• 천문학회지
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• 제56권2호
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• pp.201-212
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• 2023

The inscription of Cheonsang Yeolcha Bunyajido (天象列次分野之圖) has the sun's locations at the equinoxes, which must have been copied from the astronomical treatises in Chinese historical annals, Songshu (宋書) and Jinshu (晉書). According to the treatises, an astronomer Wang Fan (王蕃, 228-266 CE) referred those values from a calendrical system called Qianxiangli (乾象曆, 223 CE), from which it is confirmed that it adopted the sun's location at the winter solstice of the $(21{\frac{1}{4}})^{th}$ du of the 8th lunar lodge Dou (斗) as the reference direction for equatorial lodge angles. This indicates that the sun's locations at equinoxes and solstices in the calendrical system are the same as those in Jingchuli (景初曆, 237 CE). Hence, we propose that the sun's location at the autumnal equinox in Cheonsang Yeolcha Bunyajido should be corrected from 'wu du shao ruo' (五度少弱), meaning the $(5{\frac{1}{6}})^{th}$ du, to 'wu du ruo' (五度弱), meaning the $(4{\frac{11}{12}})^{th}$ du, of the first lunar lodge Jiao (角), as seen in Jingchuli. We reconstruct the polar coordinate system used in circular star charts, assuming that the mean motion rule was applied and its reference direction was the sun's location at the winter solstice. Considering the precession, we determined the observational epoch of the sun's location at the winter solstice to be t_o = -18.3 ± 43.0 adopting the observational error of the so-called archaic determinatives (古度). It is noteworthy that the sun's locations at equinoxes inscribed in Cheonsang Yeolcha Bunyajido originated from Houhan Sifenli (後漢 四分曆) of the Latter Han dynasty (85 CE), while the coordinate origin in the star chart is related to Taichuli (太初曆) of the Former Han dynasty (104 BCE).

• Journal of Astronomy and Space Sciences
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• 제30권1호
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• pp.43-48
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• 2013

The geomagnetic activity shows the semiannual variation stronger in vernal and autumnal equinoxes than in summer and winter solstices. The semiannual variation has been explained by three main hypotheses such as Axial hypothesis, Equinoctial hypothesis, and Russell-McPherron Effect. Many studies using the various geomagnetic indices have done to support three main hypotheses. In recent, Oh & Yi (2011) examined the solar magnetic polarity dependency of the geomagnetic storm occurrence defined by Dst index. They reported that there is no dependency of the semiannual variation on the sign of the solar polar fields. This study examines the solar magnetic polarity dependency of quiet time geomagnetic activity. Using Dxt index (Karinen & Mursula 2005) and Dcx index (Mursula & Karinen 2005) which are recently suggested, in addition to Dst index, we analyze the data of three-year at each solar minimum for eight solar cycles since 1932. As a result, the geomagnetic activity is stronger in the period that the solar magnetic polarity is anti-parallel with the Earth's magnetic polarity. There exists the difference between vernal and autumnal equinoxes regarding the solar magnetic polarity dependency. However, the difference is not statistically significant. Thus, we conclude that there is no solar magnetic polarity dependency of the semiannual variation for quiet time geomagnetic activity.

• Journal of Astronomy and Space Sciences
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• 제27권3호
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• pp.181-188
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• 2010

We have carried out all-sky imaging of OH Meinel, $O_2$ atmospheric and OI 557.7 nm airglow layers in the period from July of 2001 through September of 2005 at Mt. Bohyun, Korea ($36.2^{\circ}$ N, $128.9^{\circ}$ E, Alt = 1,124 m). We analyzed the images observed during a total of 153 clear moonless nights and found 97 events of band-type waves. The characteristics of the observed waves (wavelengths, periods, and phase speeds) are consistent with internal gravity waves. The wave occurrence shows an approximately semi-annual variation, with maxima near solstices and minima near equinoxes, which is consistent with other studies of airglow wave observations, but not with those of mesospheric radar/lidar observations. The observed waves tended to propagate westward during fall and winter, and eastward during spring and summer. Our ray tracing study of the observed waves shows that majority of the observed waves seemed to originate from mesospheric altitudes. The preferential directions and the apparent source altitudes can be explained if the observed waves are secondary waves generated from primary waves that have been selected by the filtering process and break up at the mesospheric altitudes.

• Journal of Astronomy and Space Sciences
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• 제33권1호
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• pp.29-36
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• 2016

The East African ionosphere (3°S-18°N, 32°E-50°E) was mapped using Total Electron Content (TEC) measurements from ground-based GPS receivers situated at Asmara, Mekelle, Bahir Dar, Robe, Arbaminch, and Nairobi. Assuming a thin shell ionosphere at 350 km altitude, we project the Ionospheric Pierce Point (IPP) of a slant TEC measurement with an elevation angle of >10° to its corresponding location on the map. We then infer the estimated values at any point of interest from the vertical TEC values at the projected locations by means of interpolation. The total number of projected IPPs is in the range of 24-66 at any one time. Since the distribution of the projected IPPs is irregularly spaced, we have used an inverse distance weighted interpolation method to obtain a spatial grid resolution of 1°×1° latitude and longitude, respectively. The TEC maps were generated for the year 2008, with a 2 hr temporal resolution. We note that TEC varies diurnally, with a peak in the late afternoon (at 1700 LT), due to the equatorial ionospheric anomaly. We have observed higher TEC values at low latitudes in both hemispheres compared to the magnetic equatorial region, capturing the ionospheric distribution of the equatorial anomaly. We have also confirmed the equatorial seasonal variation in the ionosphere, characterized by minimum TEC values during the solstices and maximum values during the equinoxes. We evaluate the reliability of the map, demonstrating a mean error (difference between the measured and interpolated values) range of 0.04-0.2 TECU (Total Electron Content Unit). As more measured TEC values become available in this region, the TEC map will be more reliable, thereby allowing us to study in detail the equatorial ionosphere of the African sector, where ionospheric measurements are currently very few.

• Journal of Astronomy and Space Sciences
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• 제31권2호
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• pp.149-157
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• 2014

As the prediction of geomagnetic storms is becoming an important and practical problem, conditions in the Earth's magnetosphere have been studied rigorously in terms of those in the interplanetary space. Another approach to space weather forecast is to deal with it as a probabilistic geomagnetic storm forecasting problem. In this study, we carry out detailed statistical analysis of solar wind parameters and geomagnetic indices examining the dependence of the distribution on the solar cycle and annual variations. Our main findings are as follows: (1) The distribution of parameters obtained via the superimposed epoch method follows the Gaussian distribution. (2) When solar activity is at its maximum the mean value of the distribution is shifted to the direction indicating the intense environment. Furthermore, the width of the distribution becomes wider at its maximum than at its minimum so that more extreme case can be expected. (3) The distribution of some certain heliospheric parameters is less sensitive to the phase of the solar cycle and annual variations. (4) The distribution of the eastward component of the interplanetary electric field BV and the solar wind driving function BV2, however, appears to be all dependent on the solar maximum/minimum, the descending/ascending phases of the solar cycle and the equinoxes/solstices. (5) The distribution of the AE index and the Dst index shares statistical features closely with BV and $BV^2$ compared with other heliospheric parameters. In this sense, BV and $BV^2$ are more robust proxies of the geomagnetic storm. We conclude by pointing out that our results allow us to step forward in providing the occurrence probability of geomagnetic storms for space weather and physical modeling.

• 건축역사연구
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• 제7권4호
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• pp.191-198
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• 1998

로마의 판테온은 고대 로마 시대의 건축 유구 중에서 그 원형을 가장 잘 유지하고 있는 건축물중의 하나이다. 않은 부분이 헐리거나 다시 지어졌음에도 불구하고 대형 로툰다와 벽체, 그리고 포티코는 아직도 원래의 장중한 모습을 그대로 지니고 있다. 직경 43.3M의 로툰다 내부는 그와 같은 높이인 돔 상부에 뚫려있는 직경 8.1M의 '눈'(Oculo)을 통해 들어오는 햇빛만으로 밝혀진다. 판테온은 정 남-북으로 방위를 잡았고 포티코는 로툰다의 정 북 방향으로 놓였다. 어떤 건축물이 정 방위하는 것은 그 자체로 매우 특이한 일이다. 이집트의 피라미드, 메소포타미아의 지구라트 등이 그러한 예에 해당한다. 이는 개략적인 정 방위와는 근본적으로 다른 배치 개념인 것이다. 필자는 그 중에서도 특히 정 남-북 방위를 잡은 경우는 일사각과 뗄 수 없는 관계가 있다고 믿는다. 이집트의 피라미드가 정 사각추 라는 단순한 기하학적 형태를 지닌 것처럼 판테온도 구형 및 원통형이라는 단순한 기하학적 형태를 지녔다. 돔 상부의 '눈'을 통해 들어오는 원형의 햇빛은 마치 규칙적으로 돌아가는 탐조등처럼 하루하루 로툰다 내부를 비추며 돌아간다. 햇빛은 당연히 규칙적으로 돌아가는 것이다. 그렇다면 햇빛과 판테온의 형태 사이에 어떤 관계가 있을 수 있으리라고 추정할 수 있다. 필자는 이러한 관계를 찾기 위해 scanning한 판테온 도면 위에, autocad로 로마의 위도에 맞춘 해의 궤적도를 그리는 작업을 했다. 기대했던 만큼의 결과는 아니었지만 다음과 같은 결론을 얻을 수 있었다. (1) 포티코 앞쪽 지붕 정점은 동지일 정오 돔의 그림자와 만난다. (2) 포티코 앞쪽 기둥열의 평면상 중심선은 돔의 입체적 중심에서 그린 동지일 정오 해의 고도각과 일치한다. (3) 춘, 추분 정오, '눈'을 통해 들어오는 햇빛은 로툰다 출입구 아치를 지나 포티코 바닥에 특이한 형태의 빛을 만든다. 이는 춘, 추분 정오에만 만들어지는, 아치의 원호와 '눈'의 원호가 만나서 만드는 특이한 형태의 빛이다. 여기서 판테온이 춘, 추분을 정시(定時)하기 위한 일종의 해시계였다는 가설이 성립될 수 있다.

• 한국콘텐츠학회논문지
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• 제11권3호
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• pp.460-466
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• 2011

감은사는 첨성대가 건축되고 46년 후 서력 682년에 세워진 신라시대 사찰로 현재는 금당터와 석탑 및 각종 석조 유물로 전해지고 있다. 본 논문에서는 1959년 1차 발굴 때 감은사지 금당터의 동편에서 발견된 동편 태극 장대석과 2차 발굴 때 감은사지 남편 연못에서 발견되어 1993년 인위적으로 서편에 배치된 서편 태극 장대석에 대한 과학적 의미를 파악하기 위하여 유물에 각인된 도형의 기하학적 분석을 한다. 그리하여 감은사지 태극 장대석이 의미하는 수학적, 천문학적인 도형의 현대적 해석을 통하여 당시의 과학 수준을 가늠할 중요한 척도를 얻게 되었다. 또한 동편 및 서편 태극 장대석이 나타내는 이등변삼각형들의 배치가 각각 해와 달과 관련된 책력과 연관함을 추론하게 된다. 이러한 엄밀한 수학적 개념 조사를 통하여 역사적 사실이 빈약한 오래된 역사적 구조물을 이해하고 고증하는데 새로운 연구 방향을 제시해준다.

• 설비공학논문집
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• 제27권8호
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• pp.395-401
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• 2015

Recently, many research studies have been carried out on the efficiency of light-shelf daylighting systems, especially comparing performance improvements and the limitations of reflective surfaces and their lighting performance. In this study, a crystal face reflective surface is proposed. The objective of the study is to evaluate the lighting performance of a crystal face light-shelf through a performance study. The performance study was carried out in a full scale test-bed in order to calculate the light distribution and energy consumption utilizing the standard indoor illumination as an index. The conclusions of the performance study are as follows. 1) The optimal angle of incidence for daylighting for both the operable flat type light-shelf and the crystal face light-shelf are taken in the natural environment on the dates of the winter and summer solstices, as well as the autumn and spring equinoxes. 2) The application and installation of the crystal face light-shelf can produce a 29.9%~34.3% increase of light distribution within the indoor space. However, the increase of light distribution can also lead to a decrease in the uniformity ratio, a design challenge that should be considered when applying a crystal face light-shelf. 3) It is possible to achieve a 7.98%~13.3% greater reduction in energy consumption when applying a crystal face light-shelf than when applying a flat type light-shelf. The increase in the number of crystal faces should concur with the analysis of the energy reduction. A limitation of the study is that only one predetermined pattern was performance tested for a crystal face light-shelf. In order to carry out further research on crystal face light-shelves, additional performance studies are needed based on alternative patterns and designs.