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REFERENCE LINKING PLATFORM OF KOREA S&T JOURNALS
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Journal of The Korean Astronomical Society
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Journal DOI :
The Korean Astronomical Society
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Volume & Issues
Volume 10, Issue 1 - Dec 1977
Selecting the target year
EFFECTIVE TEMPERATURE OF OV STARS
Cho, Soon-Wha ; Yun, Hong-Sik ;
Journal of The Korean Astronomical Society, volume 10, issue 1, 1977, Pages 3~12
-system colors for 23 OV stars compiled by Crawford have been compared with colors calculated by Mihalas from non-LTE model atmospheres. In this way, effective temperatures of these stars have been determined and plotted against spectral type,
(u-b), (b-y), (U-B), and (B-V). Within the accuracy of the observations, effective temperatures derived from the photometry for these 23 main-sequence stars are found to be in good agreement with Contiis spectroscopical temperatures.
ON THE REFERENCE PERIOD OF IL-CHIN OF SEASONAL PARTS AND EACH DATE OF THE YEAR IN OLD CHINESE CALENDAR
Lee, Eun-Sung ;
Journal of The Korean Astronomical Society, volume 10, issue 1, 1977, Pages 13~22
Il-Cohin of the 24 subseasons is found to be repeated in the period ut 103, solar yeors. And that of the date in the old Chinese calendar xear is, repeating in the period of 102 solar years. It is also found that the length of lunar month is repeating in nearly 64solar years.
MASS EXCHANGE OF THE ECLIPSING BINARY WZ ANDROMEDAE
Oh, Kyu-Dong ;
Journal of The Korean Astronomical Society, volume 10, issue 1, 1977, Pages 23~30
We have collected times of minimum light available in the literature for WZ Andromedae and analyzed the nature of the period variations. The O-C diagram of WZ And clearly shows that two abrupt changes near JD 2418000 and JD 2435000 are deduced by dp/p=
, respectively. For these period changes, we have introduced the equations which represent mass exchange in the close binery systems given by Biermann and Hall (1973), and the computation yieleled a mass flow of
. from the hotter component to the cooler one. Due to the amount of mass flow, the period decrease may also be calculated. The theoritical new period after JD 2435000 became 0.69565858 days, which is in good agreement with the value 0.69566034 days found in the O-C diagram. In this computation, the mass ratio of WZ And suggested that the hotter star is the filling its Rochclooe, and thus WZ And is in Paczynski's stage II.
SOME NOTES ON PHOTOMETRIC OBSERVATIONS: PHOTOELECTRIC PHOTOMETRIC OBSERVATIONS (I)
Lee, See-Woo ;
Journal of The Korean Astronomical Society, volume 10, issue 1, 1977, Pages 31~38
To reduce the instrumental and calibration errors in the photoelectric photometry as much as possible it is necessary to select the optimum photocell voltage and energy attenaution and to observe as many standard stars as possible over the wide range of color, spectral type and air mass.