利用高分辨率多波长阿塔卡马大型毫米/亚毫米波阵列观测对HD 163296星系盘进行尘埃特征分析
Dust characterization of the HD 163296 disk with high-resolution multi-wavelength ALMA observations
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中文总结 AI 辅助
该研究通过对HD 163296星系盘多波长高分辨率观测做SED拟合，表征其尘埃特性。利用新的ALMA波段9观测及存档数据，结合VLA观测，探索多种尘埃模型，确定DSHARP Zubko模型为首选，分析了尘埃特性及各盘尘埃质量。
中文摘要 AI 辅助
行星通过原行星盘中尘埃颗粒的生长和聚集形成。表征尘埃特性（如大小、表面密度和温度）是理解行星形成的关键。我们通过对多波长高分辨率观测进行光谱能量分布（SED）拟合来表征HD 163296周围原行星盘的尘埃特性。我们展示了对温度敏感的新的高分辨率阿塔卡马大型毫米/亚毫米波阵列（ALMA）波段9（0.45毫米）观测结果。利用这些新的波段9观测数据以及存档的ALMA波段3、4、6和7观测数据，以0.066角秒的共同分辨率进行SED拟合。将拟合结果与甚大阵（VLA）观测进行比较，并探索具有不同光学常数和孔隙率的多种尘埃模型。波段9图像显示了中心盘、0.67和1.00角秒处的两个环以及先前在其他波长看到的外部扩展发射。在较高频率下，环看起来更宽，间隙看起来更浅，扩展发射看起来更亮，这可以用光深效应和/或尺寸分离来解释。我们对每个尘埃模型的尘埃特性（包括温度、表面密度和尘埃大小）进行了表征。然而，推断出的尘埃特性取决于尘埃模型，仅ALMA数据无法确定哪种尘埃模型更优。基于VLA剖面以及物理和观测约束，我们确定DSHARP祖布科（多孔）模型为首选模型。外环温度低于被动辐射盘模型的预测，表明受内环遮挡。尽管表面密度和尘埃大小取决于尘埃模型，但首选模型表明中心盘、两个环和扩展盘各自包含超过几个地球质量的尘埃。
英文摘要
Context. Planets form through the growth and accumulation of dust grains in protoplanetary disks. Characterizing dust properties such as size, surface density, and temperature is key to understanding planet formation. Aims. We characterize the dust properties of the protoplanetary disk around HD 163296 by performing spectral energy distribution (SED) fitting of multi-wavelength high-resolution observations. Methods. We present new high-resolution ALMA Band 9 (0.45 mm) observations, which are sensitive to the temperature. We performed SED fitting at a common resolution of 0.066 arcsec using these new Band 9 observations along with archival ALMA Band 3, 4, 6, and 7 observations. We compared the fitted results with VLA observations and explored multiple dust models with different optical constants and porosities. Results. The Band 9 image shows the central disk, two rings at 0.67 and 1.00 arcsec, and outer extended emission previously seen at other wavelengths. At higher frequencies, the rings appear wider, the gaps appear shallower, and the extended emission appears brighter, which can be explained by optical-depth effects and/or size segregation. We characterized the dust properties, including temperature, surface density, and dust size, for each dust model. However, the inferred dust properties are dependent on the dust model, and the ALMA data alone do not allow us to determine which dust model is preferred. We identified the DSHARP Zubko (porous) model as the preferred model based on VLA profiles and physical and observational constraints. The outer ring temperature is lower than predicted by a passively irradiated disk model, suggesting shadowing by the inner ring. Although the surface density and dust size depend on the dust model, the preferred model indicates that the central disk, both rings, and the extended disk each contain more than a few Earth masses of dust.
发表机构
- Max-Planck Institute for Astronomy（马克斯·普朗克天文学研究所）
- National Astronomical Observatory of Japan（日本国立天文台）
- Graduate Institute for Advanced Studies, SOKENDAI（综合研究大学院大学）
- Department of Physics, National Sun Yat-Sen University（国立中山大学物理系）
- Center of Astronomy and Gravitation, National Taiwan Normal University（国立台湾师范大学天文与引力研究中心）
- Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内科克天文学研究所）
- Department of Earth Science and Astronomy, The University of Tokyo（东京大学地球科学及天文学系）
- Dipartimento di Fisica, Università degli Studi di Milano（米兰大学物理系）
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