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arXiv 2024年

作者： Liu, Qichun Lin, Jie Wang, Xiaofeng Dai, Zhibin Sun, Yongkang Xi, Gaobo Mo, Jun Liu, Jialian Yan, Shengyu Filippenko, Alexei V. Brink, Thomas G. Yang, Yi Patra, Kishore C. Cai, Yongzhi Chen, Zhihao Chen, Liyang Guo, Fangzhou Jiang, Xiaojun Li, Gaici Li, Wenxiong Lin, Weili Miao, Cheng Ma, Xiaoran Peng, Haowei Xia, Qiqi Xiang, Danfeng Zhang, Jicheng Physics Department Tsinghua Center for Astrophysics Tsinghua University Beijing100084 China 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 Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China 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 University of California BerkeleyCA94720-3411 United States International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China CAS Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100101 China Department of Astronomy Xiamen University Xiamen361005 China Department of Astronomy Beijing Normal University Beijing100875 China

The Tsinghua University–Ma Huateng Telescopes for Survey (TMTS) started to monitor the LAMOST plates in 2020, leading to the discovery of numerous short-period eclipsing binaries, peculiar pulsators, flare stars, and other variable objects. Here, we present the uninterrupted light curves for a sample of 64 cataclysmic variables (CVs) observed/discovered using the TMTS during its first three-year observations, and we introduce new CVs and new light-variation periods (from known CVs) revealed through the TMTS observations. Thanks to the high-cadence observations of TMTS, diverse light variations, including superhumps, quasi-periodic oscillations, large-amplitude orbital modulations, and rotational modulations, are able to be detected in our CV samples, providing key observational clues for understanding the fast-developing physical processes in various CVs. All of these short-timescale light-curve features help further classify the subtypes of CV systems. We highlight the light-curve features observed in our CV sample and discuss further implications of minute-cadence light curves for CV identifications and classifications. Moreover, we examine the Hα emission lines in the spectra from our nonmagnetic CV samples (i.e., dwarf novae and nova-like subclasses) and find that the distribution of Hα emission strength shows significant differences between the sources with orbital periods above and below the period gap, which agrees with the trend seen from the SDSS nonmagnetic CV sample. Copyright © 2024, The Authors. All rights reserved.

关键词： Seismology

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Velocity-Resolved Ionization Mapping of Broad Line Region. I. Insights into Diverse Geometry and Kinematics

arXiv

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arXiv 2024年

作者： Li, Sha-Sha Feng, Hai-Cheng Liu, H.T. Bai, J.M. Ji, Xiang Pang, Yu-Xuan Cheng, Cheng Lu, Kai-Xing Wang, Jian-Guo Li, Rui Yunnan Observatories Chinese Academy of Sciences Yunnan Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Yunnan Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory of Radio Astronomy and Technology Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100101 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Department of Astronomy School of Physic Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China CAS Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Physics and Microelectronics Zhengzhou University Zhengzhou450001 China

Broad emission lines of active galactic nuclei (AGNs) originate from the broad-line region (BLR), consisting of dense gas clouds in orbit around an accreting supermassive black hole. Understanding the geometry and kinematics of the region is crucial for gaining insights into the physics and evolution of AGNs. Conventional velocity-resolved reverberation mapping may face challenges in disentangling the degeneracy between intricate motion and geometry of this region. To address this challenge, new key constraints are required. Here, we report the discovery of an asymmetric BLR using a novel technique: velocity-resolved ionization mapping, which can map the distance of emitting gas clouds by measuring Hydrogen line ratios at different velocities. By analyzing spectroscopic monitoring data, we find that the Balmer decrement is anticorrelated with the continuum and correlated with the lags across broad emission line velocities. Some line ratio profiles deviate from the expectations for a symmetrically virialized BLR, suggesting that the red-shifted and blue-shifted gas clouds may not be equidistant from the supermassive black hole (SMBH). This asymmetric geometry might represent a formation imprint, provide new perspectives on the evolution of AGNs, and influence SMBH mass measurements. © 2024, CC BY.

关键词： Kinematics

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One Reliable Method for Stellar Parameter Determination Based on Space Photometry and the Phoenix Spectral Library

SSRN

引用

SSRN 2022年

作者： Liu, Yisi Gu, Shenghong Perdelwitz, Volker Liu, Jing Yunnan Observatories Chinese Academy of Sciences Yunnan Kunming650216 China National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Yunnan Kunming650216 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Hamburger Sternwarte Gojenbergsweg 112 Hamburg21029 Germany Department of Physics Ariel University Ariel40700 Israel

For a survey project, to get precise determination on parameters of stars is quite important. Although the second data release of Gaia provided stellar parameters for an unprecedented number of stars, due to the proximity of the Gaia passbands, the reliability of these parameters is still not unshakeable, especially for specific targets. In order to establish a reliable estimation of stellar parameters such as the effective temperature and so on, we are currently developing an algorithm which compares the absolute fluxes of all Gaia passbands, combined with those from the WISE mission, to PHOENIX spectra. Results have shown that a broader wavelength range enables a reliable determination of these parameters. Furthermore, the effective temperature we derived has a better precision than Gaia’s one, which shows the good performance of PHOENIX model. © 2022, The Authors. All rights reserved.

关键词： Surveys

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FAST discovery of an extremely radio-faint millisecond pulsar from the Fermi-LAT unassociated source 3FGL J0318.1+0252

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Science China(Physics,Mechanics & Astronomy) 2021年第12期64卷 10-17页

作者： Pei Wang Di Li Colin J.Clark Pablo M.Saz Parkinson Xian Hou Weiwei Zhu Lei Qian Youling Yue Zhichen Pan Zhijie Liu Xuhong Yu Shanping You Xiaoyao Xie Qijun Zhi Hui Zhang Jumei Yao Jun Yan Chengmin Zhang Kwok Lung Fan Paul S.Ray Matthew Kerr David A.Smith Peter F.Michelson Elizabeth C.Ferrara David J.Thompson Zhiqiang Shen Na Wang FAST&Fermi-LAT Collaboration CAS Key Laboratory of FAST National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China University of Chinese Academy of Sciences Beijing 100049China Jodrell Bank Centre for Astrophysics Department of Physics and AstronomyUniversity of ManchesterManchester M139PLUK Department of Physics and Laboratory for Space Research University of Hong KongHong Kong 999077China Santa Cruz Institute for Particle Physics University of CaliforniaSanta Cruz CA 95064USA Yunnan Observatories Chinese Academy of SciencesKunming 650216China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650216China School of Computer Science and Technology Key Laboratory of Information and Computing Guizhou ProvinceGuizhou Normal UniversityGuiyang 550001China School of Physics and Electronic Science Guizhou Normal UniversityGuiyang 550001China Physics Department Stanford UniversityStanford CA 94305USA UMCP/CRESST/GSFC NASAGreenbeltMaryland MD 20771USA GSFC NASAGreenbeltMaryland MD 20771USA Centre d’´Etudes Nucl´eaires de Bordeaux Gradignan IN2P3/CNRSUniversit´e BordeauxGradignan 33175France Space Science Division U.S.Naval Research LaboratoryWashington DC 20375-5352USA Shanghai Astronomical Observatory Chinese Academy of SciencesShanghai 200030China Xinjiang Astronomical Observatory Urumqi 830011China Department of Physics University of MarylandCollege Park MD 20742USA NAOC-UKZN Computational Astrophysics Centre University of KwaZulu-NatalDurban 4000South Africa 不详

High sensitivity radio searches of unassociated γ-ray sources have proven to be an effective way of finding new pulsars. Using the Five-hundred-meter Aperture Spherical radio Telescope(FAST) during its commissioning phase, we have carried out a number of targeted deep searches of Fermi Large Area Telescope(LAT) γ-ray sources. On February 27, 2018 we discovered an isolated millisecond pulsar(MSP), PSR J0318+0253, coincident with the unassociated γ-ray source 3 FGL J0318.1+0252. PSR J0318+0253 has a spin period of 5.19 ms, a dispersion measure(DM) of 26 pc cm-3 corresponding to a DM distance of about 1.3 kpc, and a period-averaged flux density of(~11±2) μJy at L-band(1.05-1.45 GHz). Among all high energy MSPs, PSR J0318+0253 is the faintest ever detected in radio bands, by a factor of at least ~4 in terms of L-band fluxes. With the aid of the radio ephemeris, an analysis of 9.6 years of Fermi-LAT data revealed that PSR J0318+0253 also displays strong γ-ray pulsations. Follow-up observations carried out by both Arecibo and FAST suggest a likely spectral turn-over around 350 MHz. This is the first result from the collaboration between FAST and the Fermi-LAT teams as well as the first confirmed new MSP discovery by FAST, raising hopes for the detection of many more MSPs. Such discoveries will make a significant contribution to our understanding of the neutron star zoo while potentially contributing to the future detection of gravitational waves, via pulsar timing array(PTA) experiments.

关键词： FAST pulsar radio gamma rays

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Unprecedented Central Engine "Breathing" Phenomenon in an Active Supermassive Black Hole

arXiv

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arXiv 2024年

作者： Zhou, Shuying Sun, Mouyuan Feng, Hai-Cheng Li, Sha-Sha Xue, Yongquan Wang, Jun-Xian Cai, Zhen-Yi Bai, Jin-Ming Li, Danyang Guo, Hengxiao Liu, H.T. Lu, Kai-Xing Mao, Jirong Marculewicz, Marcin Wang, Jian-Guo Department of Astronomy Xiamen University Fujian Xiamen361005 China SHAO-XMU Joint Center for Astrophysics Fujian Xiamen361005 China Yunnan Observatories Chinese Academy of Sciences Yunnan Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Yunnan Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China Department of Astronomy University of Science and Technology of China Anhui Hefei230026 China School of Astronomy and Space Science University of Science and Technology of China Anhui Hefei230026 China High School Affiliated to Yunnan Normal College Yunnan Kunming650506 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China

Resolving the inner structures of active galactic nuclei (AGNs) provides the "standard ruler" to measure the parallax distances of the Universe and a powerful way to weigh supermassive black holes (SMBHs). Thanks to time-domain observations, it is possible to use the reverberation mapping (RM) technique to measure time delays between different light curves that probe the structures of the SMBH accretion disks and broad line regions (BLRs), which are otherwise often too compact to be spatially resolved with current facilities for most AGNs. Despite decades of RM studies, the critical physical process that controls the structures of SMBH accretion disk and BLR and their temporal evolution remains unclear. Here we report the variation of the SMBH accretion disk structure of NGC 4151, a highly variable AGN, in response to changes in luminosity within ∼ 6 years. In the high-flux state, the time delays measured from our continuum RM with high-cadence (∼ 2 days) spectroscopy are 3.8+1.8−1.0 times larger than that in the low-flux state and 14.9 ± 2.0 times longer than the classical standard thin disk (SSD) prediction. This result provides the first piece of direct evidence that the SMBH disk structure "breathes" in highly-variable AGN manifestations. The significant time-delay change severely challenges the popular X-ray reprocessing of the classical SSD model, with or without contributions from BLRs. More importantly, the continuum time delays can be comparable with the time delay between the light curves of the broad Hβ emission line and the nearby optical continuum, and the latter is commonly used to calculate the BLR sizes. Hence, the BLR sizes are significantly underestimated if the continuum time delays are not properly considered. This underestimation introduces up to 0.3 dex systematic uncertainties on RM SMBH masses and BLR parallax distances. Our findings underscore that simultaneous continuum and BLR RM studies are vital for better deciphering the SMBH mass growt

关键词： Reverberation

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Interference location using an improved TDOA algorithm with antenna array and beamforming

Interference location using an improved TDOA algorithm with ...

引用

International Conference on Intelligent Computing, Communication and Devices, ICCD 2017

作者： Miao, Sheng Zhou, Hua Yang, Hongji Southwest Forestry University Kunming China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming China Centre for Creative Computing Bath Spa University Bath United Kingdom

ISBN: (纸本)9789811089435

Time Difference of Arrival (TDOA) is a popular interference location algorithm in the radio astronomy monitoring environment, where radio interference source may interfere with the performance of the receiver. However, with the geomagnetic white noise interference, interference detection is hard for a normal TDOA algorithm. In this paper, an improved interfere detection method is proposed. Single receiving antenna has been replaced by array antenna, and the adaptive beamforming algorithm is used in data preprocessing. A composite signal after beam-forming as an input of TDOA algorithm. The experiment shows that, comparing with the traditional TDOA algorithm and using beamforming, the location of the interference has been enhanced about 10 m for normal in the about 5 km. © Springer Nature Singapore Pte Ltd. 2019.

关键词： Beamforming

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Close binary black hole in a radio-quiet quasar: a candidate of Nano-Hertz gravitational wave emitter

Research Square

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Research Square 2021年

作者： Feng, Hai-Cheng Liu, Hong-Tao Bai, Jin-Ming Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan650011 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming Yunnan650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China

Close supermassive binary black holes (SMBBHs) with separations less than ∼ 0.1 parsec are expected to be Nano-Hertz gravitational wave sources1. SMBBH systems should exhibit periodic variability2. However, periodic variability in radio-loud quasars may be interpreted with the jet model3. Here we report the detection of a robust periodic signal in the optical variability of the radio-quiet quasar PG 0923+201 with an observed period of 726.8 ± 4.7 days, obtained from the sinusoid-like light curve of a temporal baseline of about 9 years. This periodicity is probably from a close SMBBH with a total mass of 109.3 solar masses and a separation of ∼ 0.01 parsec, implying relativistic orbital speeds. Such a system has passed through the well-known "final parsec problem" of SMBBH systems4, and the Nano-Hertz gravitational wave radiation becomes significant. The ratio of the separation between these two black holes to the broad-line region size is ∼ 0.1. A close SMBBH is also suggested by this small ratio and the spectral properties of Balmer broad lines in this quasar. This radio-quiet quasar is a candidate emitter of Nano-Hertz gravitational waves at a frequency of about 30 Nano-Hertz. © 2021, CC BY.

关键词： Gravity waves

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Minute-Cadence Observations of the LAMOST Fields with the TMTS: V. Machine Learning Classification of TMTS Catalogues of Periodic Variable Stars

arXiv

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arXiv 2024年

作者： Guo, Fangzhou Lin, Jie Wang, Xiaofeng Chen, Xiaodian Li, Tanda Chen, Liyang Xia, Qiqi Mo, Jun Xi, Gaobo Zhang, Jicheng Liu, Qichun Jiang, Xiaojun Yan, Shengyu Peng, Haowei Liu, Jialian Li, Wenxiong Lin, Weili Xiang, Danfeng Ma, Xiaoran Cai, Yongzhi Tsinghua University Haidian District Beijing100084 China 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 Beijing Planetarium Beijing Academy of Sciences and Technology Beijing100044 China CAS 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 Department of Astronomy Beijing Normal University Beijing100875 China School of Physics and Astronomy The University of Birmingham B15 2TT United Kingdom National Astronomical Observatories of China Chinese Academy of Sciences Beijing100012 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing100049 China The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China

Periodic variables are always of great scientific interest in astrophysics. Thanks to the rapid advancement of modern large-scale time-domain surveys, the number of reported variable stars has experienced substantial growth for several decades, which significantly deepened our comprehension of stellar structure and binary evolution. The Tsinghua University–Ma Huateng Telescopes for Survey (TMTS) has started to monitor the LAMOST sky areas since 2020, with a cadence of 1 minute. During the period from 2020 to 2022, this survey has resulted in densely sampled light curves for ~30,000 variables of the maximum powers in the Lomb-Scargle periodogram above the 5σ threshold. In this paper, we classified 11,638 variable stars into 6 main types using XGBoost and Random Forest classifiers with accuracies of 98.83% and 98.73%, respectively. Among them, 5301 (45.55%) variables are newly discovered, primarily consisting of δ Scuti stars, demonstrating the capability of TMTS in searching for short-period variables. We cross-matched the catalogue with Gaia’s second Data Release (DR2) and LAMOST’s seventh Data Release (DR7) to obtain important physical parameters of the variables. We identified 5504 δ Scuti stars (including 4876 typical δ Scuti stars and 628 high-amplitude δ Scuti stars), 5899 eclipsing binaries (including EA-, EB- and EW-type) and 226 candidates of RS Canum Venaticorum. Leveraging the metal abundance data provided by LAMOST and the Galactic latitude, we discovered 8 candidates of SX Phe stars within the class of "δ Scuti stars". Moreover, with the help of Gaia color-magnitude diagram, we identified 9 ZZ ceti stars. Copyright © 2024, The Authors. All rights reserved.

关键词： Stars

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A long-period pre-ELM system discovered from LAMOST medium-resolution survey

arXiv

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arXiv 2022年

作者： Zhang, Zhi-Xiang Zheng, Ling-Lin Gu, Wei-Min Sun, Mouyuan Yi, Tuan Shi, Jian-Rong Wang, Song Bai, Zhong-Rui Zhang, Hao-Tong Cui, Wen-Yuan Wang, Junfeng Wu, Jianfeng Li, Xiang-Dong Shao, Yong Lu, Kai-Xing Bai, Yu Li, Chunqian Fu, Jin-Bo Liu, Jifeng Department of Astronomy Xiamen University Fujian Xiamen361005 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing100049 China Department of Physics Hebei Normal University Shijiazhuang050024 China Department of Astronomy Nanjing University Nanjing210023 China Key laboratory of Modern Astronomy and Astrophysics Nanjing University Ministry of Education Nanjing210023 China Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China WHU-NAOC Joint Center for Astronomy Wuhan University Wuhan430072 China

We present LAMOST J041920.07+072545.4 (hereafter J0419), a close binary consisting of a bloated extremely low mass pre-white dwarf (pre-ELM WD) and a compact object with an orbital period of 0.607189 days. The large-amplitude ellipsoidal variations and the evident Balmer and He I emission lines suggest a filled Roche lobe and ongoing mass transfer. No outburst events were detected in the 15 years of monitoring of J0419, indicating a very low mass transfer rate. The temperature of the pre-ELM, Teff = 5793+124−133 K, is cooler than the known ELMs, but hotter than most CV donors. Combining the mean density within the Roche lobe and the radius constrained from our SED fitting, we obtain the mass of the pre-ELM, M1 = 0.176 ± 0.014 Mo. The joint fitting of light and radial velocity curves yields an inclination angle of i = 66.5+1.4−1.7 degrees, corresponding to the compact object mass of M2 = 1.09 ± 0.05 Mo. The very bloated pre-ELM has a smaller surface gravity (log g = 3.9 ± 0.01, R1 = 0.78 ± 0.02 Ro) than the known ELMs or pre-ELMs. The temperature and the luminosity (Lbol = 0.62+0.11−0.10. Lo) of J0419 are close to the main sequence, which makes the selection of such systems through the HR diagram inefficient. Based on the evolutionary model, the relatively long period and small log g indicate that J0419 could be close to the "bifurcation period" in the orbit evolution, which makes J0419 to be a unique source to connect ELM/pre-ELM WD systems, wide binaries and cataclysmic variables. Copyright © 2022, The Authors. All rights reserved.

关键词： Mass transfer

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MODELING Hα AND HE 10830 TRANSMISSION SPECTRUM OF WASP-52B

arXiv

引用

arXiv 2022年

作者： Yan, Dongdong Seon, Kwang-Il Guo, Jianheng Chen, Guo Li, Lifang Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 Kunming650011 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650011 China Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of Astronomy and Space Science Major University of Science and Technology 217 Gajeong-ro Yuseong-gu Daejeon34113 Korea Republic of Key Laboratory of Planetary Sciences Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China

Escaping atmosphere has been detected by the excess absorption of Lyα, Hα and He triplet (10830Å) lines. Simultaneously modeling the absorption of the Hα and He 10830 lines can provide useful constraints about the exoplanetary atmosphere. In this paper, we use a hydrodynamic model combined with a non-local thermodynamic model and a new Monte Carlo simulation model to obtain the H(2) and He(23S) populations. The Monte Carlo simulations of Lyα radiative transfer are performed with assumptions of a spherical stellar Lyα radiation and a spherical planetary atmosphere, for the first time, to calculate the Lyα mean intensity distribution inside the planetary atmosphere, necessary in estimating the H(2) population. We model the transmission spectra of the Hα and He 10830 lines simultaneously in hot Jupiter WASP-52b. We find that models with many different H/He ratios can reproduce the Hα observations well if the host star has (1) a high X-ray/extreme ultraviolet (XUV) flux (FXUV) and a relatively low X-ray fraction in XUV radiation (βm), or (2) a low FXUV and a high βm. The simulations of He 10830 Å triplet suggest that a high H/He ratio (∼ 98/2) is required to fit the observation. The models that fit both lines well confine FXUV to be about 0.5 times the fiducial value and βm to have a value around 0.3. The models also suggest that hydrogen and helium originate from the escaping atmosphere, and the mass-loss rate is about 2.8×1011 g s−1 © 2022, CC BY-NC-ND.

关键词： Radiative transfer

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