C
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• 제11C권5호
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• pp.645-652
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• 2004

본 논문에서는 대역폭과 지연 파라미터를 참조하여 PG내의 토폴로지 정보를 하는 기법으로 라인 세그먼트를 이용하여 경계노드 사이의 다중 경로 정보를 하였다. 제안된 star 토폴로지 기법에서는 모든 경로를 찾는 대신 홉 카운트 기반의 깊이 우선 방식을 사용하여 효율적으로 다중 경로를 탐색할 수 있도록 하였다. 이를 위해 토폴로지 정보를 줄이고 다중링크 에 유연성을 부여하기 위하여 대역폭과 지연의 한 쌍으로 구성된 두 개의 라인 세그먼트를 이용하는 수정된 라인 세그먼트 기법을 제안하였다. 그리고, 이를 기존의 star 토폴로지에 적용한 효율적인 토폴로지 기법을 제안하였다. 제안된 기법의 성능을 평가하기 위해 기존의 star 기법과 호 성공율, 접근시간 및 크랭크 백율에 대하여 컴퓨터 시뮬레이션을 통해 비교 분석하였다. 시뮬레이션 분석결과 제안된 star TA 기법이 기존의 기법보다 성능이 향상됨을 알 수 있었다.

• 부동산연구
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• 제24권1호
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• pp.7-14
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• 2014

본 연구는 2006년 1월부터 2013년 6월까지의 서울시 아파트 개별 실거래가격에 대한 시공간 자료로 시공간자기상관의 문제를 헤도닉가격결정모형에 의한 통상최소자승법(OLS), 시간효과를 고려한 시간자기회귀모형(TAR), 공간효과를 고려한 공간자기회귀모형(SAR)과 시공간자기회귀모형(STAR)을 이용해 아파트 가격 추정결과를 비교분석하였다. 실증분석결과, STAR모형이 기존의 OLS에 비해 수정결정계수가 약 10% 증가하였으며, 추정오차는 약 18% 감소한 것으로 나타나 시공간효과를 고려했을 때 아파트 가격 추정이 기존모형에 비해 정확함을 알 수가 있었다. STAR모형 분석결과, 아파트 매매가격에 전용면적(-), 아파트연수(-), 저층더미(-), 개별난방(-), 도시가스(-), 재건축더미(+), 계단식(+), 단지규모(+)등이 영향을 주는 것으로 나타났으며 다른 분석방법론과도 대부분 같은 부호를 나타냈다. 시공간자기회귀모형을 이용해 부동산 가격을 추정시 정부 당국자는 부동산시장의 동향을 정확히 파악해 정책을 수립 집행해 정책효율을 높을 수 있고 투자자의 입장에서는 객관적인 정보를 바탕으로 합리적 투자를 할 수 있다.

• 천문학회지
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• 제54권1호
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• pp.17-35
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• 2021

We study galaxies undergoing ram pressure stripping in the Virgo cluster to examine whether we can identify any discernible trend in their star formation activity. We first use 48 galaxies undergoing different stages of stripping based on H i morphology, H i deficiency, and relative extent to the stellar disk, from the VIVA survey. We then employ a new scheme for galaxy classification which combines H i mass fractions and locations in projected phase space, resulting in a new sample of 365 galaxies. We utilize a variety of star formation tracers, which include g - r, WISE [3.4]-[12] colors, and starburstiness that are defined by stellar mass and star formation rates to compare the star formation activity of galaxies at different stripping stages. We find no clear evidence for enhancement in the integrated star formation activity of galaxies undergoing early to active stripping. We are instead able to capture the overall quenching of star formation activity with increasing degree of ram pressure stripping, in agreement with previous studies. Our results suggest that if there is any ram pressure stripping induced enhancement, it is at best locally modest, and galaxies undergoing enhancement make up a small fraction of the total sample. Our results also indicate that it is possible to trace galaxies at different stages of stripping with the combination of H i gas content and location in projected phase space, which can be extended to other galaxy clusters that lack high-resolution H i imaging.

• 대한수학회보
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• 제37권4호
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• pp.755-764
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• 2000

We introduce a new class of functions $H_{\kappa}({\beta})$ which is related to close-to-star functions and we derive a few geometric properties for the class $H_{\kappa}({\beta}),{\;}(2{\leq}k{\kappa}{\leq}4)$.

• 충청수학회지
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• 제11권1호
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• pp.53-58
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• 1998

In this paper we study (positive) implicativeness of $BCK^{\star}(X^{\star})$, and investigate some properties of ideals in $BCK^{\star}(X)$.

• 대한환경공학회지
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• 제28권10호
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• pp.983-986
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• 2006

• Journal of applied mathematics & informatics
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• 제28권5_6호
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• pp.1507-1518
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• 2010

In this article some generalized refinements of some inequalities for real quasi-cinvex, convex, concave, s-convex, s-concave, and $\alpha$-star s-convex mappings are obtained.

• 충청수학회지
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• 제26권2호
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• pp.403-409
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• 2013

In [20] and [22], the author proved that the union of two linear star-configurations in $\mathbb{P}^2$ of type $t{\times}s$ with $3{\leq}t{\leq}10$ and $t{\leq}s$ has generic Hilbert function. In this paper, we prove that the union of two linear star-configurations in $\mathbb{P}^2$ of type $t{\times}s$ with $3{\leq}t$ and $({a\atop2})-1{\leq}s$ has also generic Hilbert function.

• 천문학논총
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• 제27권4호
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• pp.331-334
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• 2012

We investigate the role of galaxy environment in the evolution of individual galaxies through the AKARI observations of the merging galaxy cluster A2255. MIR diagnostics using N3-S11 colors are adopted to select star-forming galaxies and galaxies in transition between star-forming galaxies and quiescent galaxies. We do not find particular enhancement of star formation rates as a function of galaxy environment, reflected in cluster-centric distance and local surface density of galaxies. Instead, the locations of intermediate MIR-excess galaxies (-1.2 < N3 - S11 < 0.2) show that star-forming galaxies are transformed into passive galaxies in the substructures of A2255, where the local surface density of galaxies is relatively high.