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Suzaku monitoring of the Wolf-Rayet binary WR140 around periastron passage: An approach for quantifying the wind parameters

机译:朱雀监视环绕天体通道周围的Wolf-Rayet二进制WR140:量化风参数的一种方法

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Suzaku observations of theWolf-Rayet (W-R) binaryWR 140 (WC7pd+O5.5fc) were made at four different times around periastron passage in 2009 January. The spectra changed in shape and flux with the phase. As periastron approached, the column density of the low-energy absorption increased, which indicates that the emission from the wind-wind collision plasma was absorbed by the dense W-R wind. The spectra can be mostly fitted with two different components: a warm component with k(B)T = 0.3-0.6 keV and a dominant hot component with k(B)T similar to 3 keV. The emission measure of the dominant, hot component is not inversely proportional to the distance between the two stars. This can be explained by the O star wind colliding before it has reached its terminal velocity, leading to a reduction in its wind momentum flux. At phases closer to periastron, we discovered a cool plasma component in a recombining phase, which is less absorbed. This component may be a relic of the wind-wind collision plasma, which was cooled down by radiation, and may represent a transitional stage in dust formation.
机译:Suzaku在2009年1月围绕着绕星流的四个不同时间对Wolf-Rayet(W-R)binaryWR 140(WC7pd + O5.5fc)进行了观测。光谱的形状和通量随相位而变化。随着近日天文学家的到来,低能吸收的柱密度增加,这表明来自风-风碰撞等离子体的发射被密集的W-R风吸收。频谱可以主要由两个不同的分量拟合:k(B)T = 0.3-0.6 keV的温暖分量和k(B)T类似于3 keV的主要热分量。占主导地位的炽热分量的发射量度与两颗恒星之间的距离不成反比。这可以通过O型星风在达到其最终速度之前发生碰撞而导致风动量通量减小而解释。在更接近围产期激素的阶段,我们发现了重组阶段的冷血浆成分,吸收较少。该成分可能是风-风碰撞等离子体的遗物,它已被辐射冷却,并可能代表尘埃形成的过渡阶段。

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