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First photometric study of ultrashort-period contact binary 1SWASP J140533.33+114639.1 被引量:2

First photometric study of ultrashort-period contact binary 1SWASP J140533.33+114639.1
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摘要 In this paper,CCD photometric light curves for the short-period eclipsing binary 1 SWASP J140533.33+114639.1(hereafter J1405) in the BV R bands are presented and analyzed using the 2013 version of the Wilson-Devinney(W-D) code. It is discovered that J1405 is a W-subtype shallow contact binary with a contact degree of f = 7.9±0.5% and a mass ratio of q = 1.55±0.02. In order to explain the asymmetric light curves of the system,a cool starspot on the more massive component is employed. This shallow contact eclipsing binary may have been formed from a short-period detached system through orbital shrinkage due to angular momentum loss. Based on the(O-C) method,the variation of orbital period is studied using all the available times of minimum light. The(O-C) diagram reveals that the period is increasing continuously at a rate of d P/dt = +2.09×10^-7 d yr^-1,which can be explained by mass transfer from the less massive component to the more massive one. In this paper,CCD photometric light curves for the short-period eclipsing binary 1 SWASP J140533.33+114639.1(hereafter J1405) in the BV R bands are presented and analyzed using the 2013 version of the Wilson-Devinney(W-D) code. It is discovered that J1405 is a W-subtype shallow contact binary with a contact degree of f = 7.9±0.5% and a mass ratio of q = 1.55±0.02. In order to explain the asymmetric light curves of the system,a cool starspot on the more massive component is employed. This shallow contact eclipsing binary may have been formed from a short-period detached system through orbital shrinkage due to angular momentum loss. Based on the(O-C) method,the variation of orbital period is studied using all the available times of minimum light. The(O-C) diagram reveals that the period is increasing continuously at a rate of d P/dt = +2.09×10^-7 d yr^-1,which can be explained by mass transfer from the less massive component to the more massive one.
出处 《Research in Astronomy and Astrophysics》 SCIE CAS CSCD 2018年第3期57-62,共6页 天文和天体物理学研究(英文版)
基金 partly supported by the National Natural Science Foundation of China (Nos.11133007 and 11573063) the Science Foundation of Yunnan Province (Grant No.2012HC011)
关键词 STARS BINARIES close - stars BINARIES eclipsing - stars individual (1SWASPJ140533.33+114639.1) stars binaries close - stars binaries eclipsing - stars individual (1SWASPJ140533.33+114639.1)
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