Multi-wavelength modeling of the spatially resolved debris disk of HD 107146
Multi-wavelength modeling of the spatially resolved debris disk of HD 107146
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HD 107146 空间分辨碎片盘的多波长建模
DOI：
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发表时间：
2011
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通讯作者：
M. Silverstone
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作者：
S. Ertel;S. Wolf;S. Metchev;G. Schneider;J. Carpenter;M. Meyer;L. Hillenbrand;M. Silverstone
目标。我们的目标是限制年轻的类太阳 (G2V) 恒星 HD107146 周围的星子群和尘埃的位置、组成和动力学状态。方法。我们考虑使用哈勃太空望远镜 (HST) 上的先进巡天相机 (HST/ACS) 在宽 V (lambda(c) 近似于 0.6 μ m) 和宽 I (lambda(c) 近似 0.8 μ m) 滤波器中获得的日冕观测结果，通过毫米波天文学研究组合阵列 (CARMA) 获得的分辨率 1.3 mm 图，斯皮策/IRS 低分辨率光谱在 7.6 μ 范围内m至37.0μm，以及物体在3.5μm至3.1mm波长范围内的光谱能量分布（SED）。我们使用 F110W 滤光片中 HST 上的近红外相机和多目标光谱仪 (HST/NICMOS) 对碎片盘进行新的日冕高分辨率观测来补充这些数据（lambda(c) 约为 1.1 μm）。在我们的建模中，使用盘密度分布和灰尘光学特性的参数化模型，将 SED 和盘在散射光以及热再发射中的图像结合起来。结果。提出了 HD107146 周围碎片盘的详细分析模型，使我们能够重现几乎整套空间分辨和未分辨的多波长观测结果。考虑到互补观测数据的多样性，我们能够打破单独对 SED 数据建模所产生的简并性。我们发现圆盘是一个延长的环，表面密度峰值为 131 天文单位。此外，我们发现了额外的内盘的证据，该内盘可能由在外盘内边缘释放的小颗粒组成，并由于坡印廷-罗伯逊阻力而向内移动。人们发现，出生环场景（即通过碰撞产生尘埃盘的或多或少较宽的星子环）是对盘的环形形状最有可能的解释。
Aims. We aim to constrain the location, composition, and dynamical state of planetesimal populations and dust around the young, sun-like (G2V) star HD107146. Methods. We consider coronagraphic observations obtained with the Advanced Camera for Surveys (HST/ACS) onboard the Hubble Space Telescope (HST) in broad V (lambda(c) approximate to 0.6 mu m) and broad I (lambda(c) approximate to 0.8 mu m) filters, a resolved 1.3 mm map obtained with the Combined Array for Research in Millimeter-wave Astronomy (CARMA), Spitzer/IRS low resolution spectra in the range of 7.6 mu m to 37.0 mu m, and the spectral energy distribution (SED) of the object at wavelengths ranging from 3.5 mu m to 3.1 mm. We complement these data with new coronagraphic high resolution observations of the debris disk using the Near Infrared Camera and Multi-Object Spectrometer (HST/NICMOS) aboard the HST in the F110W filter (lambda(c) approximate to 1.1 mu m). The SED and images of the disk in scattered light as well as in thermal reemission are combined in our modeling using a parameterized model for the disk density distribution and optical properties of the dust. Results. A detailed analytical model of the debris disk around HD107146 is presented that allows us to reproduce the almost entire set of spatially resolved and unresolved multi-wavelength observations. Considering the variety of complementary observational data, we are able to break the degeneracies produced by modeling SED data alone. We find the disk to be an extended ring with a peak surface density at 131 AU. Furthermore, we find evidence for an additional, inner disk probably composed of small grains released at the inner edge of the outer disk and moving inwards due to Poynting-Robertson drag. A birth ring scenario (i.e., a more or less broad ring of planetesimals creating the dust disk trough collisions) is found to be the most likely explanation of the ringlike shape of the disk.