HD 32297盘的星际介质雕刻
Interstellar Medium Sculpting of the HD 32297 Disk
摘要：
我们在1.6和2.05 \micron的散射光中探测到HD 32297碎片盘。我们使用这些新的意见与以前的散射光图像的磁盘在1.1 \micron检查的结构和散射效率的磁盘作为波长的函数。除了表面亮度的不对称性和扭曲的形态超过$\sim$ 1 \farcs 5的一个叶盘，我们发现，存在着不对称的光谱特征的颗粒之间的东北和西南叶。盘叶的大多数中性颜色意味着大约1 \micron大小的颗粒负责散射。我们发现，在颜色和形态的不对称性，可以合理地解释HD 32297的运动到一个密集的ISM云在相对速度为15公里的$^{-1}$。我们模拟了尘埃颗粒与HI气体在云中的相互作用。我们认为，超音速弹道阻力可以解释HD 32297，HD 15115和HD 61005的碎片盘的形态。
英文摘要：
We detect the HD 32297 debris disk in scattered light at 1.6 and 2.05 \micron. We use these new observations together with a previous scattered light image of the disk at 1.1 \micron to examine the structure and scattering efficiency of the disk as a function of wavelength. In addition to surface brightness asymmetries and a warped morphology beyond $\sim$1\farcs5 for one lobe of the disk, we find that there exists an asymmetry in the spectral features of the grains between the northeastern and southwestern lobes. The mostly neutral color of the disk lobes imply roughly 1 \micron-sized grains are responsible for the scattering. We find that the asymmetries in color and morphology can plausibly be explained by HD 32297's motion into a dense ISM cloud at a relative velocity of 15 km s$^{-1}$. We model the interaction of dust grains with HI gas in the cloud. We argue that supersonic ballistic drag can explain the morphology of the debris disks of HD 32297, HD 15115, and HD 61005.
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