• Communications of the Korean Institute of Information Scientists and Engineers
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• v.3 no.1
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• pp.12-17
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• 1985

This pape rdeals with the first half of ALGOL-60(Subset) compiler -scanner and analyzer-, which is writter in FORTRAN IV. As the original syntax description of ALGOL-60 is too complex to use, real number array, and procedures are omitted. And a subset of ALGOL-60 is defined.

• Journal of Astronomy and Space Sciences
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• v.10 no.2
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• pp.123-145
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• 1993

UBVRi photometry of Algol was carried out from December of 1988 to March of 1991 at Chungbuk National University Observatory and a total of 3465 observations in U, B, V, R, I were obtained. Three times of primary minimum light of JDH el 2447898.0938, JEH el 2448265.1205 and JDH el 2448288.0598, and two secondary minimum light of JDH el 2447808.1014 and JDH el 2448275.146 were determined from our observations. We analyzed simultaneously the UBVRI light curves of the Algol system with the Wilson-Devinney method for the determination of the photometric parameters. Indivisual masses for the 3 components of Algol are derived as $m_1$=3.36, $m_2$=0.76, $m_3$=1.6 in solar mass and radii as $R_1$=2.97, $R_2$=0.76 in solar radinus using i=$82.{\circ}47$, q=0.227, $r_1$=0.2102, $r_2$=0.2512 of our solution and some parameters of the spectroscopic solution of Hill et al. (1971). Our results is simiar to those reported by Kim (1989). The temperature of Algol C, $T_3$=8800 was obtained by means of fitting $l_1$, $l_2$, and $l_3$ of five colors to Planckian curve, and $R_3$=$1.6R_\odot$ is derived from its result. It is believed that its semidetached configuration of Algol A and B is the consequence of case B mass transfer. According to its location in a mass-radius diagram. Algol b may have evolved significantly in its Hburnning phase.

• Bulletin of the Korean Space Science Society
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• 1992.10a
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• pp.17-17
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• 1992

As a part of the project for The Atlas of (d-C) Diagams of Eclipsing Binaries, a total of 1822 times of minimum lights for Algol distributed from 1782 to 1988 are collecte dand analyzed to investigate the period-changes of the system. An (0-C) diagram constructed shows that the orbital period of Algol has varied in complicated ways. In this paper, we would interprets these variations as the sudden changes of the periodrather than as a somewhat periodic ones. The importancy of the observations for the times of minimum lights of Algol system will be stressed.

• Journal of The Korean Astronomical Society
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• v.46 no.4
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• pp.151-159
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• 2013

We discuss the orbital period changes of the Algol semi-detached eclipsing binary DI Peg by constructing the (O-C) residual diagram via using all the available precise minima times. We conclude that the period variation can be explained by a sine-like variation due to the presence of a third body orbiting the binary, together with a long-term orbital period increase (dP/dt=0.17 sec/century) that can be interpreted to be due to mass transfer from the evolved secondary component (of rate $1.52{\times}10^{-8}M_{\odot}/yr$) to the primary one. The detected low-mass third body ($M_{3min.}=0.22{\pm}0.0006M_{\odot}$) is responsible for a periodic variation of about 55 years light time effect. We have determined the orbital parameters of the third component which show a considerable eccentricity $e_3=0.77{\pm}0.07$ together with a longitude of periastron ${\omega}_3=300^{\circ}{\pm}10^{\circ}$.

• Journal of The Korean Astronomical Society
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• v.47 no.3
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• pp.99-104
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• 2014

We present the rst period variation study for the Algol eclipsing binary V346 Cyg by constructing the (O-C) residual diagram using all the available precise minima times. We conclude that the period variation can be explained by a sine-like variation due to the presence of a third body orbiting the binary in about $68.89{\pm}4.69$ years, together with a long-term orbital period decrease ($dP/dt=-1.23{\times}10^{-7}day/yr$) that can be interpreted to be due to slow mass loss from the ${\delta}$-Scuti primary component. The sinusoidal variation may also be explained by using the the Applegate (1992) mechanism involving cyclic magnetic activity due to star-spots on the secondary component. The present preliminary solution needs more precise photometric observations to be confirmed.

• Journal of Astronomy and Space Sciences
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• v.29 no.2
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• pp.141-143
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• 2012

Some Algol-type interacting binary stars exhibit strange photometric variations that can be phase-dependent and/or secular. This paper discusses the possibility of explaining these observed variations as resulting from an accretion structure eclipsing one or both of the stars. Some previous studies are reviewed and suggestions for future work are made, including the prospective of incorporating data from the Kepler Observatory.

• The Bulletin of The Korean Astronomical Society
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• v.31 no.1
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• pp.34.1-34.1
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• 2006

• The Bulletin of The Korean Astronomical Society
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• v.24 no.2
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• pp.103-103
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• 1999

• Bulletin of the Korean Space Science Society
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• 1994.04a
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• pp.20-20
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• 1994

• Bulletin of the Korean Mathematical Society
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• v.11 no.1
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• pp.39-43
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• 1974