접촉쌍성 AW UMa의 측광학적 연구

PHOTOMETRIC STUDY OF CONTACY BINARY AW UMa

충북대학교 천문우주학과의 35cm Schmidt-Cassegrain 망원경으로 접촉쌍성 AW UMa를 1994년 3월부터 4월 사이의 13일 밤 동안 BVRI 광전측광관측 하여 각 필터별로 273점씩 총 1092개의 관측점을 얻었다. 이 관측점들을 이용하여 BVRI 광도곡선을 그렸으며, 이로부터 주극심시각 JD Hel 2449456.1502 와 부극심시각 JD Hel 2449432.2412, JD Hel 2449447.1567을 결정하였다. 수집한 극심시각 자료들을 가지고 그린 O-C도에서, 공전주기 변화량 $-0.^d00000394$를 구하고 그에 해당하는 질량이동량 $-6.4\times10^{-7}M_\odot/year$를 계산하였다. AW UMA의 광도변화를 질량이동과 연관하여 해석할 수 있는 가능성을 제시했다.

BVRI observatins of AW UMa were made from March to April during 13 nights in 1994 using the 35cm Schmidt-Cassegrain telescope of Department of Astronomy and Space Science, Chungbuk National University. A total of 1092 observations (273 in B, 273 in V, 273 in R, 273 in I) were obtained. We constructed the light curves of BVRI with these observations. The one time of primary minimum light of JD Hel 2449456.1502 and the two times of secondary minimum light of JD Hel 2449456.1502 and JD Hel 2449447.1567 were determined from our observations. Orbital period change of -0.d00000394 was determined from O-C diagram which was constructed with collected times of minimum lights. Mass transfer rate of $-6.4\times10^{-7}M_\odot/year$ was derived using the period changing ratio. It is suggested that the inhomogeneous distribution of transferred matter around the secondary component would produce the irregular light variation of the AW UMa system.