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- 저자 : SADAKANE KOZO (검색결과 4 건)
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DOUBLE PEAKED OUTBURSTS OF THE BLAZAR OJ 287 IN 1994 - 1996
ARIMOTO JUN'ICHI,SADAKANE Kozo,HONDA SATOSHI,TANABE KAZUHITO The Korean Astronomical Society 1996 Journal of The Korean Astronomical Society Vol.29 No.suppl1
VRI bands CCD photometric observations of the BL Lac object OJ 287 have been carried out during the period from October, 1994 to May, 1996. OJ 287 underwent two major outbursts during our observations. The first peak (V14.0 mag.) occurred in the first half of November, 1994 and faded out to 16.5 mag within 150 days. The second peak (14.0 mag.) was observed in late December, 1995. The latter peak continued at nearly the same brightness until May, 1996. Such a long lasting outburst has never been reported for OJ 287. Color indices (V - R and V-I) remained nearly constant during the outbursts.
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PULSATIONAL CHARACTERISTICS OF V1719 CYGNI WITH PECULIAR LIGHT CURVE
KIM CHULHEE,KIM SEUNG-LI,SADAKANE KOZO The Korean Astronomical Society 1993 Journal of The Korean Astronomical Society Vol.26 No.2
The light curve and radial velocity curve of multiperiodic dwarf cepheid VI719 Cyg (HD200925) with peculiar light curve have been reanalyzed in order to identify the oscillation modes to confirm the helium settling within the envelope. To do these, through the period search for the photometric and radial velocity data from the literature, two different periods were determined and the oscillation modes corresponding to the first and second periods were identified as the fundamental and first radial overtones. Hence the helium settling within the envelope was confirmed from the period ratio. The color excess, metallicity, effective temperature, and surface gravity corresponding to two different modes were determined and it was found that these parameters almost do not depend upon different oscillation mode. By utilizing the surface brightness method, we investigated the variation of angular diameter and radial displacement and it was found that the angular variation is very peculiar. Also by referring to the stellar models, mass and age were determined as $2.7M_{\bigodot}$ and 0.42 Gyr respectively which make this variable star heavier and younger than other multimode dwarf cepheids. Preliminary spectroscopic CCD observations were carried out and it was found that Mg in VI719 Cygni is nearly solar abundent according to the analysis of $5172.68{\AA}MgI$ line which is inconsistent with the photometric result. It was suggested that VI719 Cyg may be classified as a $\rho$ Pup stars according to the photometric characteristics.
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PULSATIONAL CHARACTERISTICS OF V1719 CYGNI WITH PECULIAR LIGHT CURVE
KIM, CHULHEE,KIM, SEUNG-LI,SADAKANE, KOZO 全北大學校 基礎科學硏究所 1994 基礎科學 Vol.16 No.-
The light curve and radial velocity curve of multiperiodic dwarf cepheid V1719 Cyg(HD200925) with peculiar light curve have reanalyzed in order to identify the oscillation modes to confirm the hellium sattling within the envelope. To do these, through the period search for the photmetric and radial velocity data from the literature, two different periods were determined and the oscillation modes corresponding to the first and second periods were identifed as the fundamental and first radial overtones. Hence the helium settling within the envelope was confirmed from the period ratio. The color excess, metallicity, effective temperature, and surface gravity corresponding to two different modes were determined and it was found that these parameters almost do not depend upon different oscillation mode. By utilizing the surface brightness method, we investigated the variation of angular diameter and radial displacement and it was found that the angular variation is very peculiar. Also by referring to the stellar models, mass and age were dtermined as 2.7M_?? and 0.42 Gyr respectively which make this variable star heavier and younger than other multimode dwarf cepheids. Preliminary spectroscopic CCD observations were carried out and it was found that Mg in V1719 Cygni is nearly solar abundent according to the analysis of 5172.68ÅMgI line which is inconsistent with the photometric result. It was suggested that V1719 Cyg may be classified as a ρ Pup stars according to the photometric characteristics.
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