A new determination of the orbit and masses of the Be binary system δ Scorpii
A new determination of the orbit and masses of the Be binary system δ Scorpii
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Be 双星系统 δ Scorpii 的轨道和质量的新确定
DOI：
10.1111/j.1365-2966.2009.14272.x
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发表时间：
2008
影响因子：
4.8
通讯作者：
P. Tuthill
中科院分区：
文献类型：
--
作者：
W. Tango;J. Davis;A. Jacob;A. Mendez;J. North;J. O'Byrne;E. Seneta;P. Tuthill
双星星星δ Sco（HD 143275）在2000年经历了可见光区的显著增亮，并继续呈不规则变化。该系统在1999年、2000年、2001年、2006年和2007年被悉尼大学恒星干涉仪（SUSI）观测到。1999年的观测结果与根据以前公布的轨道要素所作的预测相一致。随后的观测只能通过假设在2000年在主星周围形成了一个角尺寸为2 ± 1质量的光学明亮发射区来解释。到2006/2007年，该地区的规模估计增长到400万。我们已经确定了一个一致的轨道要素，同时拟合所有公布的干涉和光谱数据，以及SUSI数据在这里报道。在2000年爆发之前测量的系统的产生的元素和亮度比已被用来估计组件的质量。测得MA = 15 ± 7 M�，MB = 8.0 ± 3.6 M�.动力学视差为7.03 ± 0.15mas，与修正的依巴谷视差基本一致。
The binary starδ Sco (HD143275) underwent remarkable brightening in the visible in 2000, and continues to be irregularly variable. The system was observed with the Sydney University Stellar Interferometer (SUSI) in 1999, 2000, 2001, 2006 and 2007. The 1999 observations were consistent with predictions based on the previously published orbital elements. The subsequent observations can only be explained by assuming that an optically bright emission region with an angular size of 2 ± 1 mas formed around the primary in 2000. By 2006/2007 the size of this region grew to an estimated 4m as. We have determined a consistent set of orbital elements by simultaneously fitting all the published interferometric and spectroscopic data as well as the SUSI data reported here. The resulting elements and the brightness ratio for the system measured prior to the outburst in 2000 have been used to estimate the masses of the components. We find MA = 15 ± 7M � and MB = 8.0 ± 3.6 M� . The dynamical parallax is estimated to be 7.03 ± 0.15 mas, which is in good agreement with the revised Hipparcos parallax.