Scalable, Advanced Machine Learning-based Approaches for Stellar Flare Identification: Application to TESS short-cadence Data and Analysis of a New Flare Catalogue
Chia-Lung Lin, Daniel Apai, Mark S. Giampapa, Wing-Huen Ip
We apply multi-algorithm machine learning models to TESS 2-minute survey data from Sectors 1-72 to identify stellar flares. Models trained with Deep Neural Network, Random Forest, and XGBoost algorithms, respectively, utilized four flare light curve characteristics as input features. Model performance is evaluated using accuracy, precision, recall, and F1-score metrics, all exceeding 94%. Validation against previously reported TESS M dwarf flare identifications showed that our models successfully recovered over 92% of the flares while detecting $\sim2,000$ more small events, thus extending the detection sensitivity of previous work. After processing 1.3 million light curves, our models identified nearly 18,000 flare stars and 250,000 flares. We present an extensive catalog documenting both flare and stellar properties. We find strong correlations in total flare energy and flare amplitude with color, in agreement with previous studies. Flare frequency distributions are analyzed, refining power-law slopes for flare behavior with the frequency uncertainties due to the detection incompleteness of low-amplitude events. We determine rotation periods for $\sim120,000$ stars thus yielding the relationship between rotation period and flare activity. We find that the transition in rotation period between the saturated and unsaturated regimes in flare energy coincides with the same transition in rotation period separating the saturated and unsaturated levels in coronal X-ray emission. We find that X-ray emission increases more rapidly with flare luminosity in earlier-type and unsaturated stars, indicating more efficient coronal heating in these objects. Additionally, we detect flares in white dwarfs and hot subdwarfs that are likely arising from unresolved low-mass companions.
Diverse Variability of O and B Stars Revealed from 2-minute Cadence Light Curves in Sectors 1 and 2 of the TESS Mission: Selection of an Asteroseismic Sample
Fast-Cadence TESS Photometry and Doppler Tomography of the Asynchronous Polar CD Ind: A Revised Accretion Geometry from Newly Proposed Spin and Orbital Periods
Large-scale variability in macroturbulence driven by pulsations in the rapidly rotating massive star Zeta Oph from high-cadence ESPRESSO spectroscopy and TESS photometry
Rapidly oscillating Ap stars observed with TESS. The LAMOST Ap sample and 49 Cam
Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto（波尔图大学空间与天体物理研究所）；Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto（波尔图大学理学院物理与天文学系）；South African Astronomical Observatory（南非天文台）；School of Physics, Engineering and Technology, University of York（约克大学物理、工程与技术学院）；DTU Space, Technical University of Denmark（丹麦技术大学空间中心）；Centre for Space Research, North-West University（西北大学太空研究中心）；Jeremiah Horrocks Institute, University of Lancashire（兰开夏大学杰里米亚·霍罗克斯研究所）；Department of Astronomy, Cornell University（康奈尔大学天文学系）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学、法国原子能与替代能源委员会、法国国家科学研究中心、天体物理学与信息分子研究所）
A Catalogue of Orbital Periods of Cataclysmic Variables and Candidates from TESS Observations
Durham University（杜伦大学）；INAF – Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；South African Astronomical Observatory（南非天文台）；University of Cape Town（开普敦大学）；Eberhard Karls Universität Tübingen（蒂宾根大学）；NASA Ames Research Center（美国宇航局艾姆斯研究中心）
Doppler imaging combined with high-cadence photometry. I. Revisiting the surface of a pre-main-sequence flare star
Kyoto University（京都大学）；Ankara University（安卡拉大学）；Max-Planck-Institut für Sonnensystemforschung（马克斯·普朗克太阳系研究所）；Hitotsubashi University（一桥大学）；The Hakubi Center for Advanced Research, Kyoto University（京都大学哈库比高级研究中心）；NASA Goddard Space Flight Center（美国国家航空航天局戈达德太空飞行中心）；The Catholic University of America（美利坚天主教大学）；National Astronomical Observatory of Japan（日本国立天文台）；Nishi-Harima Astronomical Observatory, University of Hyogo（兵库县立西播磨天文台）
High-Time-Cadence Spectroscopy and Photometry of Stellar Flares on M-dwarf YZ Canis Minoris with Seimei Telescope and TESS. I. Discovery of Rapid and Short-Duration Prominence Eruptions
Microlensify: a Transformer Based Machine Learning Classifier for Microlensing Events Trained on TESS Light Curves
Institute for Advanced Studies in Basic Sciences (IASBS)（基础科学高等研究院）；Lehigh University（利哈伊大学）；University of Virginia（弗吉尼亚大学）；Isfahan University of Technology（伊斯法罕理工大学）；University of Delaware（特拉华大学）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密森天体物理中心）
A very rapidly rotating white dwarf in nova YZ Reticuli
Universidad Nacional de Hurlingham (UNAHUR)（乌尔哈林国立大学）；Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET)（国家科学研究委员会）；South African Astronomical Observatory（南非天文台）；International Gemini Observatory/NSF NOIRLab（国际双子座天文台/美国国家光学红外天文实验室）；INAF-Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Department of Astronomy, University of Wisconsin（威斯康星大学天文学系）；Centre for Extragalactic Astronomy, Department of Physics, Durham University（达勒姆大学物理学系河外天文中心）；INAF – Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Advanced Technologies Research Institute, Faculty of Materials Science and Technology in Trnava, Slovak University of Technology in Bratislava（布拉迪斯拉发斯洛伐克技术大学特尔纳瓦材料科学与技术学院先进技术研究所）
High-Time-Cadence Spectroscopy and Photometry of Stellar Flares on M-dwarf YZ Canis Minoris with Seimei Telescope and TESS. II. Statistical Properties of Blue/Red Asymmetries in the H$α$ Line
Magnetic OB[A] Stars with TESS: probing their Evolutionary and Rotational properties (MOBSTER) - I. First-light observations of known magnetic B and A stars
Understanding Accretion Variability Through TESS Observations of Taurus
解释被称为经典金牛T星的吸积、年轻、低质量恒星的短时间尺度变化仍然是一个开放的任务。来自凌日系外行星勘测卫星（\textit{TESS}）的长达一个月的连续光变曲线已经可以用于数百颗金牛座T星。有了这一庞大的数据集，确定之间的联系所观察到的变化\TESS和短时间尺度吸积变化是有价值的吸积过程的特点。为此，我们获得了短节奏的\TESS观测金牛座恒星形成区域的14颗金牛座T星，同时地面，UBVRI波段测光作为吸积诊断。此外，我们结合我们的数据集与以前公布的同时NUV-NIR \textit{Hubble Space Telescope}光谱的一个成员的样品。我们发现的证据表明，在\TESS光变曲线中观察到的短时间尺度的变化可以归因于吸积率的变化，但注意到显着的分散在不同的夜晚和对象。我们确定在我们的数据集内的时间滞后的提示，增加在较短的波长，我们建议可能是纵向的吸积柱的密度分层的证据。我们的研究结果强调，同时，多波长观测仍然是至关重要的，为这些恒星的观测变化提供背景。
The rise of the black hole X-ray binary AT2019wey observed with TESS
American Museum of Natural History（美国自然历史博物馆）；CUNY City College of the City University of New York（纽约市立大学城市学院）；Columbia University（哥伦比亚大学）；Center for Computational Astrophysics, Flatiron Institute（Flatiron研究所计算天体物理学中心）
Revisiting bright delta Scuti stars and their period-luminosity relation with TESS and Gaia DR3
University of Pennsylvania（宾夕法尼亚大学）；Sydney Institute for Astronomy, School of Physics, University of Sydney（悉尼大学物理学院天体物理研究所）；Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University（奥胡斯大学物理与天文系恒星天体物理中心）；Centre for Astrophysics, University of Southern Queensland（昆士兰南部大学天体物理中心）；Institute for Astronomy, University of Hawai‘i（夏威夷大学天体物理研究所）
Luminaries in the Sky: The TESS Legacy Sample of Bright Stars. I. Asteroseismic detections in naked-eye main-sequence and sub-giant solar-like oscillators
