检索结果-内蒙古大学图书馆

arXiv 2019年

作者： Wang, R. Luo, A.-L. Chen, J.-J. Bai, Z.-R. Chen, L. Chen, X.-F. Dong, S.-B. Du, B. Fu, J.-N. Han, Z.-W. Hou, J.-L. Hou, Y.-H. Hou, W. Jiang, D.-K. Kong, X. Li, L.-F. Liu, C. Liu, J.-M. Qin, L. Shi, J.-R. Tian, H. Wu, H. Wu, C.-J. Xie, J.-W. Zhang, H.-T. Zhang, S. Zhao, G. Zhao, Y.-H. Zhong, J. Zong, W.-K. Zuo, F. Wu, H. Wu, C.-J. Xie, J.-W. Zhang, H.-T. Zhang, S. Zhao, G. Zhao, Y.-H. Zhong, J. Zong, W.-K. Zuo, F. Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Department of Astronomy Beijing Normal University Beijing100875 China Nanjing Institute of Astronomical Optics and Technology National Astronomical Observatories Chinese Academy of Sciences Nanjing210042 China School of Astronomy and Space Science Nanjing University Nanjing210093 China Key Laboratory of Modern Astronomy and Astrophysics in Ministry of Education Nanjing University Nanjing210093 China

The radial velocity (RV) is a basic physical quantity which can be determined through Doppler shift of the spectrum of a star. The precision of RV measurement depends on the resolution of the spectrum we used and the accuracy of wavelength calibration. In this work, radial velocities of LAMOST-II medium resolution (R ∼ 7500) spectra are measured for 1,594,956 spectra (each spectrum has two wavebands) through matching with templates. A set of RV standard stars are used to recalibrate the zero point of the measurement, and some reference sets with RVs derived from medium/high-resolution observations are used to evaluate the accuracy of the measurement. Comparing with reference sets, the accuracy of our measurement can get 0.0227 km1 s-1with respect to radial velocities standard stars. The intrinsic precision is estimated with the multiple observations of single stars, which can achieve to 1.36 km s-1,1.08 km s-1, 0.91 km s-1for the spectra at signal-to-noise levels of 10, 20, 50, respectively. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

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Probing the Final-stage Progenitor evolution for Type IIP Supernova 2017eaw in NGC 6946

arXiv

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arXiv 2019年

作者： Rui, Liming Wang, Xiaofeng Mo, Jun Xiang, Danfeng Zhang, Jujia Maund, Justyn R. Gal-Yam, Avishy Wang, Lifan Zhang, Tianmeng Physics Department and Tsinghua Center for Astrophysics Tsinghua University Beijing100084 China Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Department of Physics and Astronomy University of Sheffield Hicks Building Hounsfield Road SheffieldS3 7RH United Kingdom Department of Particle Physics and Astrophysics Weizmann Institute of Sciencem Rehovot76100 Israel Physics and Astronomy Department Texas A&M University College StationTX77843 United States Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China

We presented a detailed analysis of progenitor properties of type IIP supernova 2017eaw in NGC 6946, based on the pre-explosion images and early-time observations obtained immediately after the explosion. An unusually red star, with MF814W = −6.9 mag and mF606W− mF814W =2.9±0.2 mag, can be identified at the SN position in the pre-discovery Hubble Space Telescope(HST) images taken in 2016. The observed spectral energy distribution of this star, covering the wavelength of 0.6-2.0 µm, matches that of an M4-type red supergiant (RSG) with a temperature of about 3550 K. These results suggest that SN 2017eaw has a RSG progenitor with an initial mass of 12±2 M. The absolute F814W-band magnitude of this progenitor star is found to evolve from −7.2 mag in 2004 to −6.9 mag in 2016. Such a dimming effect is, however, unpredicted for a RSG in its neon/oxygen burning phase when its luminosity should modestly increase. The spectrum of SN 2017eaw taken a few hours after discovery clearly shows a narrow Hα emission feature blueshifted by ∼160 km s−1. This narrow component disappeared in the spectrum taken two days later, suggesting the presence of a circumstellar material (CSM) shell (i.e., at a distance of 14 cm). Combining the inferred distance with the expansion velocity of the CSM, we suggest that the progenitor of SN 2017eaw should have experienced violent mass loss at about 1-2 years prior to explosion, perhaps invoked by pulsational envelop ejection. This mechanism may help explain its luminosity decline in 2016 as well as the lack of detections of RSGs with initial mass in the range of 17 M Copyright © 2019, The Authors. All rights reserved.

关键词： Supernovae

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An Empirical Fit for Viscoelastic Simulations of Tertiary Tides

arXiv

引用

arXiv 2019年

作者： Gao, Yan Toonen, Silvia Grishin, Evgeni Comerford, Tom Kruckow, Matthias U. Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China University of Chinese Academy of Sciences Anton Pannekoek Institute for Astronomy University Of Amsterdam Amsterdam1090 GE Netherlands Institute for Gravitational Wave Astronomy School of Physics and Astronomy University of Birmingham BirminghamB15 2TT United Kingdom Physics Department Technion - Israel Institute of Technology Haifa3200003 Israel Institute of Astronomy University of Camridge Madingley Road CambridgeCB3 OHA United Kingdom

Tertiary tides (TTs), or the continuous tidal distortion of the tertiary in a hierarchical triple system, can extract energy from the inner binary, inducing within it a proclivity to merge. Despite previous work on the subject, which established that it is significant for certain close triple systems, it is still not a well-understood process. A portion of our ignorance in this regard stems from our inability to integrate a simulation of this phenomenon into conventional stellar evolution codes, since full calculations of these tidal interactions are computationally expensive on stellar evolution timescales. Thus, to attain a better understanding of how these TTs act on longer timescales, an empirical expression of its effects as a function of parameters of the triple system involved is required. In our work, we evaluate the rate at which TTs extract energy from the inner binary within a series of constructed hierarchical triple systems under varying parameters, and study the rate at which the inner binary orbital separation shrinks as a function of those parameters. We find that this rate varies little with the absolute values of the masses of the three component objects, but is very sensitive to the mass ratio of the inner binary q, the tertiary radius R3, the inner binary orbital separation a1, the outer orbital separation a2, and the viscoelastic relaxation time of the tertiary τ. More specifically, we find that the percentage by which a1 shrinks per unit time can be reasonably approximated by (1/a1)(da1/dt)=(2.22×10−8yrs−1) 4q (1 + q)−2 (R3/100R)5.2(a1/0.2AU)4.8(a2/2AU)−10.2 (τ/0.534yrs)−1.0. We also provide tests of how precise this fitting function is. Copyright © 2019, The Authors. All rights reserved.

关键词： Astrophysics

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Past and future of the central double-degenerate core of Henize 2-428

arXiv

引用

arXiv 2018年

作者： Wu, Dong-Hao Liu, Dong-Dong 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

It has been suggested that SNe Ia could be produced in the condition of the violent merger scenario of the double-degenerate model, in which a thermonuclear explosion could be produced when the merging of double carbon-oxygen white dwarfs (CO WDs) is still ongoing. It has been recently found that the nucleus of the bipolar planetary nebula Henize 2-428 consists of double CO WDs that have a total mass of ∼1.76Mo, a mass ratio of ∼1 and an orbital period of ∼4.2 hours, which is the first and only discovered progenitor candidate of SNe Ia predicted by the violent merger scenario. In this work, we aim to reproduce the evolutionary history of the central double COWDs of Henize 2-428. We find that the planetary nebula Henize 2-428 may originate from a primordial binary that have a ∼5.4Moprimary and a ∼2.7Mosecondary with an initial orbital period of ∼15.9 days. The double CO WDs are formed after the primordial binary experiencing two Roche-lobe overflows and two common-envelope ejection processes. According to our calculations, it takes about ∼840Myr for the double CO WDs to merge and form an SN Ia driven by the gravitational wave radiation after their birth. To produce the current status of Henize 2-428, a large common-envelope parameter is needed. We also estimate that the rate of SNe Ia from the violent merger scenario is at most 2.9 × 10-4yr-1, and that the delay time is in the range of ∼90Myr to the Hubble time. Copyright © 2018, The Authors. All rights reserved.

关键词： Merging

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The Pulsation Induced by Mass Transfer in Critically Rotating Stars

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Chinese Physics Letters 2016年第9期33卷 136-139页

作者：王江涛宋汉峰 College of Science Guizhou University Geneva Observatory University of Geneva Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences

The structural characteristics of the critically rotating accretor in binaries are investigated during rapid mass transfer. It is found that the accretor is subjected to periodic pulsation due to accretions and rejections of mass and angular momentum. Tile gainer attempts to attain both hydrostatic and thermal balances. This physical process can cause tile thermal structure of the accreting star to fluctuate with a period of ~ 0.19 y. Stellar wind can be enhanced by a factor of ~1.25 ×10^4 when the accretor approaches break-down velocity. Surface entropy and density decrease with the increase of the stellar radius due to the fact that rapid rotation leads to a reduction in the number density and surface temperature. The rotational energy has the same trend as stellar radius due to stellar expansion. Surface opacity which is extremely sensitive to surface temperature has an opposite trend to stellar radius. Moreover, the rate of nuclear energy must be adjusted due to mass removal or accretion at the stellar surface.

关键词： of is on it as The Pulsation Induced by Mass Transfer in Critically Rotating Stars in by

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YZ Phe: a very short period K-type contact binary with variation of the O’Connell effect and orbital period change

arXiv

引用

arXiv 2019年

作者： Sarotsakulchai, T. Qian, S.-B. Soonthornthum, B. Zhou, X. Zhang, J. Li, L.-J. Reichart, D.E. Haislip, J.B. Kouprianov, V.V. Poshyachinda, S. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China University of Chinese Academy of Sciences 19 A Yuquan Rd. Shijingshan Beijing100049 China National Astronomical Research Institute of Thailand Donkaew MaerimChiang Mai50180 Thailand Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Rd. Chaoyang District Beijing100012 China Department of Physics and Astronomy University of North Carolina CB #3255 Chapel HillNC27599 United States

YZ Phe is a very short-period contact binary (Sp.= K2 V) with an orbital period of 0.2347 days near the short period limit (0.22 d). We present the complete light curves in V RI bands, which photometric data were obtained with the 0.61-m reflector of PROMPT-8 at CTIO in Chile during June to October 2016 and August 2017. The photometric solutions were determined by using the W-D method and the results reveal that YZ Phe is a W-subtype shallow contact binary (f ∼ 10%, q = 2.635 or 1/q = 0.379 for W subtype) with rotational motion of a large hot spot on the more massive component, showing a strong O’Connell effect with variation of maxima in photometric time series at period of 4.20 yr and stellar cycle at period of 1.28 yr. By compiling all available eclipse times, the result shows a long-term period decrease at a rate of dP/dt = −2.64(±0.02) × 10−8 d yr−1, superimposed on a cyclic variation (A3 = 0.0081 days and P3 = 40.76 years). This variation cannot be explained by Applegate mechanism. Thus, the cyclic change may be interpreted as light-travel time effect via the presence of a cool third body. Based on photometric solutions, the third light was detected with 2% of total light in V and I bands. Those support the existence of a third body. For the long-term period decrease, it can be explained by mass transfer from the more massive component (M2 ∼ 0.74M☉) to the less massive one (M1 ∼ 0.28M☉) or plus AML via magnetic braking. With 1/q Copyright © 2019, The Authors. All rights reserved.

关键词： Photometry

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Observing the changing surface structures of the active K giant σ Gem with SONG

arXiv

引用

arXiv 2020年

作者： Korhonen, Heidi Roettenbacher, R.M. Gu, S. Grundahl, F. Andersen, M.F. Henry, G.W. Jessen-Hansen, J. Antoci, V. Pallé, P.L. Alonso de Córdova 3107 Vitacura Santiago Chile Yale Center for Astronomy and Astrophysics Department of Physics Yale University New HavenCT06520 United States Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan Province650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Stellar Astrophysics Centre Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Center of Excellence in Information Systems Tennessee State University NashvilleTN37209 United States DTU Space National Space Institute Technical University of Denmark Elektrovej 328 Kgs. LyngbyDK-2800 Denmark Instituto de Astrofísica de Canarias E-38205 La Laguna Tenerife Spain Universidad de La Laguna Departamento de Astrofísica La Laguna TenerifeE-38206 Spain

Aims. We aim to study the spot evolution and differential rotation in the magnetically active cool K-type giant star σ Gem from broadband photometry and continuous spectroscopic observations that span 150 nights. Methods. We use high-resolution, high signal-to-noise ratio spectra obtained with the Hertzsprung SONG telescope to reconstruct surface (photospheric) temperature maps with Doppler imaging techniques. The 303 observations span 150 nights and allow for a detailed analysis of the spot evolution and surface differential rotation. The Doppler imaging results are compared to simultaneous broadband photometry from the Tennessee State University T3 0.4 m Automated Photometric Telescope. The activity from the stellar chromosphere, which is higher in the stellar atmosphere, is also studied using SONG observations of Balmer Hα line profiles and correlated with the photospheric activity. Results. The temperature maps obtained during eight consecutive stellar rotations show mainly high-latitude or polar spots, with the main spot concentrations above latitude 45◦. The spots concentrate around phase 0.25 near the beginning of our observations and around phase 0.75 towards the end. The photometric observations confirm a small jump in spot phases that occurred in February 2016. The cross-correlation of the temperature maps reveals rather strong solar-like differential rotation, giving a relative surface differential rotation coefficient of α = 0.10 ± 0.02. There is a weak correlation between the locations of starspots and enhanced emission in the chromosphere at some epochs. Copyright © 2020, The Authors. All rights reserved.

关键词： Photometry

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Observations of the Very Young Type Ia Supernova 2019np with Early-excess Emission

arXiv

引用

arXiv 2022年

作者： Sai, Hanna Wang, Xiaofeng Elias-Rosa, Nancy Yang, Yi Zhang, Jujia Lin, Weili Mo, Jun Piro, Anthony L. Zeng, Xiangyun Andrea, Reguitti Brown, Peter Burns, Christopher R. Cai, Yongzhi Fiore, Achille Hsiao, Eric Y. Isern, Jordi Itagaki, K. Li, Wenxiong Li, Zhitong Pessi, Priscila J. Phillips, M.M. Schuldt, Stefan Shahbandeh, Melissa Stritzinger, Maximilian D. Tomasella, Lina Vogl, Christian Wang, Bo Wang, Lingzhi Wu, Chengyuan Yang, Sheng Zhang, Jicheng Zhang, Tianmeng Zhang, Xinghan Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China INAF - Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 Padova35122 Italy Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Department of Astronomy University of California BerkeleyCA94720-3411 United States 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 20A Datun Road Chaoyang District Beijing100012 China Carnegie Observatories 813 Santa Barbara Street PasadenaCA91101 United States Center for Astronomy and Space Sciences China Three Gorges University Yichang443000 China Departamento de Ciencias Físicas Universidad Andrés Bello Avda. República 252 Santiago8320000 Chile Millennium Institute of Astrophysics Nuncio Monsenor Sótero Sanz 100 Providencia Santiago8320000 Chile George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy Texas A. & M. University 4242 TAMU College StationTX77843 United States Department of Physics Florida State University 77 Chieftan Way TallahasseeFL32306 United States c/Gran Capitá 2-4 Edif. Nexus 201 Barcelona08034 Spain Itagaki Astronomical Observatory Yamagata Yamagata990-2492 Japan The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Paseo del Bosque S/N La PlataB1900FWA Argentina Carnegie Observatories Las Campanas Observatory Colina El Pino Casilla 601 Chile Max-Planck-Institut für Astrophysik Karl-Schwarzschild Str. 1 G

Early-time radiative signals from type Ia supernovae (SNe Ia) can provide important constraints on the explosion mechanism and the progenitor system. We present observations and analysis of SN 2019np, a nearby SN Ia discovered within 1-2 days after the explosion. Follow-up observations were conducted in optical, ultraviolet, and near-infrared bands, covering the phases from ∼ −16.7 days to ∼+367.8 days relative to its B−band peak luminosity. The photometric and spectral evolutions of SN 2019np resembles the average behavior of normal SNe Ia. The absolute B-band peak magnitude and the post-peak decline rate are Mmax(B) =−19.52 ± 0.47 mag and ∆m15(B) =1.04±0.04 mag, respectively. No Hydrogen line has been detected in the near-infrared and nebular-phase spectra of SN 2019np. Assuming that the 56Ni powering the light curve is centrally located, we find that the bolometric light curve of SN 2019np shows a flux excess up to 5.0% in the early phase compared to the radiative diffusion model. Such an extra radiation perhaps suggests the presence of an additional energy source beyond the radioactive decay of central nickel. Comparing the observed color evolution with that predicted by different models such as interactions of SN ejecta with circumstellar matter (CSM)/companion star, a double-detonation explosion from a sub-Chandrasekhar mass white dwarf (WD), and surface 56Ni mixing, the latter one is favored. © 2022, CC BY.

关键词： Supernovae

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Discovery of an accretion-rate independent absolute RMS amplitude of millihertz quasi-periodic oscillations in 4U 1636−53

arXiv

引用

arXiv 2019年

作者： Lyu, Ming Méndez, Mariano Altamirano, D. Zhang, Guobao Mancuso, G.C. Department of Physics Xiangtan University Xiangtan Hunan411105 China Kapteyn Astronomical Institute University of Groningen PO BOX 800 GroningenNL-9700 AV Netherlands Physics & Astronomy University of Southampton SouthamptonHampshireSO17 1BJ United Kingdom Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China C.C. No. 5 Villa Elisa1894 Argentina Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Paseo del Bosque s/n La Plata1900 Argentina

We investigate the frequency and amplitude of the millihertz quasi-periodic oscillations (mHz QPOs) in the neutron-star low-mass X-ray binary (NS LMXB) 4U 1636–53 using Rossi X-ray Timing Explorer observations. We find that no mHz QPOs appear when the source is in the hard spectral state. We also find that there is no significant correlation between the frequency and the fractional rms amplitude of the mHz QPOs. Notwithstanding, for the first time, we find that the absolute RMS amplitude of the mHz QPOs is insensitive to the parameter Sa, which measures the position of the source in the colour-colour diagram and is usually assumed to be an increasing function of mass accretion rate. This finding indicates that the transition from marginally stable burning to stable burning or unstable burning could happen very rapidly since, before the transition, the mHz QPOs do not gradually decay as the rate further changes. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

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The metamorphosis of the Type Ib SN 2019yvr: late-time interaction

arXiv

引用

arXiv 2024年

作者： Ferrari, Lucía Folatelli, Gastón Kuncarayakti, Hanindyo Stritzinger, Maximilian Maeda, Keiichi Bersten, Melina Román Aguilar, Lili M. Sáez, M. Manuela Dessart, Luc Lundqvist, Peter Mazzali, Paolo Nagao, Takashi Ashall, Chris Bose, Subhash Brennan, S.J. Cai, Y.-Z. Handberg, Rasmus Holmbo, Simon Karamehmetoglu, Emir Pastorello, Andrea Reguitti, Andrea Anderson, Joseph Chen, Ting-Wan Galbany, Lluís Gromadzki, Mariusz Gutiérrez, Claudia P. Inserra, Cosimo Kankare, Erkki Müller Bravo, Tomás E. Mattila, Seppo Nicholl, Matt Pignata, Giuliano Sollerman, Jesper Srivastav, Shubham Young, David R. Instituto de Astrofísica de La Plata CONICET Argentina Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Paseo del Bosque S La PlataN B1900FWA Argentina The University of Tokyo Chiba Kashiwa277-8583 Japan Department of Physics and Astronomy University of Turku TurkuFI-20014 Finland University of Turku FI-20014 Finland Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan RIKEN Saitama Wako351-0198 Japan Department of Physics University of California BerkeleyCA94720 United States Institut d’Astrophysique de Paris CNRS-Sorbonne Université 98 bis boulevard Arago Paris75014 France The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1 GarchingD-85748 Germany Astrophysics Research Institute Liverpool John Moores University 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Aalto University Metsähovi Radio Observatory Metsähovintie 114 Kylmälä02540 Finland Aalto University Department of Electronics and Nanoengineering P.O. BOX 15500 AaltoFI-00076 Finland Department of Physics Virginia Tech BlacksburgVA24061 United States Department of Astronomy The Ohio State University 140 W. 18th Avenue ColumbusOH43210 United States 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 INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy Merate23807 Italy European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago Chile Graduate Institute of Astronomy National Central University 300 Jhongda Road Jhongli32001

We present observational evidence of late-time interaction between the ejecta of the hydrogen-poor Type Ib supernova (SN) 2019yvr and hydrogen-rich circumstellar material (CSM), similar to the Type Ib SN 2014C. A narrow Hα emission line appears simultaneously with a break in the light-curve decline rate at around 80 − 100 d after explosion. From the interaction delay and the ejecta velocity, under the assumption that the CSM is detached from the progenitor, we estimate the CSM inner radius to be located at ∼ 6.5 − 9.1 × 1015 cm. The Hαemission line persists throughout the nebular phase at least up to +420 d post-explosion, with a full width at half maximum (FWHM) of ∼ 2000 km s−1. Assuming a steady mass loss, the estimated mass-loss rate from the luminosity of the Hα line is ∼ 3 − 7 × 10−5 M☉ yr−1. From hydrodynamical modeling and analysis of the nebular spectra, we find a progenitor He-core mass of 3 − 4 M, which would imply an initial mass of 13 − 15 M☉Our result supports the case of a relatively low mass progenitor possibly in a binary system as opposed to a higher mass single star undergoing an LBV phase. Copyright © 2024, The Authors. All rights reserved.

关键词： Supernovae

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