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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
- Chu, Sun-Il
- 天文學會誌 = The journal of the Korean Astronomical Society
- 6, n.1
- pp.19-28
- 1973
- 원문 바로보기
16세기 후반에서 17세기 초에 우리나라에서 관측된 4개의 초신성(Tycho Supernova, Kepler Supernova, Cassiopeia Nova 및 Cassiopeia A)의 기록은 세계 어느 나라 천문관측기록 보다 더 자세히, 또 더 정확히 표시되어 있다. 특히 Kepler Supernova의 기록은 우리나라 이조 왕조실록에 가장 자세하게 실려있다. 위치뿐만 아니라 밝기, 관측시간 및 관측상태를 낱낱이 표기한 이 관측치로부터 다음과 같은 광도곡선상의 특징을 알아낼 수 있다. 1. 준극대광도(Pre-max-halt)는 1604년 10월 20일부터 10월 26일 사이 2. 극대광도(Maximum Luminosity)는 1604년 10월 29일부터 11월6일 사이 3. 천이과정(Transition)은 아마도 1604년 11월 28일부터 1604년 12월 26일 사이에 있었을 것이다.
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
- 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.
1199
- Lee, See-Woo
- 天文學會誌 = The journal of the Korean Astronomical Society
- 3, n.1
- pp.13-16
- 1970
- 원문 바로보기
A hyperbolic orbit is expanded in terms of F analogous to the eccentric anomaly of an elliptical orbit: <TEX>${\tau}^p\;sinq{\upsilon}\;and\;{\tau}^p\;cosq{\upsilon}$</TEX> are expressed in terms of F. The true anomaly <TEX>${\upsilon}$</TEX> is expressed in terms of F, and F in terms of <TEX>${\upsilon}$</TEX>.
1200
- 김정흠
- 天文學會誌 = The journal of the Korean Astronomical Society
- 3, n.1
- pp.17-27
- 1970
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