Variability in the infrared emission from disks around pre-main sequence stars over the course of days to weeks appears to be common, but the physical cause of the changes in disk structure are not constrained. Here we present coordinated monitoring of one young cluster with the Spitzer and Chandra space telescopes aimed at studying the physical source of the variability. In fall 2011 we obtained ten epochs of Chandra ACIS photometry over a period of 30 days with a roughly 3 day cadence contemporaneous with 20 epochs of Spitzer [3.6],[4.5] photometry over 40 days with a roughly 2 day cadence of the IC 348 cluster. This cadence allows us to search for week to month long responses of the infrared emission to changes in the high-energy flux. We find no strong evidence for a direct link between the X-ray and infrared variability on these timescales among 39 cluster members with circumstellar disks. There is no significant correlation between the shape of the infrared and X-ray light curves, or between the size of the X-ray and infrared variability. Among the stars with an X-ray flare none showed evidence of a correlated change in the infrared photometry on timescales of days to weeks following the flare. This lack of connection implies that X-ray heating of the planet forming region of the disk is not significant, although we cannot rule out rapid or instantaneous changes in infrared emission.
Ruling out nucleonic direct Urca cooling in low-mass neutron stars using nuclear data
Université de Caen Normandie, ENSICAEN, CNRS/IN2P3, LPC Caen UMR6534（卡昂诺曼底大学，ENSICAEN，CNRS/IN2P3，LPC Caen UMR6534）；Dipartimento di Fisica “Aldo Pontremoli”, Università degli Studi di Milano（米兰大学物理系“Aldo Pontremoli”）；INFN, Sezione di Milano（意大利国家核物理研究所，米兰分部）；Department of Physics, University of Houston（休斯顿大学物理系）；Grand Accélérateur National d’Ions Lourds (GANIL), CEA/DRF-CNRS/IN2P3（重离子国家大型加速器（GANIL），CEA/DRF-CNRS/IN2P3）
Multi-Observatory Study of Young Stellar Energetic Flares (MORYSEF): No Evidence For Abnormally Strong Stellar Magnetic Fields After Powerful X-ray Flares
Ongoing flyby in the young multiple system UX Tauri
我们目前的观测年轻的多系统UX金牛座寻找拱盘和动力学相互作用的迹象。获得了J波段和H波段的SPHERE/IRDIS深差极化图像。我们还使用了ALMA档案CO数据。在UX Tau A盘发出的散射光中可以很好地检测到大的延伸螺旋。南部螺旋形成了连接UX Tau A和C的桥梁。这些螺旋，包括连接两颗恒星的桥梁，都有一个由ALMA看到的CO（3-2）对应物。在散射光中检测UX Tau C的盘。它比UX Tau A的圆盘小得多，并且沿着不同的位置角有一个主轴，这表明没有对准。我们进行了PHANTOM SPH流体动力学模型来解释数据。散射光螺旋，CO发射螺旋和旋转盘的速度模式，以及UX Tau C盘的紧凑性都指向一个场景，其中UX Tau A最近（大约1000年）被UX Tau C近距离通过而扰动。
A JWST, ALMA and VLA survey of the Ophiuchus-A star-forming region: Unveiling hidden dust mass and connecting infrared outflows to their radio origins
University of Leeds（利兹大学）；Universitat de Barcelona（巴塞罗那大学）；Institut d’Estudis Espacials de Catalunya（加泰罗尼亚空间研究所）；National Sun Yat-Sen University（国立中山大学）；National Taiwan Normal University（国立台湾师范大学）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）
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）
Stellar mergers and chemical element mixing: implications for the metamorphic stellar evolution in AGN disks
Canadian Institute for Theoretical Astrophysics, University of Toronto（多伦多大学理论天体物理研究所）；TAPIR, MC 350-17, California Institute of Technology（加州理工学院）；Department of Astronomy and Astrophysics, University of California, Santa Cruz（加州大学圣克鲁兹分校天文与天体物理系）；Institute for Advanced Study, Tsinghua University（清华大学高等研究院）；Department of Astronomy, Westlake University（西湖大学天文系）
