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arXiv 2023年

作者： Fiore, Achille Benetti, Stefano Tartaglia, Leonardo Jerkstrand, Anders Salmaso, Irene Tomasella, Lina Morales-Garoffolo, Antonia Geier, Stefan Elias-Rosa, Nancy Cappellaro, Enrico Wang, Xiaofeng Mo, Jun Chen, Zhihao Yan, Shengyu Pastorello, Andrea Mazzali, Paolo A. Ciolfi, Riccardo Cai, Yongzhi Fraser, Morgan Gutiérrez, Claudia P. Karamehmetoglu, Emir Kuncarayakti, Hanindyo Moran, Shane Ochner, Paolo Reguitti, Andrea Reynolds, Thomas M. Valerin, Giorgio Institut für Theoretische Physik Goethe Universität Max-von-Laue-Str. 1 Frankfurt am Main60438 Germany INFN-TIFPA Trento Institute for Fundamental Physics and Applications Via Sommarive 14 TrentoI-38123 Italy INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy INAF - Osservatorio Astronomico d’Abruzzo via M. Maggini snc TeramoI-64100 Italy The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden Dipartimento di Fisica e Astronomia ‘G. Galilei’ Università di Padova Vicolo dell’Osservatorio 3 PadovaI-35122 Italy Department of Applied Physics School of Engineering University of Cádiz Campus of Puerto Real CádizE-11519 Spain Instituto de Astrofisíca de Canarias Tenerife Canary Islands La Laguna38200 Spain GRANTECAN Cuesta de San José s/n La Palma Breña Baja38712 Spain Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China Astrophysics Research Institute Liverpool John Moores University LiverpoolL3 5RF United Kingdom Max-Planck Institute for Astrophysics Garching Germany INFN – Sezione di Padova Via Francesco Marzolo 8 PadovaI-35131 Italy 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 School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Ireland Gran Capità 2-4 Edifici Nexus Desp. 201 BarcelonaE-08034 Spain Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Department of Physics and Astronomy University of Turku Vesilinnantie 5 20500 Finland INAF - Osse

SN 2019neq was a very fast evolving superluminous supernova. At a redshift Z = 0.1059, its peak absolute magnitude was -21.5 ± 0.2 mag in g band. In this work, we present data and analysis from an extensive spectrophotometric follow-up campaign using multiple observational facilities. Thanks to a nebular spectrum of SN 2019neq, we investigated some of the properties of the host galaxy at the location of SN 2019neq and found that its metallicity and specific star formation rate are in a good agreement with those usually measured for SLSNe-I hosts. We then discuss the plausibility of the magnetar and the circumstellar interaction scenarios to explain the observed light curves, and interpret a nebular spectrum of SN 2019neq using published sumo radiative-transfer models. The results of our analysis suggest that the spindown radiation of a millisecond magnetar with a magnetic field B 6 × 1014 G could boost the luminosity of SN 2019neq. Copyright © 2023, The Authors. All rights reserved.

关键词： Supernovae

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Optical multi-color monitoring of OJ 287 from 2006 to 2012

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Research in Astronomy and Astrophysics 2017年第8期17卷 57-68页

作者： Qian Guo Ding-Rong Xiong Jin-Ming Bai Xu-Liang Fan Wei-Min Yi Yunnan Observatories Chinese Academy of Sciences Kunming 650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing 100012 China University of Chinese Academy of Sciences Beijing 100049 China

We present our optical multi-color monitoring of the BL Lac object OJ 287 from January 2006to December 2012 in the V,R and I bands.A relatively active state in OJ 287 has been found over all monitored epochs,among which the variations of average magnitude in V/R/I bands were measured with ?V=1.956 mag,?R=2.067 mag and ?I=2.115 mag,*** reliable intraday variability is detected,but possible variability is detected on 16 *** relative variation amplitudes fall into the range between 1% and 8%,with the majority between 2% and 4%.No time lags have been detected,but strong correlations exist among light curves in the three *** bluer-when-brighter trend is dominant over intraday timescales,which supports the shock-in-jet *** combining with additional V/R band data obtained from SMARTS and the Steward Observatory,we also find a bluer-when-brighter trend over a long-term *** possible periods of 513,176,36,30,26,17 and 14 d are found in all time-series data sets from 2006 to *** explanations about these periods are given.

关键词： BL Lacertae objects individual(OJ 287)—galaxies active—galaxies photometry

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On the diversity of strongly-interacting Type IIn supernovae

arXiv

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arXiv 2024年

作者： Salmaso, I. Cappellaro, E. Tartaglia, L. Anderson, J.P. Benetti, S. Bronikowski, M. Cai, Y.-Z. Charalampopoulos, P. Chen, T.-W. Concepcion, E. Elias-Rosa, N. Galbany, L. Gromadzki, M. Gutiérrez, C.P. Kankare, E. Lundqvist, P. Matilainen, K. Mazzali, P.A. Moran, S. Müller-Bravo, T.E. Nicholl, M. Pastorello, A. Pessi, P.J. Pessi, T. Petrushevska, T. Pignata, G. Reguitti, A. Sollerman, J. Srivastav, S. Stritzinger, M. Tomasella, L. Valerin, G. INAF-Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy INAF-Osservatorio Astronomico d’Abruzzo Via M. Maggini snc Teramo64100 Italy European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago Chile Millennium Institute of Astrophysics MAS Nuncio Monsenor Sotero Sanz 100 Off. 104 Providencia Santiago Chile Center for Astrophysics and Cosmology University of Nova Gorica Vipavska 11c Ajdovščina5270 Slovenia Yunnan Observatories Chinese Academy of Sciences Kunming650216 China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Department of Physics and Astronomy University of Turku Vesilinnantie 5 20500 Finland Graduate Institute of Astronomy National Central University 300 Jhongda Road Jhongli32001 Taiwan Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Castelldefels Barcelona08860 Spain Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warszawa00-478 Poland The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova Stockholm106 91 Sweden Nordic Optical Telescope Aarhus Universitet Rambla José Ana Fernández Pérez 7 local 5 San Antonio Breña Baja Santa Cruz TenerifeE-38711 Spain Tuorla Observatory Department of Physics and Astronomy University of Turku Vesilinnantie 5 Turku20014 Finland Astrophysics Research Institute Liverpool John Moores University ic2 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Max-Planck Institut für Astrophysik Karl-Schwarzschild-Str. 1 Garching bei München85741 Germany Astrophysics Research Centre School of Mathematics and Physics Queens University Belfast BelfastBT7 1NN United Kingdom Instituto de Estudios Astrofísicos Facultad de Ingeniería y Ciencias Universidad Diego Portales Av. Ejército Libertador 441 Santiago Chile Instituto de Alta Investigación Universidad de Ta

Context. Massive stars experience strong mass-loss rates, producing a dense, H-rich circumstellar medium (CSM). After the explosion, the collision and continued interaction of the supernova (SN) ejecta with the CSM power the light curve through the conversion of kinetic energy into radiation. When the interaction is strong, the light curve shows a broad peak and high luminosity lasting for several months. Also the spectral evolution is slower, compared to non-interacting SNe. Energetic shocks between the ejecta and the CSM create the ideal conditions for particle acceleration and production of high-energy (HE) neutrinos above 1 TeV. Aims. We study four strongly-interacting Type IIn SNe: 2021acya, 2021adxl, 2022qml, and 2022wed to highlight their peculiar characteristics, derive the kinetic energy of the explosion and the characteristics of the CSM, infer clues on the possible progenitors and their environment and relate them to the production of HE neutrinos. Methods. We analysed spectro-photometric data of a sample of interacting SNe to determine their common characteristics and derive physical properties (radii and masses) of the CSM and ejecta kinetic energies to compare them to HE neutrino production models. Results. The SNe analysed in this sample exploded in dwarf, star-forming galaxies and they are consistent with energetic explosions and strong interaction with the surrounding CSM. For SNe 2021acya and 2022wed, we find high CSM masses and mass-loss rates, linking them to very massive progenitors. For SN 2021adxl, the spectral analysis and less extreme CSM mass suggest a stripped-envelope massive star as possible progenitor. SN 2022qml is marginally consistent with being a Type Ia thermonuclear explosion embedded in a dense CSM. The mass-loss rates for all SNe are consistent with the expulsion of several solar masses of material during eruptive episodes in the last few decades before the explosion. Finally, we find that the SNe in our sample are marginally co

关键词： Kinetic energy

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The fast rise of the unusual Type IIL/IIb SN 2018ivc

arXiv

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arXiv 2024年

作者： Reguitti, Andrea Dastidar, R. Pignata, G. Maeda, K. Moriya, T.J. Kuncarayakti, H. Rodríguez, Ó. Bersten, M. Anderson, J.P. Charalampopoulos, P. Fraser, M. Gromadzki, M. Young, D.R. Benetti, S. Cai, Y.-Z. Elias-Rosa, N. Lundqvist, P. Carini, R. Cosentino, S.P. Galbany, L. Gonzalez-Bañuelos, M. Gutiérrez, C.P. Kopsacheili, M. Pineda, J.A.G. Ramirez, M. MerateI-23807 Italy INAF – Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy Instituto de Astrofìsica Universidad Andres Bello Fernandez Concha 700 Las Condes RM Santiago8320000 Chile Nuncio Monseñor Sótero Sanz 100 Providencia RM Santiago8320000 Chile Instituto de Alta Investigación Universidad de Tarapacá Casilla 7D Arica Chile Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan National Astronomical Observatory of Japan National Institutes of Natural Sciences Graduate Institute for Advanced Studies SOKENDAI 2-21-1 Osawa Mitaka Tokyo181-8588 Japan School of Physics and Astronomy Monash University ClaytonVIC3800 Australia Department of Physics and Astronomy University of Turku TurkuFI-20014 Finland University of Turku FI-20014 Finland CCT-CONICET-UNLP. Paseo del Bosque S/N La PlataB1900FWA Argentina Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Paseo del Bosque S/N La PlataB1900FWA Argentina The University of Tokyo 5-1-5 Kashiwanoha Kashiwa Chiba277-8583 Japan European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago8320000 Chile School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Ireland Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warszawa00-478 Poland Astrophysics Research Centre School of Mathematics and Physics Queen’s University Belfast BelfastBT7 1NN United Kingdom 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 Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden I-00078 Italy Università d

We present an analysis of the photometric and spectroscopic dataset of the Type II supernova (SN) 2018ivc in the nearby (10 Mpc) galaxy Messier 77. Thanks to the high cadence of the CHASE survey, we observed the SN rising very rapidly by nearly three magnitudes in five hours (or 18 mag d−1). The r-band light curve presents four distinct phases: the maximum light is reached in just one day, then a first, rapid linear decline precedes a short-duration plateau. Finally, a long, slower linear decline lasted for one year. Following a radio rebrightening, we detected SN 2018ivc four years after the explosion. The early spectra show a blue, nearly featureless continuum, but the spectra evolve rapidly: after about 10 days a prominent Hα line starts to emerge, with a peculiar profile, but the spectra are heavily contaminated by emission lines from the host galaxy. He I lines, namely λλ5876,7065, are also strong. On top of the former, a strong absorption from the Na i doublet is visible, indicative of a non-negligible internal reddening. From its equivalent width, we derive a lower limit on the host reddening of AV 1.5 mag, while from the Balmer decrement and a match of the B − V colour curve of SN 2018ivc to that of the comparison objects, a host reddening of AV 3.0 mag is obtained. The spectra are similar to those of SNe II, but with strong He lines. Given the peculiar light curve and spectral features, we suggest SN 2018ivc could be a transitional object between the Type IIL and Type IIb SNe classes. In addition, we found signs of interaction with circumstellar medium in the light curve, making SN 2018ivc also an interacting event. Finally, we modelled the early multi-band light curves and photospheric velocity of SN 2018ivc to estimate the explosion and CSM physical parameters. Copyright © 2024, The Authors. All rights reserved.

关键词： Supernovae

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

arXiv

引用

arXiv 2021年

作者： Wang, Pei Li, Di Clark, Colin J. Saz Parkinson, Pablo M. Hou, Xian Zhu, Weiwei Qian, Lei Yue, Youling Pan, Zhichen Liu, Zhijie Yu, Xuhong You, Shanping Xie, Xiaoyao Zhi, Qijun Zhang, Hui Yao, Jumei Yan, Jun Zhang, Chengmin Fan, Kwok Lung Ray, Paul S. Kerr, Matthew Smith, David A. Michelson, Peter F. Ferrara, Elizabeth C. Thompson, David J. Shen, Zhiqiang Wang, Na CAS Key Laboratory of FAST National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China University of Chinese Academy of Sciences Beijing100049 China Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy University of Manchester ManchesterM13 9PL United Kingdom Department of Physics Laboratory for Space Research University of Hong Kong Hong Kong999077 Hong Kong Santa Cruz Institute for Particle Physics University of California Santa CruzCA95064 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 School of Computer Science and Technology Key Laboratory of Information and Computing Guizhou Province Guizhou Normal University Guiyang550001 China School of Physics and Electronic Science Guizhou Normal University Guiyang550001 China Phys. Dept. Stanford University StanfordCA94305 United States UMCP CRESST GSFC NASA GreenbeltMD20771 United States GSFC NASA GreenbeltMD20771 United States Centre d’Études Nucléaires de Bordeaux Gradignan IN2P3 CNRS Université Bordeaux Gradignan33175 France Space Science Division U.S. Naval Research Laboratory WashingtonDC20375-5352 United States Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Xinjiang Astronomical Observatory 150 Science-1 Street Xinjiang Urumqi830011 China Department of Physics University of Maryland College ParkMD20742 United States NAOC-UKZN Computational Astrophysics Centre University of KwaZulu-Natal Durban4000 South Africa

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 Feb. 27th, 2018 we discovered an isolated millisecond pulsar (MSP), PSR J0318+0253, coincident with the unassociated γ-ray source 3FGL J0318.1+0252. PSR J0318+0253 has a spin period of 5.19 milliseconds, 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. Copyright © 2021, The Authors. All rights reserved.

关键词： Gamma rays

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The surviving companions in type Ia supernova remnants

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Research in Astronomy and Astrophysics 2017年第8期17卷 69-80页

作者： li-qing chen xiang-cun meng zhan-wen han yunnan observatories chinese academy of scienceskunming 650216china key laboratory for the structure and evolution of celestial objects chinese academy of scienceskunming 650216china university of chinese academy of sciences beijing 100049china center for astronomical mega-science chinese academy of sciencesbeijing 100012china

The single-degenerate(SD)model is one of the most popular progenitor models of type Ia supernovae(SNe Ia),in which the companion star can survive after an SN Ia explosion and show peculiar ***,searching for the surviving companion in type Ia supernova remnants(SNRs)is a potential method to verify the SD *** the SN 1604 remnant(Kepler’s SNR),although Chandra X-ray observation suggests that the progenitor is most likely a WD+AGB system,the surviving companion has not been *** possible reason is rapid rotation of the white dwarf(WD),causing explosion of the WD to be delayed for a spin-down timescale,and then the companion evolved into a WD before the supernova explosion,so the companion is too dim to be *** aim to verify this possible explanation by carrying out binary evolution *** this paper,we use Eggleton’s stellar evolution code to calculate the evolution of binaries consisting of a WD+red giant(RG).We assume that the rapidly rotating WD can continuously increase its mass when its mass exceeds the Chandrasekhar mass limit(MCh=1.378 M_⊙)until the mass-transfer rate decreases to be lower than a critical ***,we obtain the final masses of a WD in the range 1.378 M_⊙ to 2.707 M_⊙.We also show that if the spin-down time is less than 10~6yr,the companion star will be very bright and easily observed;but if the spin-down time is as long as^10~7 yr,the luminosities of the surviving companion would be lower than the detection *** simulation provides guidance in hunting for the surviving companion stars in SNRs,and the fact that no surviving companion has been found in Kepler’s SNR may not be definite evidence disfavoring the SD origin of Kepler’s SN.

关键词： stars evolution—binaries symbiotic—supernovae individual(SN 1604,SN 1006)

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Nucleosynthesis in Advection-Dominated Accretion Flow onto a Black Hole

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Chinese Physics Letters 2017年第4期34卷 128-131页

作者： Jiang Zhang Ren-Yi Ma Hong-Jie Li Bo Zhang Department of Mathematics and Science Hebei GEO University Shijiazhuang 050016 Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 Department of Astronomy Xiamen University Xiamen 361005 School of Sciences Hebei University of Science and Technology Shijiazhuang 050016 Department of Physics Hebei Normal University Shijiazhuang 050016

Nucleosynthesis in advection-dominated accretion flow （ADAF） onto a black hole is proposed to be an important role in chemical evolution around compact stars. We investigate the nucleosynthesis in ADAF relevant for a black hole of low mass, different from that of the self-similar solution. In particular, the presence of supersolar metal mass fractions of some isotopes seems to be associated with the known black hole nucleosynthesis in ADAF, which offers further evidence of diversity of the chemical enrichment.

关键词： Nucleosynthesis in Advection-Dominated Accretion Flow onto a Black Hole

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Energy release from magnetospheres deformed by gravitational waves

arXiv

引用

arXiv 2018年

作者： Wang, Jiancheng Li, Huiquan 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

In this work, we consider the possibility of energy release in pulsar magnetospheres deformed by gravitational waves from nearby sources. The strong electromagnetic fields in the magnetospheres may release non-negligible energy despite the weakness of the gravitational wave. When the background spacetime is perturbed due to the passage of a gravitational wave, the original force-free state of the inner magnetosphere will be slightly violated. The plasma-filled magnetosphere tends to evolve into new force-free states as the spacetime varies with time. During this process, a small portion of the electromagnetic energy stored in the magnetosphere will be released to the acceleration of charged particles along the magnetic field lines. When the pulsar is close enough to the gravitational wave source (e.g., ∼ 10−2 pc to the gravitational wave sources observed recently), the resulting energy loss rate is comparable with the radio luminosity of the pulsar. It is also noticed that, under very stringent conditions (for magnetars with much shorter distance to the sources), the released energy can reach the typical energy observed from fast radio bursts (FRBs). Copyright © 2018, The Authors. All rights reserved.

关键词： Gravitational effects

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Matter ejections behind the highs and lows of the transitional millisecond pulsar PSR J1023+0038

arXiv

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arXiv 2023年

作者： Baglio, M.C. Zelati, F. Coti Campana, S. Busquet, G. D’Avanzo, P. Giarratana, S. Giroletti, M. Ambrosino, F. Crespi, S. Zanon, A. Miraval Hou, X. Li, D. Li, J. Wang, P. Russell, D.M. Torres, D.F. Alabarta, K. Casella, P. Covino, S. Bramich, D.M. de Martino, D. Méndez, M. Motta, S.E. Papitto, A. Saikia, P. Vincentelli, F. Center for Astro Particle and Planetary Physics New York University Abu Dhabi P.O. Box 129188 Abu Dhabi United Arab Emirates INAF Osservatorio Astronomico di Brera Via Bianchi 46 LC MerateI-23807 Italy Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain Carrer Gran Capità 2–4 BarcelonaE-08034 Spain c/ Martí Franquès 1 BarcelonaE-08028 Spain c/ Martí Franquès 1 BarcelonaE-08028 Spain INAF Istituto di Radioastronomia via Gobetti 101 BolognaI-40129 Italy Department of Physics and Astronomy University of Bologna via Gobetti 93/2 BolognaI-40129 Italy INAF Osservatorio Astronomico di Roma Via Frascati 33 RM Monteporzio CatoneI-00078 Italy INAF–Istituto di Astrofisica e Planetologia Spaziali Via Fosso del Cavaliere 100 RomeI-00133 Italy Sapienza Università di Roma Piazzale Aldo Moro 5 RomeI-00185 Italy ASI - Agenzia Spaziale Italiana Via del Politecnico snc RomeI-00133 Italy 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 20A Datun Road Chaoyang District Beijing100101 China University of Chinese Academy of Sciences Beijing100049 China Research Center for Intelligent Computing Platforms Zhejiang Laboratory Hangzhou311100 China CAS Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei China School of Astronomy and Space Science University of Science and Technology of China Hefei China Institute for Frontiers in Astronomy and Astrophysics Beijing Normal University Beijing102206 China Passeig Lluís Companys 23 BarcelonaE-08010 Spain Division of Engineering New York University Abu Dhabi P.O. Box 129188 Saadiyat Island Abu Dhabi United Arab Emirates INAF−-Osservatorio Astronomico di Capodimonte Salita Moiariello 16 NapoliI-80131 Italy Kaptey

Transitional millisecond pulsars are an emerging class of sources that link low-mass X-ray binaries to millisecond radio pulsars in binary systems. These pulsars alternate between a radio pulsar state and an active low-luminosity X-ray disc state. During the active state, these sources exhibit two distinct emission modes (high and low) that alternate unpredictably, abruptly, and incessantly. X-ray to optical pulsations are observed only during the high mode. The root cause of this puzzling behaviour remains elusive. This paper presents the results of the most extensive multi-wavelength campaign ever conducted on the transitional pulsar prototype, PSR J1023+0038, covering from the radio to X-rays. The campaign was carried out over two nights in June 2021 and involved 12 different telescopes and instruments, including XMM-Newton, HST, VLT/FORS2 (in polarimetric mode), ALMA, VLA, and FAST. By modelling the broadband spectral energy distributions in both emission modes, we show that the mode switches are caused by changes in the innermost region of the accretion disc. These changes trigger the emission of discrete mass ejections, which occur on top of a compact jet, as testified by the detection of at least one short-duration millimetre flare with ALMA at the high-to-low mode switch. The pulsar is subsequently re-enshrouded, completing our picture of the mode switches. © 2023, CC BY.

关键词： Pulsars

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Mass-accreting white dwarfs and type Ia supernovae

arXiv

引用

arXiv 2018年

作者： Wang, Bo Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories 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

Type Ia supernovae (SNe Ia) play a prominent role in understanding the evolution of 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 double-degenerate model (including the violent merger scenario) and the sub-Chandrasekhar mass model. Recent 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 of SNe Ia, the possible surviving companion stars of SNe Ia, and 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. Copyright © 2018, The Authors. All rights reserved.

关键词： White dwarfs

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