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Optical properties of dust from Jupiter family comets

机译：木星族彗星尘埃的光学性质

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To try to define specific physical properties of the dust of Jupiter-family comets (JFCs), we compare the light scattered by them. Amongst the more than 1000 JFCs, less than 200 are numbered, 40 of them being rather bright. In the present work we use data from the latter. In situ observations of three nuclei show low albedo surfaces. The albedo of the dust particles in the coma is low, with generally a red colour. The A(α)fp product is a measure of cometary activity and secular changes. Images of different regions (jets and fans) give indications on the nucleus rotation and position of the emitting areas, as compared to the position of the rotation axis. Differences in physical properties between the particles in different regions are pointed out by differences in the linear polarization of the scattered light and by spectral variations in brightness and polarization. Jupiter family comets are considered as dust-poor comets. Tails and trails' studies give an estimation of the size distribution of the particles. However the dust production rates depend on the largest particles (up to centimetre size), which are mainly observed in the trails where large dark compact particles are found. These dark particles are also responsible for the high polarization in the inner most coma of some comets. The meaning, in terms of physical properties, of the linear polarization is discussed through different examples such as 2P/Encke, 9P/Tempel 1 or the fragments of 73P/Schwassmann-Wachmann 3. Cometary outbursts and splitting events show that the properties of the dust ejected from the interior of the nucleus are similar to the ones of more active comets (new or with larger semi-major axis).
机译：为了定义木星家庭彗星（JFCs）尘埃的特定物理特性，我们比较了它们散射的光。在1000多个JFC中，只有不到200个被编号，其中40个非常明亮。在当前的工作中，我们使用后者的数据。对三个原子核的原位观测显示低反照率表面。昏迷中尘埃颗粒的反照率较低，通常呈红色。 A（α）fp产物可衡量彗星活动和长期变化。与旋转轴的位置相比，不同区域（喷射器和风扇）的图像给出了原子核旋转和发射区域位置的指示。通过散射光的线性偏振的差异以及亮度和偏振的光谱变化来指出不同区域中的粒子之间的物理性质的差异。木星家族的彗星被认为是尘埃稀少的彗星。尾巴和尾迹的研究给出了颗粒尺寸分布的估计。但是，粉尘的产生率取决于最大的颗粒（最大为厘米大小），主要在发现大的深色致密颗粒的路径中观察到。这些深色粒子还导致某些彗星最内层昏迷的高度极化。通过不同的例子（例如2P / Encke，9P / Tempel 1或73P / Schwassmann-Wachmann 3的片段）讨论了线性极化在物理性质方面的意义。彗星爆发和分裂事件表明，从原子核内部喷出的尘埃类似于更活跃的彗星（新的或具有更大的半长轴）的彗星。

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