The inner disk of RY Tau: evidence of stellar occultation by the disk atmosphere at the sublimation rim from K-band continuum interferometry
Claire L. Davies, Stefan Kraus, Tim J. Harries, John D. Monnier, Brian Kloppenborg, Alicia Aarnio, Fabien Baron, Rebeca Garcia Lopez, Rafael Millan-Gabet, Rober… 展开作者
Claire L. Davies, Stefan Kraus, Tim J. Harries, John D. Monnier, Brian Kloppenborg, Alicia Aarnio, Fabien Baron, Rebeca Garcia Lopez, Rafael Millan-Gabet, Robert Parks, Ettore Pedretti, Karine Perraut, Judit Sturmann, Laszlo Sturmann, Theo A. ten Brummelaar, Yamina Touhami
We present models of the inner region of the circumstellar disk of RY Tau which aim to explain our near-infrared ($K$-band: $2.1\,μ$m) interferometric observations while remaining consistent with the optical to near-infrared portions of the spectral energy distribution. Our sub-milliarcsecond resolution CHARA Array observations are supplemented with shorter baseline, archival data from PTI, KI and VLTI/GRAVITY and modeled using an axisymmetric Monte Carlo radiative transfer code. The $K$-band visibilities are well-fit by models incorporating a central star illuminating a disk with an inner edge shaped by dust sublimation at $0.210\pm0.005\,$au, assuming a viewing geometry adopted from millimeter interferometry ($65^{\circ}$ inclined with a disk major axis position angle of $23^{\circ}$). This sublimation radius is consistent with that expected of Silicate grains with a maximum size of $0.36-0.40\,μ$m contributing to the opacity and is an order of magnitude further from the star than the theoretical magnetospheric truncation radius. The visibilities on the longest baselines probed by CHARA indicate that we lack a clear line-of-sight to the stellar photosphere. Instead, our analysis shows that the central star is occulted by the disk surface layers close to the sublimation rim. While we do not see direct evidence of temporal variability in our multi-epoch CHARA observations, we suggest the aperiodic photometric variability of RY~Tau is likely related temporal and/or azimuthal variations in the structure of the disk surface layers.
The asymmetric structure of the inner disc around HD 142527 A with VLTI/MATISSE
HUN-REN Research Centre for Astronomy and Earth Sciences, Konkoly Observatory（匈牙利研究学院地球与天体科学研究中心孔科利天文台）；Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；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）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内贝克天体物理学研究所）；SRON Netherlands Institute for Space Research（荷兰空间研究所）
ALMA's sharpest view of IRAS 08544-4431: Unveiling the dust distribution asymmetries in the circumbinary disk
Macquarie University（麦考瑞大学）；INAF, Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；ATNF, CSIRO, Space and Astronomy（澳大利亚联邦科学与工业研究组织空间与天文部射电天文国家设施）；KU Leuven（荷语鲁汶大学）
Unlocking the dynamics of Young Stellar Objects: Time-Domain Interferometry with six 4-m class telescopes
Université Côte d’Azur, Observatoire de la Côte d’Azur（蔚蓝海岸大学，蔚蓝海岸天文台）；Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences（孔科利天文台，HUN-REN 天文学与地球科学研究中心）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Université 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（美国宇航局戈达德太空飞行中心）；ESO（欧洲南方天文台）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；ALMA Observatory（阿塔卡马大型毫米波/亚毫米波阵列天文台）；Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel（基尔大学理论与天体物理研究所）；Université Paris-Saclay, Université Paris Cité CEA, CNRS, AIM（巴黎萨克雷大学，巴黎西岱大学CEA，法国国家科学研究中心，AIM）；Nicolaus Copernicus Astronomical Centre, Polish Academy of Sciences（波兰科学院尼古拉·哥白尼天文学中心）；The CHARA Array of Georgia State University, Mount Wilson Observatory（佐治亚州立大学CHARA阵列，威尔逊山天文台）
