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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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Detection of δ Scuti pulsators in the eclipsing binaries observed by TESS

arXiv

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arXiv 2022年

作者： Chen, Xinghao Ding, Xu Cheng, Liantao Zhang, Xiaobin Li, Yan Ji, Kaifan Xiong, Jianping Li, Xuzhi Luo, Changqing Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 Kunming650216 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences P.O. Box 110 Kunming650216 China School of Opto-electronic Engineering Zaozhuang University Zaozhuang277160 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Deep Space Exploration Laboratory 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

Based on 2-minute cadence TESS data from sectors 1-50, we report the results of the systematic extraction of δ Scuti-type pulsations in the 6431 eclipsing binaries with orbital periods shorter than 13 days. A total number of 242 pulsators were found in those systems, including 143 new discoveries. We examined their pulsation properties based on the H-R diagram and the relationships between the dominant pulsation period Pdom, orbital period Porb, and effective temperature Teff. As a consequence, 216 targets are likely δ Scuti stars (123 new), 11 likely γ Doradus-δ Scuti hybrid stars (8 new), 5 likely β Cephei stars (4 new), 4 likely δ Scuti-γ Doradus hybrid stars (3 new), 3 likely Maia stars (3 new), 2 likely pulsating red giants (1 new), and a new unclassified star. As for the 6 new δ Scuti pulsators in eclipsing binaries with Porb dom/Porb ratio. This may indicate that Pdom and Porb are uncorrelated for them. Finally, we statistically analyzed the dominant pulsation periods of the 216 δ Scuti stars in eclipsing binaries. Those stars concentrate around 225 µHz and the proportion of stars in the high-frequency region is significantly higher than that of single stars, which could be ascribed to the mass transfer process. Copyright © 2022, The Authors. All rights reserved.

关键词： Mass transfer

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The formation of neutron star systems through accretion-induced collapse in white-dwarf binaries

arXiv

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arXiv 2020年

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

The accretion-induced collapse (AIC) scenario was proposed 40 years ago as an evolutionary end state of oxygen-neon white-dwarfs (ONe WDs), linking them to the formation of neutron star (NS) systems. However, there has been no direct detection of any AIC event so far, even though there exists a lot of indirect observational evidence. Meanwhile, the evolutionary pathways resulting in NS formation through AIC are still not well investigated. In this article, we review recent studies on the two classic progenitor models of AIC events, i.e., the single-degenerate model (including the ONe WD+MS/RG/He star channels and the CO WD+He star channel) and the doubledegenerate model (including the double CO WD channel, the double ONe WD channel and the ONe WD+CO WD channel). Recent progress on these progenitor models is reviewed, including the evolutionary scenarios leading to AIC events, the initial parameter space for producingAIC events, and the related objects (e.g., the pre-AIC systems and the post-AIC systems). For the single-degenerate model, the pre-AIC systems (i.e., the progenitor systems of AIC events) could potentially be identified as supersoft X-ray sources, symbiotics and cataclysmic variables (such as classical novae, recurrent novae, Ne novae and He novae) in the observations, whereas the post-AIC systems (i.e., NS systems) could potentially be identified as low-/intermediate-massX-ray binaries, and the resulting low-/intermediate-mass binary pulsars, most notably millisecond pulsars. For the doubledegenerate model, the pre-AIC systems are close double WDs with short orbital periods, whereas the post-AIC systems are single isolated NSs that may correspond to a specific kind of NSs with peculiar *** also review the predicted rates of AIC events, the mass distribution of NSs produced via AIC, and the gravitationalwave (GW) signals from double WDs that are potential GW sources in the Galaxy in the context of future spacebased GW detectors, such as LISA, T

关键词： White dwarfs

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OO Dra: An Algol-type binary formed through an extremely helium-poor mass accretion revealed by asteroseismology

arXiv

引用

arXiv 2021年

作者： Chen, Xinghao Zhang, Xiaobin Li, Yan Luo, Changqing Li, Xuzhi Su, Jie Chen, Xuefei Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 Kunming650216 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences P.O. Box 110 Kunming650216 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China

Based on the two-minutes TESS data, we analyzed intrinsic oscillations of the primary component and identified seven confident independent δ Scuti frequencies (f1, f2, f3, f4, f7, f11, and f12). Both of single-star evolutionary models and mass-accreting models are computed to reproduce the δ Scuti freqiencies. Fitting results of them match well with each other. The stellar parameters of the primary star yielded by asteroseismology are (Equation presented), which match well with the dynamic ones by the binary model. Furthermore, our asteroseismic results show that OO Dra is another Algol system that has just undergone the rapid mass-transfer stage. Fitting results of single-star evlutionary models indicate that the pulsator is helium-poor star with an age of 8.22+0.12−1.33 Myr, and the further mass-accreting models show that the primary star looks like an almost unevolved star formed by an extremely helium-poor mass accretion in Case A evolutionary scenario. Copyright © 2021, The Authors. All rights reserved.

关键词： Helium

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Velocity-resolved reverberation mapping of changing-look AGN NGC 2617

arXiv

引用

arXiv 2021年

作者： Feng, Hai-Cheng Liu, H.T. Bai, J.M. Yang, Zi-Xu Hu, Chen Li, Sha-Sha Yang, Sen Lu, Kai-Xing Xiao, Ming Yunnan Observatories Chinese Academy of Sciences KunmingYunnan650011 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences KunmingYunnan650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China

NGC 2617 has attracted a lot of attention after the detection of the changes in spectral type, and its geometry and kinematics of broad-line region (BLR) are still ambiguous. In this paper, we present the high cadence (∼ 2 days) reverberation mapping campaign of NGC 2617 from 2019 October to 2020 May undertaken at Lijiang 2.4 m telescope. For the first time, the velocity-resolved reverberation signature of the object was successfully detected. Both Hα and Hβ show an asymmetrical profile with a peak in the velocity-resolved time lags. For each of both lines, the lag of the line core is longer than those of the relevant wings, and the peak of the velocity-resolved lags is slightly blueshifted. These characteristics are not consistent with the theoretical prediction of the inflow, outflow or Keplerian disk model. Our observations give the time lags of Hα, Hβ, Hγ, and He i, with a ratio of τHα:τHβ:τHγ:τHe I= 1.27:1.00:0.89:0.20, which indicates a stratified structure in the BLR of the object. It is the first time that the lags of Hα and He i are obtained. Assuming a virial factor of f = 5.5 for dispersion width of line, the masses of black hole derived from Hα and Hβ are 23.8+5−2..47 and 21.1+3−4..84 × 106M☉, respectively. Our observed results indicate the complexity of the BLR of NGC 2617. Copyright © 2021, The Authors. All rights reserved.

关键词： Velocity

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A Roche Lobe-filling hot Subdwarf and White Dwarf Binary: possible detection of an ejected common envelope

arXiv

引用

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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A Short-lived Rejuvenation during the Decades-long Changing-look Transition in the Nucleus of Mrk 1018

arXiv

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arXiv 2024年

作者： Lu, Kai-Xing Li, Yan-Rong Wu, Qingwen Ho, Luis C. Zhang, Zhi-Xiang Feng, Hai-Cheng Li, Sha-Sha Chen, Yong-Jie Sun, Mouyuan Shu, Xinwen Guo, Wei-Jian Cheng, Cheng Wang, Jian-Guo Kim, Dongchan Wang, Jian-Min Bai, Jin-Ming Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Key Laboratory for Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences 19B Yuquan Road Beijing100049 China Department of Astronomy School of Physics Huazhong University of Science and Technology Luoyu Road 1037 Wuhan China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Department of Astronomy Xiamen University Fujian Xiamen361005 China Department of Physics Anhui Normal University Anhui Wuhu241002 China National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100101 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States

Changing-look active galactic nuclei (CL-AGNs), characterized by emerging or disappearing of broad lines accompanied with extreme continuum flux variability, have drawn much attention for their potential of revealing physical processes underlying AGN evolution. We perform seven-season spectroscopic monitoring on Mrk 1018, one of the earliest identified CL-AGN. Around 2020, we detect a full-cycle changing-look transition of Mrk 1018 within one year, associated with a nucleus outburst, which likely arise from the disk instability in the transition region between the outer standard rotation-dominated disk and inner advection-dominated accretion flow. Over the past forty-five years, the accretion rate of Mrk 1018 changed 1000 times and the maximum Eddington ratio reached 0.02. By investigating the relation between broad-line properties and Eddington ratio (Lbol/LEdd), we find strong evidence that the full-cycle type transition is regulated by accretion. There exists a turnover point in the Balmer decrement, which is observed for the first time. The broad Balmer lines change from a single peak in Type 1.0-1.2 to double peaks in Type 1.5-1.8 and the double-peak separation decreases with increasing accretion rate. We also find that the full width at half maximum (FWHM) of the broad Balmer lines obeys FWHM∝ (Lbol/LEdd)−0.27, as expected for a virialized BLR. The velocity dispersion σline follows a similar trend in Type 1.5-1.8, but displays a sharp increases in Type 1.0-1.2, resulting in a dramatic drop of FWHM/σline. These findings suggest that a virialized BLR together with accretion-dependent turbulent motions might be responsible for the diversity of BLR phenomena across AGN population. © 2024, CC BY.

关键词： Active Galactic Nuclei

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A potential mass-gap black hole in a wide binary with a circular orbit

arXiv

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arXiv 2024年

作者： Wang, Song Zhao, Xinlin Feng, Fabo Ge, Hongwei Shao, Yong Cui, Yingzhen Gao, Shijie Zhang, Lifu Wang, Pei Li, Xue Bai, Zhongrui Yuan, Hailong Huang, Yang Yuan, Haibo Zhang, Zhixiang Yi, Tuan Xiang, Maosheng Li, Zhenwei Li, Tanda Zhang, Junbo Zhang, Meng Han, Henggeng Fan, Dongwei Li, Xiangdong Chen, Xuefei Liu, Zhengwei Meng, Xiangcun Liu, Qingzhong Zhang, Haotong Gu, Wei-Min Liu, Jifeng Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Beijing102206 China School of Astronomy and Space Sciences University of Chinese Academy of Sciences Beijing100049 China Tsung-Dao Lee Institute Shanghai Jiao Tong University Shanghai201210 China School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China School of Astronomy and Space Science Nanjing University Nanjing210023 China Ministry of Education Nanjing210023 China CAS Key Laboratory of FAST NAOC Chinese Academy of Sciences Beijing100101 China Department of Astronomy Beijing Normal University Beijing100875 China Department of Astronomy Xiamen University Fujian Xiamen361005 China Department of Astronomy School of Physics Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008 China College of Physics and Electronic Engineering Qilu Normal University Jinan China New Cornerstone Science Laboratory National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China

Mass distribution of black holes identified through X-ray emission suggests a paucity of black holes in the mass range of 3 to 5 solar masses. Modified theories have been devised to explain this mass gap, and it is suggested that natal kicks during supernova explosion can more easily disrupt binaries with lower mass black holes. Although recent LIGO observations reveal the existence of compact remnants within this mass gap, the question of whether low-mass black holes can exist in binaries remains a matter of debate. Such a system is expected to be noninteracting without X-ray emission, and can be searched for using radial velocity and astrometric methods. Here we report Gaia DR3 3425577610762832384, a wide binary system including a red giant star and an unseen object, exhibiting an orbital period of approximately 880 days and near-zero eccentricity. Through the combination of radial velocity measurements from LAMOST and astrometric data from Gaia DR2 and DR3 catalogs, we determine a mass of (Equation presented) M☉ of the unseen component. This places the unseen companion within the mass gap, strongly suggesting the existence of binary systems containing low-mass black holes. More notably, the formation of its surprisingly wide circular orbit challenges current binary evolution and supernova explosion theories. Copyright © 2024, The Authors. All rights reserved.

关键词： Supernovae

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Unveiling Bifurcated Blue Straggler Sequences in NGC 2173: Insights from Binary evolution

arXiv

引用

arXiv 2025年

作者： Wang, Li Jiang, Dengkai Li, Chengyuan Deng, Licai Milone, Antonino P. Wang, Long School of Physics and Astronomy Sun Yat-sen University Daxue Road Zhuhai519082 China CSST Science Center for the Guangdong–Hong Kong–Macau Greater Bay Area Zhuhai519082 China Yunnan Observatories 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 Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing100049 China Department of Astronomy School of Physics and Astronomy China West Normal University Nanchong637002 China Dipartimento di Fisica e Astronomia "Galileo Galilei" Univ. di Padova Vicolo dell’Osservatorio 3 PadovaIT-35122 Italy Istituto Nazionale di Astrofisica Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaIT-35122 Italy

Identifying bifurcated blue straggler (BS) sequences in color-magnitude diagrams (CMDs) of star clusters has long been regarded as a powerful diagnostic for distinguishing different BS formation mechanisms. While such bifurcations are typically associated with core-collapsed clusters, their detection in dynamically young clusters raises new questions about their origins. In this study, using high-precision proper motion data derived from Hubble Space Telescope multi-epoch observations, we confirm the existence of two distinct BS sequences in the Large Magellanic Cloud cluster NGC 2173 (∼ 1.58 Gyr): a well-defined, narrow blue sequence and a sparser red sequence. The extended core region excludes collisional formation as a viable channel for BS formation. Our binary evolution models suggest that non-conservative mass transfer (MT) is essential for shaping the distribution of BS binaries in the CMD. The red sequence primarily comprises BS binaries formed through conservative ongoing MT. In contrast, the blue sequence BS binaries are formed through non-conservative post-MT processes, all involving white dwarf (WD) companions. These BS+WD binary systems may subsequently undergo a second MT phase, leading to the formation of double WD systems. © 2025, CC BY.

关键词： White dwarfs

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Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5

引用

Astrophysical Journal Letters 2023年第2期953卷 L17-L17页

作者： Takata, J. Kong, A.K.H. Wang, X.F. Song, F.F. Mao, J. Hou, X. Hu, C.-P. Lin, L.C.-C. Li, K.L. Hui, C.Y. Department of Astronomy School of Physics Huazhong University of Science and Technology Wuhan 430074 China Institute of Astronomy National Tsing Hua University Hsinchu 30013 Taiwan Yunnan Observatories Chinese Academy of Sciences Yunnan Province Kunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China University of Chinese Academy of Sciences Beijing 100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing 100012 China Department of Physics National Changhua University of Education Changhua 50007 Taiwan Department of Physics National Cheng Kung University Tainan 701401 Taiwan Department of Astronomy and Space Science Chungnam National University Daejeon 305-764 South Korea

ASASSN-V J205543.90+240033.5 (ASJ2055) is a possible post-common-envelope binary system. Its optical photometric data show an orbital variation of about 0.52 days and a fast period modulation of P ₀ ∼ 9.77 minutes, whose origin is unknown. In this Letter, we report evidence of the stellar oscillation of the companion star as the origin of the fast period modulation. We analyze the photometric data taken by the Transiting Exoplanet Survey Satellite, the Liverpool Telescope, and the Lulin One-meter Telescope. It is found that the period of the 9.77 minutes signal measured in 2022 August is significantly shorter than that in 2021 July/August, and the magnitude of the change is of the order of ∣△P ₀∣/P ₀ ∼ 0.0008(4). Such a large variation will be incompatible with the scenario of the white dwarf (WD) spin as the origin of the 9.77 minutes periodic modulation. We suggest that the fast periodic signal is related to the emission from the irradiated companion star rather than that of the WD. Using existing photometric data covering a wide wavelength range, we estimate that the hot WD in ASJ2055 has a temperature of T _eff ∼ 80,000 K and is heating the oscillating M-type main-sequence star with T _eff ∼ 3500 K on its unirradiated surface. The stellar oscillation of the M-type main-sequence star has been predicted in theoretical studies, but no observational confirmation has been done. ASJ2055, therefore, has the potential to be a unique laboratory for investigating the stellar oscillation of an M-type main-sequence star and the heating effect on stellar oscillation. © 2023. The Author(s). Published by the American Astronomical Society.

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