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arXiv 2022年

作者： Li, Jiangdan Onken, Christopher A. Wolf, Christian Németh, Péter Bessell, Mike Li, Zhenwei Zhang, Xiaobin Li, Jiao Wang, Luqian Li, Lifang Luo, Yangping Chen, Hailiang Ji, Kaifan Chen, Xuefei Han, Zhanwen 396 Yangfangwang Guandu District Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650011 China University of Chinese Academy of Sciences Beijing100049 China Research School of Astronomy and Astrophysics Australian National University Weston CreekACT2611 Australia Centre for Gravitational Astrophysics Australian National University CanberraACT2600 Australia Astronomical Institute of the Czech Academy of Sciences OndřejovCZ-25165 Czech Republic *** Fő tér 1 Malomsok8533 Hungary Key Laboratory of Optical Astronomy National Astronomical Observatories CAS Beijing100012 China Key Lab of Space Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Department of Astronomy China West Normal University Nanchong637002 China

Binaries consisting of a hot subdwarf star and an accreting white dwarf (WD) are sources of gravitational wave radiation at low frequencies and possible progenitors of type Ia supernovae if the WD mass is large enough. Here, we report the discovery of the third binary known of this kind: it consists of a hot subdwarf O (sdO) star and a WD with an orbital period of 3.495 hours and an orbital shrinkage of 0.1 s in 6 yr. The sdO star overfills its Roche lobe and likely transfers mass to the WD via an accretion disk. From spectroscopy, we obtain an effective temperature of Teff = 54 240 ± 1 840 K and a surface gravity of log g = 4.841 ± 0.108 for the sdO star. From the light curve analysis, we obtain a sdO mass of MsdO = 0.55 M☉ and a mass ratio of q = MWD/MsdO = 0.738 ± 0.001. Also, we estimate that the disk has a radius of ∼ 0.41R☉ and a thickness of ∼ 0.18R☉. The origin of this binary is probably a common envelope ejection channel, where the progenitor of the sdO star is either an RGB star or, more likely, an early AGB star;the sdO star will subsequently evolve into a WD and merge with its WD companion, likely resulting in an R CrB star. The outstanding feature in the spectrum of this object is strong Ca H&K lines, which are blueshifted by ∼200 km/s and likely originate from the recently ejected common envelope, and we estimated that the remnant CE material in the binary system has a density ∼ 6 × 10−10g/cm3 Copyright © 2022, The Authors. All rights reserved.

关键词： White dwarfs

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Starspot evolution, differential rotation and correlation between chromospheric and photospheric activities on kepler-411

arXiv

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arXiv 2020年

作者： Xu, Fukun Gu, Shenghong Ioannidis, Panos Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Hamburger Sternwarte Universität Hamburg Gojenbergsweg 112 Hamburg21029 Germany School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China

We present an analysis of the starspot evolution, the surface differential rotation (SDR), the correlation between chromospheric activity indicators and the spatial connection between chromospheric and photospheric activities on the active star Kepler-411, using time series photometry over 4 years from Kepler, and spectroscopic data from Keck I 10-m telescope and Lijiang 2.4-m telescope. We constructed the light curve by re-performing photometry and reduction from the Target Pixel Files and Cotrending Basis Vectors with a manually redefined aperture using the software PyKE3. An efficient program, GEMC_LCM, was developed to apply a two-spots model to chosen light curve segments with three spot groups at fixed latitudes (30◦, 45◦), (30◦, 60◦) and (45◦, 60◦). We found a periodic variation of the starspots at period of about 660 days which independs on spot latitudes, and estimated the lower limit of SDR as Peq = 9.7810(0.0169) days and α = 0.1016(0.0023). Simultaneously, the relative variations of chromospheric activity indicators were derived by subtracting the overall mean spectrum from individual spectrum. It is found that Ca II H and K emissions are strongly correlated with each other, and there also exists a correlation between Hα and Ca II H & K emissions, with large dispersion, in accordance with previous results. Furthermore we find the correlation between Ca II H and K emissions is different in 2011 and 2012. The chromospheric emission variation shows a highly spatial anti-correlation with the light curve, suggesting a spatial connection between the chromospheric active region and spot region. Copyright © 2020, The Authors. All rights reserved.

关键词： Chromophores

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Synchrotron Radiation Dominates the Extremely Bright GRB 221009A

arXiv

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arXiv 2023年

作者： Yang, Jun Zhao, Xiao-Hong Yan, Zhenyu Wang, Xiangyu Ivy Zhang, Yan-Qiu An, Zheng-Hua Cai, Ce Li, Xin-Qiao Li, Zihan Liu, Jia-Cong Liu, Zi-Ke Ma, Xiang Meng, Yan-Zhi Peng, Wen-Xi Qiao, Rui Shao, Lang Song, Li-Ming Tan, Wen-Jun Wang, Ping Wang, Chen-Wei Wen, Xiang-Yang Xiao, Shuo Xue, Wang-Chen Yang, Yu-Han Yin, Yihan Zhang, Bing Zhang, Fan Zhang, Shuai Zhang, Shuang-Nan Zheng, Chao Zheng, Shi-Jie Xiong, Shao-Lin Zhang, Bin-Bin School of Astronomy and Space Science Nanjing University Nanjing210093 China Key Laboratory of Modern Astronomy and Astrophysics Nanjing University Ministry of Education China Yunnan Observatories Chinese Academy of Sciences Kunming China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China University of Chinese Academy of Sciences Beijing100049 China College of Physics Hebei Key Laboratory of Photophysics Research and Application Hebei Normal University Hebei Shijiazhuang050024 China College of Physics Hebei Normal University Shijiazhuang050024 China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Guiyang550001 China Department of Physics University of Rome "Tor Vergata" via della Ricerca Scientifica 1 RomeI-00133 Italy School of Physics Nanjing University Nanjing210093 China Department of Physics and Astronomy University of Nevada Las Vegas NV89154 United States Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China

The brightest Gamma-ray burst, GRB 221009A, has spurred numerous theoretical investigations, with particular attention paid to the origins of ultra-high energy TeV photons during the prompt phase. However, analyzing the mechanism of radiation of photons in the ∼MeV range has been difficult because the high flux causes pile-up and saturation effects in most GRB detectors. In this letter, we present systematic modeling of the time-resolved spectra of the GRB using unsaturated data obtained from Fermi/GBM (precursor) and SATech-01/GECAM-C (main emission and flare). Our approach incorporates the synchrotron radiation model, which assumes an expanding emission region with relativistic speed and a global magnetic field that decays with radius, and successfully fits such a model to the observational data. Our results indicate that the spectra of the burst are fully in accordance with a synchrotron origin from relativistic electrons accelerated at a large emission radius. The lack of thermal emission in the prompt emission spectra supports a Poynting-flux-dominated jet composition. Copyright © 2023, The Authors. All rights reserved.

关键词： Synchrotron radiation

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An Automatic Detection Method of Solar Radio Burst based on Otsu Binarization

An Automatic Detection Method of Solar Radio Burst based on ...

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2019第十一届数字图像处理国际会议

作者： Menglin Jin Guowu Yuan Guannan Gao Liang Dong Hao Zhou Yun Gao Shaojie Guo Min Wang School Of Information Science And Engineering Yunnan University Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Yunnan Observatories Chinese Academy of Sciences

With the development of solar radio spectrometer,it is difficult to process a large number of observed data quickly by manual detection *** automatic detection method of solar radio burst based on Otsu binarization is proposed in this *** this method,channel normalization is used to denoise the original solar radio *** experimental comparison,Otsu method is selected as a binary method of solar radio spectrum,and Open and Close operations are used to smooth the binary *** show that the proposed method for automatic detection of solar radio bursts is effective.

关键词： Solar radio spectrum image denoise binarization threshold setting method

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Flares hunting in hot subdwarf and white dwarf stars from Cycles 1-5 of TESS photometry

arXiv

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arXiv 2024年

作者： Xing, Keyu Zong, Weikai Silvotti, Roberto Fu, Jian-Ning Charpinet, Stéphane Cang, Tianqi Hermes, J.J. Ma, Xiao-Yu Wang, Haotian Wang, Xuan Wu, Tao Wang, Jiaxin Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Beijing102206 China Department of Astronomy Beijing Normal University Beijing100875 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China INAF-Osservatorio Astrofisico di Torino strada dell’Osservatorio 20 Pino TorineseI-10025 Italy Institut de Recherche en Astrophysique et Planétologie CNRS Université de Toulouse CNES 14 Avenue Edouard Belin ToulouseF-31400 France Department of Astronomy Institute for Astrophysical Research Boston University 725 Commonwealth Avenue BostonMA02215 United States Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China College of Science Chongqing University of Posts and Telecommunications Chongqing400065 China

Stellar flares are critical phenomena on stellar surfaces, which are closely tied to stellar magnetism. While extensively studied in main-sequence (MS) stars, their occurrence in evolved compact stars, specifically hot subdwarfs and white dwarfs (WDs), remains scarcely explored. Based on Cycles 1-5 of TESS photometry, we conducted a pioneering survey of flare events in ∼12 000 compact stars, corresponding to ∼38 000 light curves with 2-minute cadence. Through dedicated techniques for detrending light curves, identifying preliminary flare candidates, and validating them via machine learning, we established a catalog of 1016 flares from 193 compact stars, including 182 from 58 sdB/sdO stars and 834 from 135 WDs, respectively. However, all flaring compact stars showed signs of contamination from nearby objects or companion stars, preventing sole attribution of the detected flares. For WDs, it is highly probable that the flares originated from their cool MS companions. In contrast, the higher luminosities of sdB/sdO stars diminish companion contributions, suggesting that detected flares originated from sdB/sdO stars themselves or through close magnetic interactions with companions. Focusing on a refined sample of 23 flares from 13 sdB/sdO stars, we found their flare frequency distributions were slightly divergent from those of cool MS stars;instead, they resemble those of hot B/A-type MS stars having radiative envelopes. This similarity implies the flares on sdB/sdO stars, if these flares did originate from them, may share underlying mechanisms with hot MS stars, which warrants further investigation. © 2024, CC BY.

关键词： Machine learning

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Science objectives of the Einstein Probe mission

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Science China(Physics,Mechanics & Astronomy) 2025年第3期68卷 1-60页

作者： Weimin Yuan Lixin Dai Hua Feng Chichuan Jin Peter Jonker Erik Kuulkers Yuan Liu Kirpal Nandra Paul O’Brien Luigi Piro Arne Rau Nanda Rea Jeremy Sanders Lian Tao Junfeng Wang Xuefeng Wu Bing Zhang Shuangnan Zhang Shunke Ai Johannes Buchner Esra Bulbul Hechao Chen Minghua Chen Yong Chen Yu-Peng Chen Alexis Coleiro Francesco Coti Zelati Zigao Dai Xilong Fan Zhou Fan Susanne Friedrich He Gao Chong Ge Mingyu Ge Jinjun Geng Giancarlo Ghirlanda Giulia Gianfagna Lijun Gou Sebastien Guillot´ Xian Hou Jingwei Hu Yongfeng Huang Long Ji Shumei Jia S.Komossa Albert K.H.Kong Lin Lan An Li Ang Li Chengkui Li Dongyue Li Jian Li Zhaosheng Li Zhixing Ling Ang Liu Jinzhong Liu Liangduan Liu Zhu Liu Jiawei Luo Ruican Ma Pierre Maggi Chandreyee Maitra Alessio Marino Stephen Chi-Yung Ng Haiwu Pan Surangkhana Rukdee Roberto Soria Hui Sun Pak-Hin Thomas Tam Aishwarya Linesh Thakur Hui Tian Eleonora Troja Wei Wang Xiangyu Wang Yanan Wang Junjie Wei Sixiang Wen Jianfeng Wu Ting Wu Di Xiao Dong Xu Renxin Xu Yanjun Xu Yu Xu Haonan Yang Bei You Heng Yu Yunwei Yu Binbin Zhang Chen Zhang Guobao Zhang Liang Zhang Wenda Zhang Yu Zhang Ping Zhou Zecheng Zou National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Astronomy and Space Sciences University of Chinese Academy of SciencesBeijing 100049China Department of Physics University of Hong KongPokfulam RoadHong Kong 999077China Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Department of Astrophysics/IMAPP Radboud UniversityNijmegen6500 GLthe Netherlands SRON Netherlands Institute for Space ResearchLeiden2333 CAthe Netherlands ESA/ESTEC Noordwijk2201 AZthe Netherlands Max Planck Institute for Extraterrestrial Physics Garching85748Germany School of Physics and Astronomy University of LeicesterLeicesterLE17RHUK INAF-Istituto di Astrofisica e Planetologia Spaziali Rome00133Italy Institute of Space Sciences(ICE) CSICCampus UABBarcelonaE-08193Spain Institut d’Estudis Espacials de Catalunya(IEEC) BarcelonaE-08034Spain Department of Astronomy Xiamen UniversityXiamen 361005China Purple Mountain Observatory Chinese Academy of SciencesNanjing 210023China School of Astronomy and Space Sciences University of Science and Technology of ChinaHefei 230026China Nevada Center for Astrophysics University of NevadaLas VegasNV 89154USA Department of Physics and Astronomy University of NevadaLas VegasNV 89154USA Department of Astronomy School of Physics and TechnologyWuhan UniversityWuhan 430072China School of Physics and Astronomy Yunnan UniversityKunming 650500China Xinjiang Astronomical Observatory Chinese Academy of SciencesUrumqi 830011China Universit´e Paris Cit´e CNRSAstroparticule et CosmologieParisF-75013France Department of Astronomy University of Science and Technology of ChinaHefei 230026China Institute for Frontier in Astronomy and Astrophysics Beijing Normal UniversityBeijing 102206China Department of Astronomy Beijing Normal UniversityBeijing 100875China INAF-Osservatorio Astronomico di Brera Merate(LC)I-23807Italy INFN-sezione di Milano-Bicocca Milano(M

The Einstein Probe(EP)is an interdisciplinary mission of time-domain and X-ray *** with a wide-field lobstereye X-ray focusing imager,EP will discover cosmic X-ray transients and monitor the X-ray variability of known sources in 0.5-4 keV,at a combination of detecting sensitivity and cadence that is not accessible to the previous and current wide-field monitoring *** can perform quick characterisation of transients or outbursts with a Wolter-I X-ray telescope *** this paper,the science objectives of the EP mission are *** is expected to enlarge the sample of previously known or predicted but rare types of transients with a wide range of *** them,fast extragalactic transients will be surveyed systematically in soft X-rays,which includeγ-ray bursts and their variants,supernova shock breakouts,and the predicted X-ray transients associated with binary neutron star *** will detect X-ray tidal disruption events and outbursts from active galactic nuclei,possibly at an early phase of the flares for *** will monitor the variability and outbursts of X-rays from white dwarfs,neutron stars and black holes in our and neighbouring galaxies at flux levels fainter than those detectable by the current instruments,and is expected to discover new objects.A large sample of stellar X-ray flares will also be detected and *** the era of multi-messenger astronomy,EP has the potential of detecting the possible X-ray counterparts of gravitational wave events,neutrino sources,and ultra-high energyγ-ray and cosmic ray *** is expected to help advance the studies of extreme objects and phenomena revealed in the dynamic X-ray universe,and their underlying physical *** EP's strength in time-domain science,its follow-up telescope,with excellent performance,will also enable advances in many areas of X-ray astronomy.

关键词： Einstein Probe X-ray astronomy X-ray telescopes time-domain astronomy transients variability

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He-shell flashes on the surface of oxygen-neon white dwarfs

arXiv

引用

arXiv 2020年

作者： Guo, Yunlang Liu, Dongdong Wu, Chengyuan Wang, Bo Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China Tsinghua University Beijing100084 China

Accretion induced collapse (AIC) may be responsible for the formation of some interesting neutron star binaries, e.g., millisecond pulsars, intermediate-mass binary pulsars, etc. It has been suggested that oxygen-neon white dwarfs (ONe WDs) can increase their mass to the Chandrasekhar limit by multiple He-shell flashes, leading to AIC events. However, the properties of He-shell flashes on the surface of ONe WDs are still not well understood. In this article, we aim to study He-shell flashes on the surface of ONe WDs in a systematic approach. We investigated the long-term evolution of ONe WDs accreting He-rich material with various constant mass-accretion rates by time-dependent calculations with the stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA), in which the initial ONe WD masses range from 1.1 to 1.35 M☉. We found that the mass-retention efficiency increases with the ONe WD mass and the mass-accretion rate, whereas both the nova cycle duration and the ignition mass decrease with the ONe WD mass and the mass-accretion rate. We also present the nuclear products in different accretion scenarios. The results presented in this article can be used in the future binary population synthesis studies of AIC events. Copyright © 2020, The Authors. All rights reserved.

关键词： White dwarfs

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AT2023lli: A Tidal Disruption Event with Prominent Optical Early Bump and Delayed Episodic X-ray Emission

arXiv

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arXiv 2024年

作者： Huang, Shifeng Jiang, Ning Zhu, Jiazheng Wang, Yibo Wang, Tinggui Wang, Shan-Qin Gan, Wen-Pei Liang, En-Wei Qin, Yu-Jing Lin, Zheyu Xu, Lin-Na Cai, Min-Xuan Jiang, Ji-An Kong, Xu Li, Jiaxun Li, Long Wang, Jian-Guo Xu, Ze-Lin Xue, Yongquan Yuan, Ye-Fei Cheng, Jingquan Fan, Lulu Gao, Jie Hu, Lei Hu, Weida Li, Bin Li, Feng Liang, Ming Liu, Hao Liu, Wei Lou, Zheng Luo, Wentao Qian, Yuan Tang, Jinlong Wan, Zhen Wang, Hairen Wang, Jian Yang, Ji Yao, Dazhi Zhang, Hongfei Zhang, Xiaoling Zhao, Wen Zheng, Xianzhong Zhu, Qingfeng Zuo, Yingxi CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China School of Astronomy and Space Sciences University of Science and Technology of China Hefei230026 China Institute of Deep Space Sciences Deep Space Exploration Laboratory Hefei230026 China Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and Technology Guangxi University Nanning530004 China Nanjing Hopes Technology Co. Ltd. Pukou District Nanjing210000 China Division of Physics Mathematics and Astronomy California Institute of Technology 1200 E California Blvd. PasadenaCA91125 United States National Astronomical Observatory of Japan National Institutes of Natural Sciences Tokyo181-8588 Japan Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Kunming650011 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China State Key Laboratory of Particle Detection and Electronics University of Science and Technology of China Hefei230026 China McWilliams Center for Cosmology Department of Physics Carnegie Mellon University 5000 Forbes Ave PittsburghPA15213 United States Department of Physics University of California Santa Barbara Santa BarbaraCA93106 United States 950 N Cherry Ave TucsonAZ85726 United States Institute of Optics and Electronics Chinese Academy of Sciences Chengdu610209 China

High-cadence, multiwavelength observations have continuously revealed the diversity of tidal disruption events (TDEs), thus greatly advancing our knowledge and understanding of TDEs. In this work, we conducted an intensive optical-UV and X-ray follow-up campaign of TDE AT2023lli, and found a remarkable month-long bump in its UV/optical light curve nearly two months prior to maximum brightness. The bump represents the longest separation time from the main peak among known TDEs to date. The main UV/optical outburst declines as t−4.10, making it one of the fastest decaying optically selected TDEs. Furthermore, we detected sporadic X-ray emission 30 days after the UV/optical peak, accompanied by a reduction in the period of inactivity. It is proposed that the UV/optical bump could be caused by the self-intersection of the stream debris, whereas the primary peak is generated by the reprocessed emission of the accretion process. In addition, our results suggest that episodic X-ray radiation during the initial phase of decline may be due to the patched obscurer surrounding the accretion disk, a phenomenon associated with the inhomogeneous reprocessing process. The double TDE scenario, in which two stars are disrupted in sequence, is also a possible explanation for producing the observed early bump and main peak. We anticipate that the multicolor light curves of TDEs, especially in the very early stages, and the underlying physics can be better understood in the near future with the assistance of dedicated surveys such as the deep high-cadence survey of the 2.5-meter Wide Field Survey Telescope (WFST). © 2024, CC BY.

关键词： Luminance

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Mass-accreting white dwarfs and type Ia supernovae

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Research in Astronomy and Astrophysics 2018年第5期18卷 1-28页

作者： Bo Wang Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy ofSciences Kunming 650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing 100101 China University of Chinese Academy of Sciences Beijing 100049 China

Type Ia supernovae（SNe Ia） play a prominent role in understanding the evolution of the Universe. They are thought to be thermonuclear explosions of mass-accreting carbon-oxygen white dwarfs（CO WDs） in binaries, although the mass donors of the accreting WDs are still not well determined. In this article, I review recent studies on mass-accreting WDs, including H-and He-accreting WDs. I also review currently most studied progenitor models of SNe Ia, i.e., the single-degenerate model（including the WD＋MS channel, the WD＋RG channel and the WD＋He star channel）, the doubledegenerate model（including the violent merger scenario） and the sub-Chandrasekhar mass *** progress on these progenitor models is discussed, including the initial parameter space for producing SNe Ia, the binary evolutionary paths to SNe Ia, the progenitor candidates for SNe Ia, the possible surviving companion stars of SNe Ia, some observational constraints, etc. Some other potential progenitor models of SNe Ia are also summarized, including the hybrid CONe WD model, the core-degenerate model, the double WD collision model, the spin-up/spin-down model and the model of WDs near black holes. To date, it seems that two or more progenitor models are needed to explain the observed diversity among SNe Ia.

关键词： supernovae general - binaries close - stars evolution - white dwarfs

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A highly mutually-inclined, compact warm-Jupiter system KOI-984 ?

arXiv

引用

arXiv 2021年

作者： Sun, Leilei Ioannidis, Panagiotis Gu, Shenghong Schmitt, Jürgen H.M.M. Wang, Xiaobin Kouwenhoven, M.B.N. Perdelwitz, Volker Dotti, Francesco Flammini Czesla, Stefan Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Hamburger Sternwarte Universität Hamburg Gojenbergsweg 112 Hamburg21029 Germany School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China 111 Renai Rd. Suzhou Dushu Lake Science and Education Innovation District Suzhou Industrial Park Suzhou215123 China Department of Physics Ariel University Ariel40700 Israel

The discovery of a population of close-orbiting giant planets (≤ 1 au) has raised a number of questions about their origins and dynamical histories. These issues have still not yet been fully resolved, despite over 20 years of exoplanet detections and a large number of discovered exoplanets. In particular, it is unclear whether warm Jupiters (WJs) form in situ, or whether they migrate from further outside and are even currently migrating to form hot Jupiters (HJs). Here, we report the possible discovery and characterization of the planets in a highly mutually-inclined (Imut 45◦), compact two-planet system (KOI-984), in which the newly discovered warm Jupiter KOI-984c is on a 21.5-day, moderately eccentric (e 0.4) orbit, in addition to a previously known 4.3-day planet candidate KOI-984b. Meanwhile, the orbital configuration of a moderately inclined (Imut 15◦), low-mass (mc 24M⊕;Pb 8.6 days) perturbing planet near 1:2 mean motion resonace with KOI-984b could also well reproduce observed transit timing variations and transit duration variations of KOI-984b. Such an eccentric WJ with a close-in sibling would pose a challenge to the proposed formation and migration mechanisms of WJs, if the first scenario is supported with more evidences in near future;this system with several other well-measured inclined WJ systems (e.g., Kepler-419 and Kepler-108) may provide additional clues for the origin and dynamical histories of WJs. Copyright © 2021, The Authors. All rights reserved.

关键词： Extrasolar planets

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