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- W2604991303 abstract "1995년 11월부터 1999년 12월까지 총 10일간 W형 접촉쌍성 AB And를 소백산천문대의 61cm 망원경과 BVR필터를 사용하여 CCD 측광관측을 수행하였다. 우리의 관측으로부터 AB And의 1995, 1996그리고 1999년에 걸친 년도별 광도곡선을 완성하였고, 8개의 새로운 극심시각을 결정하였다. 새로 얻은 광도곡선은 AB And가 지난 5년 동안 심한 광도변화를 겪어왔음을 보여주고 있다. 기준 광도곡선으로 선정된 1996년의 광도곡선을 Wilson-Devinney쌍성모델의 접촉모드에 적용하여 AB And의 측광해를 구하였다. 이 분석에서 광도변화의 원인을 흑점에 의한 것으로 가정하여 시스템 인자들을 산출한 후, 단지 흑점만을 조정인자로 하여 1995년과 1999년 광도곡선을 분석하였다. 그 결과, 우리는 광도변화가 반성 표면 위에 hot spot과 cool spot가 동시에 존재해서 일어난다고 해석하였다. 반성 표면 위의 hot spot는 이재우(1999)가 제안한 질량교환에 의한 것으로 유추할 수 있다. We performed CCD photometric observations of the W-type contact binary AB And for 10 nights from November 1995 to December 1999 using the 61-cm reflector and BVR filters at Sobaeksan Optical Astronomy Observatory. From our observations, the seasonal light curves of AB And for 1995, 1996 and 1999 were completed and 8 new times of minimum light were determined. Newly obtained light curves show that strong light variations occurred in AB And during the past five years. We adopted the 1996 light curves as reference ones and obtained the photometric solutions of them with contact mode in the Wilson-Devinney binary code. Assuming such light variations were produced by the existence of a star spot (or star spots) in the analysis, we derived the system parameters and analyzed the 1995 and 1999 light curves by adjusting only the spot parameters. As the results, we interpreted that those light variations are produced by the simultaneous existence of a hot spot and a cool spot on the secondary. We could infer that the hot spot on the secondary is produced due to mass exchange between the components suggested by Lee (1999)." @default.
- W2604991303 created "2017-04-14" @default.
- W2604991303 date "2003-06-01" @default.
- W2604991303 modified "2023-10-14" @default.
- W2604991303 title "PHOTOMETRIC SOLUTIONS AND SPOT MODEL OF THE CONTACT BINARY AB ANDROMEDAE" @default.
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- W2604991303 doi "https://doi.org/10.5140/jass.2003.20.2.123" @default.
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