• 천문학회보
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• 제39권1호
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• pp.61.2-61.2
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• 2014

We present a set of fiducial sequences of horizontal-branch stars in bright Galactic globular clusters, which have previously been observed in the Sloan Digital Sky Survey (SDSS). We derive fiducial lines on color-magnitude diagrams in multiple color indices (g - r, g - i, g - z, and u - g), after rejecting foreground and background objects as well as RR Lyrae variables utilizing these color indices. We compare our fiducial sequences with model predictions from Yonsei-Yale evolutionary tracks and BaSel spectral libraries, and find a satisfactory agreement between them in terms of their color-magnitude relations, except in u - g. We also compare theoretical models to color-magnitude diagrams of two open clusters (M67 and NGC 6791). Based on our best available cluster distance and reddening, we find that the mass of red clump (RC) stars in NGC 6791 is about a factor of two smaller than an earlier estimate from the application of asteroseismic scaling relations for solar-like oscillations. The smaller RC mass implies an enhanced mass loss along the red giant branch, which is in accordance with other compelling evidences found in this metal-rich system. Our estimated luminosity of RC stars in NGC 6791 is about 0.2 mag fainter than in earlier investigations based on solar-metallicity calibrations, and results in ~10% reduction in the RC-based distance estimation, when applied to metal-rich systems such as in the Galactic bulge.

• 한국재료학회지
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• 제1권2호
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• pp.86-92
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• 1991

Morse potential을 변형한 2체항(2-body tem)과 Axilrod-Teller potential을 변형한 3체항(3-body tem)으로 구성된 포텐셜에너지 함수를 사용하여 $C_2-C_6$ cluster 동소체들의 에너지들의 에너지를 3체항 세기인자(3-body intensity factor)의 함수로 나타냄으로써 3체 인력의 기여도의 증가함에 따라 carbon cluster들의 구조는 open structure로부터 closed structure로, 또한 복잡한 구조로부터 단순한 구조, 즉 3차원적인 형태로부터 2차원 및 1차원적인 형태로 변해감을 알 수 있었다.

• 천문학회지
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• 제37권3호
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• pp.119-129
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• 2004

A new method has been developed to solve the star cluster membership problem. It is based on synthetic photometry employing the Black Body concept as stellar radiation simulator. Synthetic color-magnitude diagram is constructed showing the main sequence band and the positions of binary star systems of combinations of various components through different photometric tracks. The method has been applied to the Hyades. The cluster membership problem has been re-appraised for the cluster (both single and binary) stars. For the binary members, the components' spectral types have been derived by the method. The results obtained agree very well with those found in literature, The method is simpler than the others and can be developed to undertake other cases as multiple star systems.

• 천문학회보
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• 제29권2호
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• pp.64.1-64.1
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• 2004

• 천문학회보
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• 제34권2호
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• pp.44.2-44.2
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• 2009

• 천문학회보
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• 제22권
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• pp.11.1-11.1
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• 1997

• 천문학회지
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• 제21권2호
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• pp.182-182
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• 1988

• 천문학회보
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• 제24권1호
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• pp.55-55
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• 1999

• 천문학회보
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• 제19권
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• pp.8.2-9
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• 1994

• 천문학회보
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• 제34권1호
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• pp.145.1-145.1
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• 2009