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- The Korean Astronomical Society (The Korean Astronomical Society)
- 계간 (Quarterly)
- ISSN : 1225-4614 (ISSN : 1225-4614)
1225-4614
- DB구축현황 : 1,211건 (DB Construction : 1,211 Articles)
총 게시글 1,211건
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1191
- Chu, Sun-Il
- 天文學會誌 = The journal of the Korean Astronomical Society
- 6, n.1
- pp.1-8
- 1973
- 원문 바로보기
Presumable explosion time of Cas A has been listed from Dec. 6, 1592 to Mar. 5, 1593 in ancinet Korean observational records. It may have been overlooked, due to other supernova(Cassiopeia Nova) which appeared at that time near its original position of Cas A.
1192
- 유경노
- 天文學會誌 = The journal of the Korean Astronomical Society
- 6, n.1
- pp.9-14
- 1973
- 원문 바로보기
A simple model of the galactic mass distribution consisting of one sphere and two spheroids with different eccentricities is considered. The resulting model is found to be consistent with the recent observations of the galactic rotation as well as suggested shape of the Galaxy.
1193
- Yun, Hong-Sik
- 天文學會誌 = The journal of the Korean Astronomical Society
- 6, n.1
- pp.15-17
- 1973
- 원문 바로보기
Observational implication for a possible presence of a magnetic monopole-like field in the visible layers of sunspots is examined by constructing a magnetostatic model of sunspots with a monopole-like field configuration. The resulting monopole approximation for a magnetic structure of spots is found to be compatible with the observations within a certain limited range of optical depth, which happens to lie mostly in its visible range.
1194
- Hyun, Jong-June
- 天文學會誌 = The journal of the Korean Astronomical Society
- 5, n.1
- pp.1-6
- 1972
- 원문 바로보기
환성진화(桓星進化)의 최종단계(最終段階)에서 이루어지는 고밀도성(高密度星)(백색왜성(白色矮星), 중성자성(中性子星))의 평형(平衡)의 한계질량(限界質量)은 현재(現在)까지 태양질량(太陽質量)의 <TEX>$0.6{\sim}2$</TEX>배(倍)로 알려졌다. 이 값의 차이(差異)는 가정(假定)한 상태방정식(狀態方程式)에 따르고 있으나 그 어느것이나 모두 태양(太陽)의 질량(質量)과 대차(大差)없다는 사실(事實)은 주목(注目)할 일이다. 또 관측(觀測)된 보통(普通)의 별의 질량(質量)도 태양질량(太陽質量)의 <TEX>$\frac{1}{10}{\sim}60$</TEX>배(倍)의 범위에 있다. 이 두 사실(事實)을 종합(綜合)하여 태양(太陽)의 질량(質量)이 가지는 특정(特定)한 자리의 물리적(物理的)인 근거(根據)로서 Polytrope 기체(氣體)의 지수(指數) <TEX>$({\gamma}=\frac{4}{3})$</TEX>와 <TEX>$(\frac{{\hbar}c}{Gm_H{^2}})^{\frac{3}{2}}$</TEX>의 지수(指數)사이의 연관성(聯關性)을 고찰(考察)하였다.
1195
- 강용희
- 天文學會誌 = The journal of the Korean Astronomical Society
- 5, n.1
- pp.7-14
- 1972
- 원문 바로보기
We have investigated the structure of the general relativistic polytrope(G.R.P.) of n=5. The numerical solutions of the general relativistic Lane-Emden functions <TEX>${\upsilon}\;and\;{\theta}$</TEX> for the ratio of the central pressure to the central density <TEX>${\sigma}=0.1$</TEX>, 0.3, 0.5 and 0.8333 are plotted graphically. We may summarize the results as follows: 1. As the invariant radius <TEX>$\bar{\xi}$</TEX> increases, the numerical value of the mass parameter <TEX>${\upsilon}$</TEX> does not approach toward the assymptotic limit, as it does in the classical case <TEX>$({\upsilon}{\sim}{\sqrt{3}})$</TEX>, but it increases continuously with progressively smaller rate as compared with the classical case. 2. When <TEX>$\bar{\xi}$</TEX> is less than <TEX>${\sim}5.5$</TEX>, the value of the density function <TEX>${\theta}$</TEX> drops more rapidly than the classical one, whereas when <TEX>$\bar{\xi}$</TEX> is greater than <TEX>${\sim}5.5$</TEX>, <TEX>${\theta}$</TEX> becomes greater than the classical value. For the greater values of <TEX>${\sigma}$</TEX> these phenomena become significant. 3. From the above results it is expected that the equilibrium mass of the G.R.P. of n=5 must be larger than the classical masse <TEX>$({\sqrt{3}})$</TEX> and the mass is more dispersed than the classical configuration (i.e. equilibrium with infinite radius).
1196
- 박홍서
- 天文學會誌 = The journal of the Korean Astronomical Society
- 4, n.1
- pp.9-16
- 1971
- 원문 바로보기
The asymmetry of received intensity pattern within the bandwidth is derived from the analogy of the intensity distribution of two-slit interference. This suggests that the length of <TEX>$\frac{1}{2}{\lambda}$</TEX> delay line should be adjusted to the slightly upper frequency than the central frequency of the radio telescope with a wide bandwith. Some strange communication signals and man-made noises prevented us from obtaining the discernible information from the observed data for the sun. To overcome this difficulties, it is necessary to alter the operating frequency and site. It will be fo1lowed to measure the angular dimensions of the superposed radio sources by changing the distance between two antennas.
1197
- 이영범
- 天文學會誌 = The journal of the Korean Astronomical Society
- 4, n.1
- pp.1-8
- 1971
- 원문 바로보기
The average velocity, 330km/sec. of the high velocity stars with respect to the galactic center is obtained from the data used by Fricke on the assumption that the rotational velocity of the Local Standard of Rest is 250km/sec. Comparing this value with the escape velocity, 380km/sec, at the solar neighborhood which is calculated from Mestel's model of the Galaxy, it is shown that most of the high velocity stars are bound to the Galaxy and that their average apogalacticon is about 40 kpc from the galactic center. And the fact that stars with radial velocities larger than 63km/sec are missing in the direction of galactic rotation of L.S.R. is interpreted as the result partly of the random distribution of the directions of motion of the high velocity stars and partly of the observational errors.
1198
- 김정흠
- 天文學會誌 = The journal of the Korean Astronomical Society
- 3, n.1
- pp.17-27
- 1970
- 원문 바로보기
1199
- 우종옥
- 天文學會誌 = The journal of the Korean Astronomical Society
- 3, n.1
- pp.7-11
- 1970
- 원문 바로보기
Optical thickness of Rosette Nebula for Lyman Continuum is examined with W. Gebel's data. And the effective temperatures of the six exciting 0 stars of the nebula are obtained on the assumption that O stars emit black body radiation. The results are found to be generally in between Spitzers old and revised values.
1200
- Yun, Hong-Sik
- 天文學會誌 = The journal of the Korean Astronomical Society
- 3, n.1
- pp.1-5
- 1970
- 원문 바로보기
The earlier findings on the radiative heating through the umbral walls in large sunspots are further investigated. No significant evidence for the umbra! heating has been found in small-sized sunspot umbrae.