Diagnosing 0.1-10 au scale morphology of the FU\,Ori disk using ALMA and VLTI/GRAVITY
Hauyu Baobab Liu, Antoine Mérand, Joel D. Green, Sebastián Pérez, Antonio S. Hales, Yao-Lun Yang, Michael M. Dunham, Yasuhiro Hasegawa, Thomas Henning, Roberto … 展开作者
Hauyu Baobab Liu, Antoine Mérand, Joel D. Green, Sebastián Pérez, Antonio S. Hales, Yao-Lun Yang, Michael M. Dunham, Yasuhiro Hasegawa, Thomas Henning, Roberto Galván-Madrid, Ágnes Kóspál, Michihiro Takami, Eduard I. Vorobyov, Zhaohuan Zhu
We report new Atacama Large Millimeter/submillimeter Array Band 3 (86-100 GHz; $\sim$80 mas angular resolution) and Band 4 (146-160 GHz; $\sim$50 mas angular resolution) observations of the dust continuum emission towards the archetypal and ongoing accretion burst young stellar object FU Ori, which simultaneously covered its companion, FU Ori S. In addition, we present near-infrared (2-2.45 $μ$m) observations of FU Ori taken with the General Relativity Analysis via VLT InTerferometrY (GRAVITY; $\sim$1 mas angular resolution) instrument on the Very Large Telescope Interferometer (VLTI). We find that the emission in both FU Ori and FU Ori S at (sub)millimeter and near infrared bands is dominated by structures inward of $\sim$10 au radii. We detected closure phases close to zero from FU Ori with VLTI/GRAVITY, which indicate the source is approximately centrally symmetric and therefore is likely viewed nearly face-on. Our simple model to fit the GRAVITY data shows that the inner 0.4 au radii of the FU Ori disk has a triangular spectral shape at 2-2.45 $μ$m, which is consistent with the H$_{2}$O and CO absorption features in a $\dot{M}\sim$10$^{-4}$ $M_{\odot}\,yr^{-1}$, viscously heated accretion disk. At larger ($\sim$0.4-10 au) radii, our analysis shows that viscous heating may also explain the observed (sub)millimeter and centimeter spectral energy distribution when we assume a constant, $\sim$10$^{-4}$ $M_{\odot}\,yr^{-1}$ mass inflow rate in this region. This explains how the inner 0.4 au disk is replenished with mass at a modest rate, such that it neither depletes nor accumulates significant masses over its short dynamic timescale. Finally, we tentatively detect evidence of vertical dust settling in the inner 10 au of the FU Ori disk, but confirmation requires more complete spectral sampling in the centimeter bands.
Probing the origin of UX Ori-type variability in the YSO binary CO Ori with VLTI/GRAVITY
在年轻的恒星物体（YSO）的二进制CO猎户座的主要恒星显示UX猎户座型的变化：不规则的，高振幅的光学和近红外光度波动的通量最小值与偏振最大值相吻合。这归因于局部不透明度的变化。在CO Ori A中，这些变化表现出12.4年的周期。在这里，我们调查的物理起源的波动不透明度和它的周期性使用干涉观测的CO Ori使用VLTI/重力。连续K带的环主和环二次发射边缘空间解决的第一次，而Br $γ$发射检测到的光谱中的二次。我们估计的光谱类型范围为CO Ori B的K2-K5假设的视觉消光，$A_{\rm{V}}=2$和430 pc的距离。根据连续光谱的几何模型，环一次辐射与中心点源加上高斯分量一致，其半高宽为2.31 $\pm$ 0.04毫弧秒（mas），倾斜角为30.2 $\pm$ 2.2 $^{\circ}$，主轴位置角为40 $\pm$ 6 $^{\circ}$。这个倾角比其他UX Ori-type恒星的星盘所报告的倾角要低，提供了第一个迹象，即UX Ori-type现象可能是由于星盘外部的星周物质的波动而产生的，例如在尘埃流出中。需要一个额外的宽的对称高斯分量来拟合CO Ori B的能级，这表明散射光的贡献。最后，关闭阶段的CO Ori A被用来调查是否12.4年的周期性与未检测到的第三个组成部分，如前所述。我们排除了在CO Ori A的~7.3-20质量范围内对K带通量贡献超过3.…
The close environment of high-mass X-ray binaries at high angular resolution I. VLTI/AMBER and VLTI/PIONIER near-infrared interferometric observations of Vela X-1
An interferometric study of the post-AGB binary 89 Herculis I Spatially resolving the continuum circumstellar environment at optical and near-IR wavelengths with the VLTI, NPOI, IOTA, PTI, and the CHARA Array
An interferometric mid-infrared study of the eruptive star binary Z CMa with MATISSE/VLTI. I. Imaging the protoplanetary disks during the 2023 outburst
The complex inner disk of the Herbig Ae star HD 100453 with VLTI/MATISSE
Leiden University（莱顿大学）；Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, HUN-REN（孔科利天文台，匈牙利研究网络天文学与地球科学研究中心）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内库克天文学研究所）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学，蔚蓝海岸天文台，法国国家科学研究中心，拉格朗日实验室）；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学，法国国家科学研究中心，IPAG）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）
Exomoon search with VLTI/GRAVITY around the substellar companion HD 206893 B
Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS（巴黎天文台，PSL大学，索邦大学，巴黎西岱大学，塞吉-蓬图瓦兹大学，法国国家科学研究中心）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University（西北大学天体物理学跨学科探索与研究中心及物理与天文学系）；European Southern Observatory（欧洲南方天文台）；Department of Physics & Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学物理与天文学系）；Space Telescope Science Institute（太空望远镜科学研究所）
The 2008-2009 outburst of the young binary system Z CMa unraveled by interferometry with high spectral resolution
Z CMa是一个年轻的双星系统，由一个Herbig主星和一个FU Ori伴星组成。这两个组成部分似乎都被活跃的吸积盘所包围，赫比格B 0还伴随着一个喷流。2008年11月，K.格兰金发现Z CMa爆发的幅度比过去25年中记录的任何光度变化都要大。为了研究爆发发生的最内部区域并了解其起源，我们于2009年12月在中等和高光谱分辨率模式下用ABER/VLTI观测了跨越Brγ发射线的两个二元分量。我们的观测结果表明，赫比格Be，负责增加的亮度，也产生了强大的Brγ发射，他们允许我们从不同的来源，通过定位在每个速度通过线的发射解开。考虑一个模型的开普勒磁盘单独未能再现不对称的光谱天体测量，这表明一个流出的主要贡献。
