UV polarimetry of the x‐ray binary systems 4U1700‐37, Vela XR‐1, and Cygnus XR‐1

K. Wolinski, J. Dolan, P. Boyd, J. Elliot, M. Nelson, J. Percival, L. Townsley, G. W. Citters
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Abstract

Variable linear polarization has previously been observed in the visible Tapia, 1984), Vela XR‐1 (Dolan & Tapia, 1988), and Cyg XR‐1 (Kemp et al., 1976, 1978). We present the first linear polarization observations of these systems in the ultraviolet (UV), using the High Speed Photometer (HSP) aboard the Hubble Space Telescope. The UV polarimetric light curves obtained from Vela XR‐1 and 4U1700‐37 display an added component of polarization at first quadrature inconsistent with the standard model of Brown et al. (1978) for scattering in binary systems. However, the UV polarimetric light curves toward Cyg XR‐1 are well fit by the standard model. Variations attributable to changes in scattering structure from one orbit to the next are also detected in two of the systems. Possible origins of the additional polarization detected at first quadrature in Vela XR‐1 and 4U1700‐37 are evaluated.
x射线双星系统4U1700‐37、船帆XR‐1和天鹅座XR‐1的紫外偏振度测定
在此之前,已经在可见光(Tapia, 1984)、船帆XR‐1 (Dolan & Tapia, 1988)和天鹅座XR‐1 (Kemp et al., 1976, 1978)中观测到可变线偏振。我们使用哈勃太空望远镜上的高速光度计(HSP)对这些系统的紫外(UV)进行了首次线性偏振观测。从Vela XR‐1和4U1700‐37获得的紫外偏振光曲线显示,在第一正交处增加了偏振分量,这与Brown等人(1978)的双星系统散射标准模型不一致。然而,Cyg XR‐1的紫外偏振光曲线与标准模型拟合得很好。从一个轨道到下一个轨道的散射结构变化也在其中两个系统中被探测到。对Vela XR‐1和4U1700‐37第一次正交检测到的额外偏振的可能来源进行了评估。
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