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A Characteristic Optical Variability Timescale in Jetted Active Galactic Nuclei: A Large Gamma-Ray Emission Sample

The Astrophysical Journal Supplement Series 2025年第1期279卷 3-3页

作者： Dingrong Xiong Mouyuan Sun Jun-Xian Wang Junhui Fan Yongquan Xue Minfeng Gu Liang Chen Yongyun Chen Nan Ding Fei Guo Jirong Mao Guowei Ren Rui Xue Dahai Yan Shenbang Yang Haiyun Zhang Jinming Bai Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming 650216 People’s Republic of China xiongdingrong@*** baijinming@*** Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing 100012 People’s Republic of China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming 650216 People’s Republic of China Department of Astronomy Xiamen University Xiamen Fujian 361005 People’s Republic of China Department of Astronomy University of Science and Technology of China Hefei 230026 People’s Republic of China School of Astronomy and Space Science University of Science and Technology of China Hefei 230026 People’s Republic of China Center for Astrophysics Guangzhou University Guangzhou 510006 People’s Republic of China Astronomy Science and Technology Research Laboratory of Department of Education of Guangdong Province Guangzhou 510006 People’s Republic of China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai 200030 People’s Republic of China College of Physics and Electronic Engineering Qujing Normal University Qujing 655011 People’s Republic of China School of Physical Science and Technology Kunming University 650214 People’s Republic of China Yunnan Normal University Kunming 650500 People’s Republic of China Department of Physics Zhejiang Normal University Jinhua 321004 People’s Republic of China Department of Astronomy Key Laboratory of Astroparticle Physics of Yunnan Province Yunnan University Kunming 650091 People’s Republic of China Faculty of Science Kunming University of Science and Technology Kunming 650500 People’s Republic of China

The variability mechanisms from jetted active galactic nuclei (AGNs) are still under debate. Here, the damped random walk (DRW) model, implemented through Gaussian processes (GPs), is used to fit the Zwicky Transient Facility long-term optical light curves of 1684 gamma-ray emission jetted AGNs. This analysis yields one of the largest samples with characteristic optical variability timescales for jetted AGNs. A single DRW model from GPs can fit the optical light curve of most jetted AGNs well/potentially well, while there are still some jetted AGNs whose light curve cannot be fitted well by a single DRW model. After the jet power, proxied by gamma-ray luminosity, is introduced as a new parameter, new relationships among intrinsic variability time scales, black hole mass, and jet power are discovered for efficient accretion AGNs ( ${\tau }_{\mathrm{in}}\propto {M}_{\mathrm{BH}}^{0.2{9}_{-0.06}^{+0.06}}{P}_{\mathrm{jet}}^{-0.{3}_{-0.03}^{+0.03}}$

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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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The optical properties of three type II supernovae: 2014cx, 2014cy and 2015cz

arXiv

引用

arXiv 2021年

作者： Dastidar, R. Misra, K. Singh, M. Pastorello, A. Sahu, D.K. Wang, X. Gangopadhyay, A. Tomasella, L. Zhang, J. Bose, S. Mo, J. Elias-Rosa, N. Tartaglia, L. Yan, S. Kumar, B. Anupama, G.C. Pandey, S.B. Rui, L. Zhang, T. Terreran, G. Ochner, P. Huang, F. Aryabhatta Research Institute of Observational Sciences Manora Peak Nainital263 001 India Department of Physics and Astrophysics University of Delhi Delhi110 007 India Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of INAF-Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 Padova35122 Italy Indian Institute of Astrophysics Koramangala Bangalore560 034 India Physics Department and Tsinghua Center for Astrophysics Tsinghua University Bejing100084 China Bejing Planetarium Bejing Academy of Sciences and Technology Bejing100044 China Pt.Ravi Shankar Shukla University Raipur492 010 India Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Department of Astronomy Ohio State University 140 W. 18th Avenue ColumbusOH43210 United States Ohio State University 191 W. Woodruff Avenue ColumbusOH43210 United States Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Department of Astronomy and Oskar Klein Centre AlbaNova University Centre Stockholm University StockholmSE-106 91 Sweden Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Bejing100012 China Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Department of Astronomy Shanghai Jiaotong University Shanghai200240 China

We present the photometric and spectroscopic analysis of three Type II SNe: 2014cx, 2014cy and 2015cz. SN 2014cx is a conventional Type IIP with a shallow slope (0.2 mag/50d) and an atypical short plateau (∼86 d). SNe 2014cy and 2015cz show relatively large decline rates (0.88 and 1.64 mag/50d, respectively) at early times before settling to the plateau phase, unlike the canonical Type IIP/L SN light curves. All of them are normal luminosity SN II with an absolute magnitude at mid-plateau of M50V,14cx=-16.6±0.4mag, M50V,14cy=-16.5±0.2mag and M50V,15cz=-17.4±0.3mag. A relatively broad range of 56Ni masses is ejected in these explosions (0.027-0.070 Mo). The spectra show the classical evolution of Type II SNe, dominated by a blue continuum with broad H lines at early phases and narrower metal lines with P Cygni profiles during the plateau. High-velocity H I features are identified in the plateau spectra of SN 2014cx at 11600 km s-1, possibly a sign of ejecta-circumstellar interaction. The spectra of SN 2014cy exhibit strong absorption profile of H I similar to normal luminosity events whereas strong metal lines akin to sub-luminous SNe. The analytical modelling of the bolometric light curve of the three events yields similar radii for the three objects within errors (478, 507 and 608 Ro for SNe 2014cx, 2014cy and 2015cz, respectively) and a range of ejecta masses (15.0, 22.2 and 18.7 Mo for SNe 2014cx, 2014cy and 2015cz), and a modest range of explosion energies (3.3-6.0 foe where 1 foe = 1051 erg). Copyright © 2021, The Authors. All rights reserved.

关键词： Luminance

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Long-term photometric behavior of the eclipsing Z Cam-type dwarf nova AY Psc

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Research in Astronomy and Astrophysics 2017年第6期17卷 67-76页

作者： Zhong-Tao Han Sheng-Bang Qian Irina Voloshina Li-Ying Zhu Yunnan Observatories Chinese Academy of Sciences Kunming 650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650216 China University of Chinese Academy of Sciences Beijing 100049 China Sternberg Astronomical Institute Moscow State University Universitetskij prospect 13 Moscow 119992 Russia

New eclipse timings of the Z Cam-type dwarf nova AY Psc were measured and the orbital ephemeris was revised. In addition, based on long-term AAVSO data, the outburst behaviors were also explored. Our analysis suggests that normal outbursts are quasi-periodic, with an amplitude of 2.5（4-0.1） mag and a period of - 18.3（4-0.7） d. The amplitude vs. recurrence-time relation ofAY Psc is discussed, and we conclude that this relation may represent general properties of dwarf nova outbursts. The observed standstill ends with an outburst, which is inconsistent with the general picture of Z Cam- type stars. This unusual behavior was considered to be related to mass-transfer outbursts. Moreover, the average luminosity Is brighter during standstills than during outburst cycles. The changes in brightness mark variations in M2 due to the fact that the disk of AY Psc is nearly steady state.M2 value was limited to the range from 6.35 × 10-9 to 1.18 × 10-8 M yr-1. More detailed examination shows that there are a few small outbursts present during standstills. These events with amplitudes of - 0.5 - 0.9 mag are very similar to the stunted outbursts reported in some nova-like cataclysmic variables. We discussed several possible mechanisms and suggested that the most reasonable mechanism for these stunted outbursts is a changing mass-transfer rate.

关键词： binaries close - stars cataclysmic variables - stars individual （AY Psc）

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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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The fast transient AT 2023clx in the nearby LINER galaxy NGC 3799 as a tidal disruption of a very low-mass star

arXiv

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arXiv 2024年

作者： Charalampopoulos, P. Kotak, R. Wevers, T. Leloudas, G. Kravtsov, T. Pursiainen, M. Ramsden, P. Reynolds, T.M. Aamer, A. Anderson, J.P. Arcavi, I. Cai, Y.-Z. Chen, T.-W. Dennefeld, M. Galbany, L. Gromadzki, M. Gutiérrez, C.P. Ihanec, N. Kangas, T. Kankare, E. Kool, E. Lawrence, A. Lundqvist, P. Makrygianni, L. Mattila, S. Müller-Bravo, T.E. Nicholl, M. Onori, F. Sahu, A. Smartt, S.J. Sollerman, J. Wang, Y. Young, D.R. Department of Physics and Astronomy University of Turku TurkuFI-20014 Finland Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States European Southern Observatory Alonso de Córdova 3107 Vitacura Santiago Chile DTU Space National Space Institute Technical University of Denmark Elektrovej 327 Kgs. LyngbyDK-2800 Denmark European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago Chile Department of Physics University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom Institute for Gravitational Wave Astronomy University of Birmingham BirminghamB15 2TT United Kingdom School of Physics and Astronomy University of Birmingham BirminghamB15 2TT United Kingdom Astrophysics Research Centre School of Mathematics and Physics Queen's University Belfast BelfastBT7 1NN United Kingdom Niels Bohr Institute University of Copenhagen 2200 Denmark Millennium Institute of Astrophysics MAS Nuncio Monsenor Sotero Sanz 100 Off. 104 Providencia Santiago Chile 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 Graduate Institute of Astronomy National Central University 300 Jhongda Road Jhongli32001 Taiwan IAP/Paris CNRS Sorbonne University France Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain BarcelonaE-08034 Spain Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 WarszawaPL-00-478 Poland Isaac Newton Group of Telescopes ING La Palma Santa Cruz de Tenerife38700 Spain University of Turku FI-20014 Finland The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova Stockholm10691 Sweden Institute for Astronomy University of Edinburgh Royal Observatory Blackford

We present an extensive analysis of the optical and ultraviolet (UV) properties of AT 2023clx, the closest optical/UV tidal disruption event (TDE) to date (z = 0.01107), which occurred in the nucleus of the interacting low-ionization nuclear emission-line region (LINER) galaxy, NGC 3799. After correcting for the host reddening (E(B − V)h = 0.179 mag), we find its peak absolute g-band magnitude to be −18.03 ± 0.07 mag, and its peak bolometric luminosity to be Lpk = (1.57 ± 0.19) × 1043 erg s−1. AT 2023clx displays several distinctive features: first, it rose to peak within 10.4 ± 2.5 days, making it the fastest rising TDE to date. Our SMBH mass estimate of MBH ≈ 106.0 Mo -estimated using several standard methods- rules out the possibility of an intermediate-mass BH as the reason for the fast rise. Dense spectral follow-up reveals a blue continuum that cools slowly and broad Balmer and He ii lines as well as weak He i λλ5876,6678 emission features that are typically seen in TDEs. The early, broad (width ∼ 15 000 km s−1) profile of Hα matches theoretical expectations from an optically thick outflow. A flat Balmer decrement (LHα/LHβ ∼ 1.58) suggests that the lines are collisionally excited rather than being produced via photoionisation, in contrast to typical active galactic nuclei. A second distinctive feature, seen for the first time in TDE spectra, is a sharp, narrow emission peak at a rest wavelength of ∼ 6353 Å. This feature is clearly visible up to 10 d post-peak;we attribute it to clumpy material preceding the bulk outflow, which manifests as a high-velocity component of Hα (−9 584 km s−1). Its third distinctive feature is the rapid cooling during the first ∼ 20 days after peak, reflected as a break in the temperature evolution. Combining these findings, we propose a scenario for AT 2023clx involving the disruption of a very low-mass star ( 0.1 Mo) with an outflow launched in our line of sight and with disruption properties that led to efficient circularisation a

关键词： Photoionization

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The enigmatic double-peaked stripped-envelope SN 2023aew

arXiv

引用

arXiv 2024年

作者： Kangas, T. Kuncarayakti, H. Nagao, T. Kotak, R. Kankare, E. Fraser, M. Stevance, H. Mattila, S. Maeda, K. Stritzinger, M. Lundqvist, P. Elias-Rosa, N. Ferrari, L. Folatelli, G. Frohmaier, C. Galbany, L. Kawabata, M. Koutsiona, E. Müller-Bravo, T.E. Piscarreta, L. Pursiainen, M. Singh, A. Taguchi, K. Teja, R.S. Valerin, G. Pastorello, A. Benetti, S. Cai, Y.-Z. Charalampopoulos, P. Gutiérrez, C.P. Kravtsov, T. Reguitti, A. University of Turku FI-20014 Finland Department of Physics and Astronomy University of Turku FI-20014 Finland Aalto University Metsähovi Radio Observatory Metsähovintie 114 Kylmälä02540 Finland Aalto University Department of Electronics and Nanoengineering PO Box 15500 Aalto00076 Finland School of Physics University College Dublin L.M.I. Main Building Beech Hill Road Dublin 4 D04 P7W1 Ireland Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom School of Sciences European University Cyprus Diogenes Street Engomi Nicosia1516 Cyprus Department of Astronomy Kyoto University Kitashirakawa-Oiwake-cho Sakyo-ku Kyoto606-8502 Japan Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus C8000 Denmark Oskar Klein Centre Department of Astronomy Stockholm University Albanova University Centre StockholmSE-106 91 Sweden INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Paseo del Bosque s/n La PlataB1900FWA Argentina CCT-CONICET-UNLP Paseo del Bosque S/N La PlataB1900FWA Argentina The University of Tokyo 5-1-5 Kashiwanoha Kashiwa Chiba277-8583 Japan School of Physics and Astronomy University of Southampton SouthamptonSO17 1BJ United Kingdom Gran Capitá 2-4 Edifici Nexus Desp. 201 BarcelonaE-08034 Spain Nishi-Harima Astronomical Observatory Center for Astronomy University of Hyogo 407-2 Nishigaichi Sayo-cho Sayo Hyogo679-5313 Japan Department of Physics University of Crete Vasilika Bouton Heraklion70013 Greece Department of Physics University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom Hiroshima Astrophysical Science Center Hiroshima University Hiroshima Higashi-Hiroshima739-8526 Japan Indian Institute of Astrophysics II Block Koramangala Karnataka

We present optical and near-infrared photometry and spectroscopy of SN 2023aew and our findings on its remarkable properties. This event, initially resembling a Type IIb supernova (SN), rebrightens dramatically ∼90 d after the first peak, at which time its spectrum transforms into that of a SN Ic. The slowly evolving spectrum specifically resembles a post-peak SN Ic with relatively low line velocities even during the second rise. The second peak, reached 119 d after the first peak, is both more luminous (Mr = −18.75 ± 0.04 mag) and much broader than those of typical SNe Ic. Blackbody fits to SN 2023aew indicate that the photosphere shrinks almost throughout its observed evolution, and the second peak is caused by an increasing temperature. Bumps in the light curve after the second peak suggest interaction with circumstellar matter (CSM) or possibly accretion. We consider several scenarios for producing the unprecedented behavior of SN 2023aew. Two separate SNe, either unrelated or from the same binary system, require either an incredible coincidence or extreme fine-tuning. A pre-SN eruption followed by a SN requires an extremely powerful, SN-like eruption (consistent with ∼1051 erg) and is also disfavored. We therefore consider only the first peak a true stellar explosion. The observed evolution is difficult to reproduce if the second peak is dominated by interaction with a distant CSM shell. A delayed internal heating mechanism is more likely, but emerging embedded interaction with a CSM disk should be accompanied by CSM lines in the spectrum, which are not observed, and is difficult to hide long enough. A magnetar central engine requires a delayed onset to explain the long time between the peaks. Delayed fallback accretion onto a black hole may present the most promising scenario, but we cannot definitively establish the power source. Copyright © 2024, The Authors. All rights reserved.

关键词： Supernovae

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Properties of Radial Velocities measurement based on LAMOST-II Medium-Resolution Spectroscopic Observations

arXiv

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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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BinCodex: a common output format for binary population synthesis

arXiv

引用

arXiv 2023年

作者： Valli, Ruggero Graziani, Luca Agrawal, Poojan Arca Sedda, Manuel Artale, M. Celeste Bobrick, Alexey Breivik, Katelyn Chakraborty, Srija Çalşskan, Mesut Chen, Xuefei Eldridge, Jan J. Escobar, Gastón J. Gossage, Seth Han, Zhanwen Iorio, Giuliano Korb, Erika Korol, Valeriya Kruckow, Matthias U. Larson, Shane L. Laurentiu, Caramete Li, Zhenwei Mandel, Ilya Menu, Jonathan Nelemans, Gijs Rodriguez-Segovia, Nicolas Ruiter, Ashley J. Tang, Petra Toonen, Silvia Sgalletta, Cecilia Strokov, Vladimir Sun, Meng Willcox, Reinhold Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Straße 1 Garching85741 Germany Dipartimento di Fisica Sapienza Università di Roma Piazzale Aldo Moro 5 Roma00185 Italy Department of Physics and Astronomy The University of North Carolina at Chapel Hill Chapel HillNC27599 United States Gran Sasso Science Institute V.le F. Crispi L'Aquila67100 Italy L'Aquila67100 Italy INAF Osservatorio Astronomico d'Abruzzo Via M. Maggini snc Teramo64100 Italy Instituto de Astrofísica Facultad de Ciencias Exactas Universidad Andres Bello Fernandez Concha 700 Santiago Chile Physics Department Technion - Israel Institute of Technology Haifa3200002 Israel Department of Physics McWilliams Center for Cosmology Carnegie Mellon University 5000 Forbes Avenue PittsburghPA15213 United States Department of Physics Scuola Normale Superiore Piazza dei Cavalieri 7 PI Pisa56126 Italy Department of Physics & Astronomy Johns Hopkins University 3400 North Charles Street BaltimoreMD21218 United States Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Science China International Centre of Supernovae Yunnan Key Laboratory Kunming650216 China Department of Physics University of Auckland Private Bag 92019 Auckland New Zealand Dipartimento di Fisica e Astronomia Università di Padova Vicolo dell'Osservatorio 3 Padova35122 Italy Northwestern University 1800 Sherman Ave EvanstonIL60201 United States Département d'Astronomie Université de Genève Chemin Pegasi 51 VersoixCH-1290 Switzerland Université de Genève GenevaCH-1211 Switzerland Center for Interdisciplinary Exploration & Research in Astrophysics Department of Physics & Astronomy Northwestern University EvanstonIL60201 United States Cosmology and Astroparticle Physics Laboratory Institute of Space Science Atomistilor Street 409 Magurele077125 Romania School of Physics and Astronomy Monash Uni

This document describes BinCodex, a common format for the output of binary population synthesis (BPS) codes agreed upon by the members of the LISA Synthetic UCB Catalogue Group. The goal of the format is to provide a common reference framework to describe the evolution of a single, isolated binary system or a population of isolated binaries. © 2023, CC BY.

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