HD 66051 is an eclipsing system with an orbital period of about 4.75 d that exhibits out-of-eclipse variability with the same period. New multicolour photometric observations confirm the longevity of the secondary variations, which we interpret as a signature of surface inhomogeneities on one of the components. Using archival and newly acquired high-resolution spectra, we have performed a detailed abundance analysis. The primary component is a slowly rotating late B-type star (T eff = 12500 ± 200 K; log g = 4.0, v sin i = 27 ± 2 km s−1) with a highly peculiar composition reminiscent of the singular HgMn-related star HD 65949, which seems to be its closest analogue. Some light elements as He, C, Mg, Al are depleted, while Si and P are enhanced. Except for Ni, all the iron-group elements, as well as most of the heavy elements, and in particular the REE elements, are overabundant. The secondary component was estimated to be a slowly rotating A-type star (T eff ~ 8000 K; log g = 4.0, v sin i ~ 18 km s−1). The unique configuration of HD 66051 opens up intriguing possibilities for future research, which might eventually and significantly contribute to the understanding of such diverse phenomena as atmospheric structure, mass transfer, magnetic fields, photometric variability and the origin of chemical anomalies observed in HgMn stars and related objects.
展开▼
机译:HD 66051是一种日食系统,其轨道周期约为4.75 d,在同一周期内表现出食外变化。新的多色光度学观测证实了二次变化的寿命,我们将其解释为组件之一表面不均匀的特征。使用档案和新获得的高分辨率光谱,我们进行了详细的丰度分析。主要成分是缓慢旋转的晚B型恒星(T eff = 12500±200 K; log g = 4.0,v sin i = 27±2 km s -1 sup>),具有非常特殊的成分让人联想到与HgMn相关的奇异恒星HD 65949,它似乎是与其最接近的类似物。某些轻元素如He,C,Mg,Al被耗尽,而Si和P被增强。除镍外,所有铁族元素以及大多数重元素,尤其是稀土元素都过量。次要分量估计是一颗缓慢旋转的A型星(T eff〜8000 K; log g = 4.0,v sin i〜18 km s -1 sup>)。 HD 66051的独特配置为将来的研究提供了有趣的可能性,这可能最终并极大地有助于理解各种现象,例如大气结构,传质,磁场,光度变异性以及在HgMn恒星中观测到的化学异常的起源。相关对象。
展开▼