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The Intermediate-Mass Black Hole Reverberation Mapping Project: First Detection of Mid-Infrared Lags in Prototypical IMBHs in NGC 4395 and POX 52

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arXiv 2025年

作者： Sun, Jingbo Guo, Hengxiao Zuo, Wenwen Lira, Paulina Gu, Minfeng Edwards, Philip G. Wang, Shu Stevens, Jamie An, Tao Barua, Samuzal Cai, Zhen-Yi Feng, Haicheng Gupta, Alok C. Ho, Luis C. Ilić, Dragana Kovačević, Andjelka B. Li, ShaSha Mezcua, Mar Popović, Luka Č. Sánchez-Sáez, Paula Sun, Mouyuan Shen, Rongfeng Vivian, U. Vince, Oliver Wang, Junxian Wu, Xuebing Yu, Zhefu Zheng, Zhenya Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China University of Chinese Academy of Sciences 19A Yuquan Road Beijing100049 China Departamento de Astronom ìa Universidad de Chile Casilla 36D Santiago Chile CSIRO Astronomy and Space Science PO Box 76 EppingNSW1710 Australia Department of Physics & Astronomy Seoul National University Seoul08826 Korea Republic of 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 Hefei230026 China Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District 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 Manora Peak Nainital263001 India Department of Astronomy School of Physics Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China University of Belgrade Faculty of Mathematics Department of Astronomy Studentski trg 16 Belgrade Serbia Hamburger Sternwarte Universitat Hamburg Gojenbergsweg 112 HamburgD-21029 Germany Campus UAB Carrer de Magrans Barcelona08193 Spain Edifici RDIT Campus UPC Castelldefels Barcelona08860 Spain Astronomical Observatory Volgina 7 Belgrade11060 Serbia European Southern Observatory Karl-Schwarzschild-Str. 2 Garching85748 Germany Department of Astronomy Xiamen University Fujian Xiamen361005 China School of Physics and Astronomy Sun Yat-Sen University Zhuhai519082 China CSST Science Center for the Guangdong-Hongkong-Macau Greater Bay Area Sun Yat-Sen University Zhuhai519082 China IPAC Caltech 1200 E. California Blvd. PasadenaCA91125 United States Department of Physics and Astr

The search for robust evidence of intermediate-mass black holes (IMBHs) is crucial for understanding black hole seeding process and the formation of supermassive black holes in the early Universe. NGC 4395 and POX 52 are two prototypical IMBH hosts, both exhibiting multi-line evidence of low-mass black hole activity. Here, we report the first detection of mid-infrared (MIR) lags in response to optical variability, with measurements of 3.0+2−149 days for NGC 4395 and 35.2+14−1127 days for POX 52 at 3.4 µm, respectively, using archival optical data and observations from the Wide-field Infrared Survey Explorer (WISE). This detection provides the first reverberation evidence of low-mass black hole activity in POX 52. The time lags of these two low-mass, low-luminosity active galactic nuclei (AGNs) generally follow the extent of the Rdust − L5100 relation found in higher-mass AGNs. Based on an empirical relation between the broad-line region and dusty torus size, we constrain the black hole mass of POX 52 to log(MBH/M☉) = 5.5 ± 0.37 (systemic and statistical errors), confirming its IMBH nature. Furthermore, long-term optical continuum monitoring of POX 52 reveals a mild inter-band lag of 1 day. However, no significant intranight variability was detected during its one-night, high-cadence monitoring, which we attribute to the longer duty cycle of fast variability in POX 52 compared to that in NGC 4395. © 2025, CC BY.

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GOTO065054+593624: a peculiar dwarf nova identified in real time via Kilonova Seekers

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arXiv 2025年

作者： Killestein, T.L. Ramsay, G. Kennedy, M. Kelsey, L. Steeghs, D. Littlefair, S. Godson, B. Lyman, J. Pursiainen, M. Warwick, B. Krawczyk, C. Nuttall, L.K. Wickens, E. Alexandrov, S.D. da Silva, C.M. Leadbeater, R. Ackley, K. Dyer, M.J. Jiménez-Ibarra, F. Ulaczyk, K. Galloway, D.K. Dhillon, V.S. O’Brien, P. Noysena, K. Kotak, R. Breton, R.P. Pallé, E. Pollacco, D. Kumar, A. O’Neill, D. Butterley, T. Wilson, R. Mattila, S. Sahu, A. Starling, R. Wang, C.Y. Liu, Q. Li, A. Dai, Z. Feng, H. Yuan, W. Billington, R. Bull, A.G. Gaudenzi, S. Gonano, V. Krawczyk, H. Mazzucato, M.T. Pasqua, A. da Silva Campos, J.A. Torres-Guerrero, M. Antonov, N.N. Bean, S.J. Boeneker, E.T. Brincat, S.M. Darlington, G.S. Dubois, F. Hambsch, F.-J. Messier, D. Oksanen, A. Poyner, G. Romanov, F.D. Sharp, I.D. Tordai, T. Vanmunster, T. Wenzel, K. Department of Physics & Astronomy University of Turku Vesilinnantie 5 TurkuFI-20014 Finland Armagh Observatory & Planetarium College Hill ArmaghBT61 9DG United Kingdom School of Physics University College Cork Kane Building Cork Ireland Institute of Astronomy Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Department of Physics University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom Astrophysics Research Cluster School of Mathematical and Physical Sciences University of Sheffield SheffieldS3 7RH United Kingdom Institute of Cosmology and Gravitation University of Portsmouth PortsmouthPO1 3FX United Kingdom Kilonova Seekers c/o Zooniverse Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Institute of Plant Physiology and Genetics Bulgarian Academy of Sciences Acad. G. Bontchev Str. Bl.23 Sofia1113 Bulgaria American Association of Variable Star Observers 185 Alewife Brook Parkway Suite 410 CambridgeMA02138 United States Variable Stars South Royal Astronomical Society of New Zealand P O Box 3181 Wellington New Zealand British Astronomical Association Variable Star Section Burlington House Piccadilly LondonW1J 0DU United Kingdom School of Physics & Astronomy Monash University ClaytonVIC3800 Australia Instituto de Astrofísica de Canarias Tenerife La LagunaE-38205 Spain School of Physics & Astronomy University of Leicester University Road LeicesterLE1 7RH United Kingdom National Astronomical Research Institute of Thailand 260 Moo 4 T. Donkaew A. Maerim Chiangmai50180 Thailand Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy The University of Manchester ManchesterM13 9PL United Kingdom Department of Physics Royal Holloway - University of London Egham Hill EghamTW20 0EX United Kingdom Centre for Advanced Instrumentation University of Durham DurhamDH1 3LE United Kingdom School of Sci

Dwarf novae are a crucial astrophysical laboratory for probing the nature of accretion, binary mass transfer, and binary evolution – yet their diverse observational characteristics continue to challenge our theoretical understanding. We here present the discovery of, and subsequent observing campaign on GOTO065054+593624 (hereafter GOTO0650), a dwarf nova of the WZ Sge type, discovered in real-time by citizen scientists via the Kilonova Seekers citizen science project. An extensive dataset charts the photometric and spectroscopic evolution of this object, covering the first two months of its 2024 superoutburst. GOTO0650 shows a complete absence of visible emission lines during the high state, strong H and barely-detected He II emission, and high-amplitude echo outbursts with a rapidly decreasing timescale that together do not neatly fit in with our current view of cataclysmic variables. The comprehensive dataset presented here not only underscores the uniqueness of this dwarf nova and marks it as a candidate period bouncer, but also highlights the important contribution that citizen scientists can make to the study of Galactic transients. Copyright © 2025, The Authors. All rights reserved.

关键词： Stars

Numerical Modelling of Tertiary Tides

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arXiv 2018年

作者： Gao, Yan Correia, Alexandre C.M. Eggleton, Peter P. Han, Zhanwen Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Department of Physics University of Coimbra Coimbra3004-516 Portugal CIDMA Department of Physics University of Aveiro Aveiro3810-193 Portugal ASD Imcce Psl University Paris Observatory 77 Av. Denfert-Rochereau Paris75014 France Lawrence Livermore National Laboratory 7000 East Ave LivermoreCA94551 United States

Stellar systems consisting of multiple stars tend to undergo tidal interactions when the separations between the stars are short. While tidal phenomena have been exten-sively studied, a certain tidal effect exclusive to hierarchical triples (triples in which one component star has a much wider orbit than the others) has hardly received any attention, mainly due to its complexity and consequent resistance to being modelled. This tidal effect is the tidal perturbation of the tertiary by the inner binary, which in turn depletes orbital energy from the inner binary, causing the inner binary separa-tion to shrink. In this paper, we develop a fully numerical simulation of these "tertiary tides"by modifying established tidal models. We also provide general insight as to how close a hierarchical triple needs to be in order for such an effect to take place, and demonstrate that our simulations can effectively retrieve the orbital evolution for such systems. We conclude that tertiary tides are a significant factor in the evolution of close hierarchical triples, and strongly influence at least ∼ 1% of all multiple star systems. Copyright © 2018, The Authors. All rights reserved.

关键词： Astrophysics

Testing relativistic boost as the cause of gamma-ray quasi-periodic oscillation in a blazar

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arXiv 2018年

作者： Yan, Dahai Zhou, Jianeng Zhang, Pengfei Zhu, Qianqian Wang, Jiancheng Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatory Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China Key Laboratory of Dark Matter and Space Astronomy Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008 China Key Laboratory of Astroparticle Physics of Yunnan Province Yunnan University Kunming650091 China Department of General Studies Nanchang Institute of Science & Technology Nanchang330108 China

The mechanism for producing gamma-ray quasi-periodic oscillation (QPO) in blazar is unknown. One possibility is the geometric model, in which without the need for intrinsic quasi-periodic variation, the relativistic Doppler factor changes periodically, resulting in observed gamma-ray QPO. We propose a method to test this geometric model. We analyze the Fermi-LAT data of PG 1553+113 spanning from 2008 August until 2018 February. According to 29 four-month average spectral energy distributions (SEDs) in the energy range of 0.1-300 GeV, we split the Fermi-LAT energy range into three bands: 0.1-1 GeV, 1-10 GeV, and 10-300 GeV. The spectrum in each energy range can be successfully fitted by a power-law. The light curves and photon indices in the three energy ranges are obtained. Then, light curves in three narrow energy ranges, i.e., 0.2-0.5 GeV, 2-5 GeV and 20- 40 GeV, are constructed, and the relative variability amplitudes in the three narrow energy ranges are calculated. A discrete- correlation analysis is performed for the light curves. Our results indicate that (i) the light curves in the different energy ranges follow the same pattern showed in the light curve above 0.1 GeV;(ii) the three groups of photon indices in the energy ranges of 0.1-1 GeV, 1-10 GeV, and 10-300 GeV keep nearly constant;(iii) the ratio between relative variability amplitudes in different narrow energy ranges are equal (within their errors) to the prediction by the Doppler e ect. Our results support the scenario of the relativistic boost producing the gamma-ray QPO for PG 1553+113. Copyright © 2018, The Authors. All rights reserved.

关键词： Germanium alloys

SN 2020wnt: A slow-evolving carbon-rich superluminous supernova with no O ii lines and a bumpy light curve

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arXiv 2022年

作者： Gutiérrez, C.P. Pastorello, A. Bersten, M. Benetti, S. Orellana, M. Fiore, A. Karamehmetoglu, E. Kravtsov, T. Reguitti, A. Reynolds, T.M. Valerin, G. Mazzali, P. Sullivan, M. Cai, Y.-Z. Elias-Rosa, N. Fraser, M. Hsiao, E.Y. Kankare, E. Kotak, R. Kuncarayakti, H. Li, Z. Mattila, S. Mo, J. Moran, S. Ochner, P. Shahbandeh, M. Tomasella, L. Wang, X. Yan, S. Zhang, J. Zhang, T. Stritzinger, M.D. University of Turku FI-20014 Finland Tuorla Observatory Department of Physics and Astronomy University of Turku FI-20014 Finland INAF Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 PadovaI-35122 Italy 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 Chiba Kashiwa277-8583 Japan Universidad Nacional de Río Negro. Sede Andina Mitre 630 Bariloche8400 Argentina Argentina Fondazione Bruno Kessler Trento Italy INFN TIFPA Trento Institute for Fundamental Physics and Applications Via Sommarive 14 TrentoI-38123 Italy Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark Departamento de Ciencias Físicas Universidad Andrés Bello Avda. República 252 Santiago Chile Millennium Institute of Astrophysics Nuncio Monsenor Sótero Sanz 100 Providencia Santiago Chile Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen N2200 Denmark Department of Physics and Astronomy G. Galilei University of Padova Vicolo dell'Osservatorio 3 Padova35122 Italy Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Max-Planck-Institut für Astrophysik Karl-Schwarzschild Str. 1 GarchingD-85748 Germany School of Physics and Astronomy University of Southampton SouthamptonSO17 1BJ United Kingdom Tsinghua University Beijing100084 China Institute of Space Sciences ICE CSIC Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain School of Physics O'Brien Centre for Science North University College Dublin Dublin Ireland Department of Physics Florida State University 77 Chieftan Way TallahasseeFL32306 United States Turku Collegium for Science Medicine and Technology University of Turku TurkuFI-20014

We present the analysis of SN 2020wnt, an unusual hydrogen-poor super-luminous supernova (SLSN-I), at a redshift of 0.032. The light curves of SN 2020wnt are characterised by an early bump lasting ∼ 5 days, followed by a bright main peak. The SN reaches a peak absolute magnitude of Mmaxr = −20.52 ± 0.03 mag at ∼ 77.5 days from explosion. This magnitude is at the lower end of the luminosity distribution of SLSNe-I, but the rise-time is one of the longest reported to date. Unlike other SLSNe-I, the spectra of SN 2020wnt do not show O ii, but strong lines of C ii and Si ii are detected. Spectroscopically, SN 2020wnt resembles the Type Ic SN 2007gr, but its evolution is significantly slower. Comparing the bolometric light curve to hydrodynamical models, we find that SN 2020wnt luminosity can be explained by radioactive powering. The progenitor of SN 2020wnt is likely a massive and extended star with a pre-SN mass of 80 Mo and a pre-SN radius of 15 Ro that experiences a very energetic explosion of 45 × 1051 erg, producing 4 Mo of 56Ni. In this framework, the first peak results from a post-shock cooling phase for an extended progenitor, and the luminous main peak is due to a large nickel production. These characteristics are compatible with the pair-instability SN scenario. We note, however, that a significant contribution of interaction with circumstellar material cannot be ruled out. Copyright © 2022, The Authors. All rights reserved.

关键词： Supernovae

A lower occurrence rate of bright X-ray flares in SN-GRBs than z < 1 GRBs: Evidence of energy partitions?

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arXiv 2018年

作者： Mu, Hui-Jun Gu, Wei-Min Mao, Jirong Liu, Tong Hou, Shu-Jin Lin, Da-Bin Wang, Junfeng Fang, Taotao Liang, En-Wei Department of Astronomy Xiamen University Xiamen Fujian361005 China Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan Province650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China College of Physics and Electronic Engineering Nanyang Normal University Nanyang Henan473061 China Guangxi Key Laboratory for Relativistic Astrophysics Department of Physics Guangxi University Nanning530004 China

关键词： Supernovae

Final Moments II: Observational Properties and Physical Modeling of CSM-Interacting Type II Supernovae

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arXiv 2024年

作者： Jacobson-Galán, W.V. Dessart, L. Davis, K.W. Kilpatrick, C.D. Margutti, R. Foley, R.J. Chornock, R. Terreran, G. Hiramatsu, D. Newsome, M. Padilla Gonzalez, E. Pellegrino, C. Howell, D.A. Filippenko, A.V. Anderson, J.P. Angus, C.R. Auchettl, K. Bostroem, K.A. Brink, T.G. Cartier, R. Coulter, D.A. de Boer, T. Drout, M.R. Earl, N. Ertini, K. Farah, J.R. Farias, D. Gall, C. Gao, H. Gerlach, M.A. Guo, F. Haynie, A. Hosseinzadeh, G. Ibik, A.L. Jha, S.W. Jones, D.O. Langeroodi, D. LeBaron, N. Magnier, E.A. Piro, A.L. Raimundo, S.I. Rest, A. Rest, S. Michael Rich, R. Rojas-Bravo, C. Sears, H. Taggart, K. Villar, V.A. Wainscoat, R.J. Wang, X.-F. Wasserman, A.R. Yan, S. Yang, Y. Zhang, J. Zheng, W. Department of Astronomy University of California BerkeleyCA94720-3411 United States Institut d'Astrophysique de Paris CNRS-Sorbonne Université 98 bis boulevard Arago ParisF-75014 France Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Northwestern University EvanstonIL60202 United States Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Department of Physics University of California BerkeleyCA94720-7300 United States Las Cumbres Observatory 6740 Cortona Dr. Suite 102 GoletaCA93117 United States Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138-1516 United States The NSF AI Institute for Artificial Intelligence and Fundamental Interactions United States Department of Physics University of California Santa Barbara Santa BarbaraCA93111 United States Department of Astronomy University of Virginia CharlottesvilleVA22904 United States 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 DARK Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen2200 Denmark Astrophysics Research Centre School of Mathematics and Physics Queen's University Belfast BelfastBT7 1NN United Kingdom School of Physics The University of Melbourne VIC3010 Australia Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States LSST-DA Catalyst Gemini Observatory NSF's National Optical-Infrared Astronomy Research Laboratory Casilla 603 La Serena Chile Space Telescope Science Institute BaltimoreMD21218 United States Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States David A. Dunlap Department of Astronomy and Astrophysics University of Toronto 50 St. George Street TorontoONM5S 3H4 Canada Department of As

We present ultraviolet/optical/near-infrared observations and modeling of Type II supernovae (SNe II) whose early-time (δt 15 cm) circumstellar material (CSM). The observed electron-scattering broadened line profiles (i.e., IIn-like) of H i, He i/ii, C iv, and N iii/iv/v from the CSM persist on a characteristic timescale (tIIn) that marks a transition to a lower-density CSM and the emergence of Doppler-broadened features from the fast-moving SN ejecta. Our sample, the largest to date, consists of 39 SNe with early-time IIn-like features in addition to 35 "comparison" SNe with no evidence of early-time IIn-like features, all with ultraviolet observations. The total sample consists of 50 unpublished objects with a total of 474 previously unpublished spectra and 50 multiband light curves, collected primarily through the Young Supernova Experiment and Global Supernova Project collaborations. For all sample objects, we find a significant correlation between peak ultraviolet brightness and both tIIn and the rise time, as well as evidence for enhanced peak luminosities in SNe II with IIn-like features. We quantify mass-loss rates and CSM density for the sample through matching of peak multiband absolute magnitudes, rise times, tIIn and optical SN spectra with a grid of radiation hydrodynamics and non-local thermodynamic equilibrium (nLTE) radiative-transfer simulations. For our grid of models, all with the same underlying explosion, there is a trend between the duration of the electron-scattering broadened line profiles and inferred mass-loss rate: tIIn ≈ 3.8[M¤/(0.01 M☉ yr−1)] days. Copyright © 2024, The Authors. All rights reserved.

关键词： Supernovae

Optical precursors to X-ray binary outbursts

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arXiv 2019年

作者： Russell, D.M. Bramich, D.M. Lewis, F. AlMannaei, A. Al Qaissieh, T. Al Qasim, A. Al Yazeedi, A. Baglio, M.C. Bernardini, F. Elgalad, N. Gabuya, A. Lasota, J.P. Palado, A. Roche, P. Shivkumar, H. Udrescu, S. Zhang, G. New York University Abu Dhabi Abu Dhabi United Arab Emirates Faulkes Telescope Project School of Physics and Astronomy Cardiff University Cardiff United Kingdom Astrophysics Research Institute Liverpool John Moores University Liverpool United Kingdom Al Sadeem Observatory Abu Dhabi United Arab Emirates Mullard Space Science Laboratory University College London Dorking United Kingdom INAF–Osservatorio Astronomico di Brera Merate Italy INAF–Osservatorio Astronomico di Roma Roma Italy INAF–Osservatorio Astronomico di Capodimonte Napoli Italy Paris-Sorbonne University Abu Dhabi Abu Dhabi United Arab Emirates Institut d’Astrophysique de Paris CNRS et Sorbonne Université Paris France Nicolaus Copernicus Astronomical Center Polish Academy of Sciences Warsaw Poland Kunming China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming China Center for Astronomical Mega-Science CAS Beijing China

Disc instability models predict that for X-ray binaries in quiescence, there should be a brightening of the optical flux prior to an X-ray outburst. Tracking the X-ray variations of X-ray binaries in quiescence is generally not possible, so optical monitoring provides the best means to measure the mass accretion rate variability between outbursts, and to identify the beginning stages of new outbursts. With our regular Faulkes Telescope/Las Cumbres Observatory (LCO) monitoring we are routinely detecting the optical rise of new X-ray binary outbursts before they are detected by X-ray all-sky monitors. We present examples of detections of an optical rise in X-ray binaries prior to X-ray detection. We also present initial optical monitoring of the new black hole transient MAXI J1820+070 (ASASSN-18ey) with the Faulkes, LCO telescopes and Al Sadeem Observatory in Abu Dhabi, UAE. Finally, we introduce our new real-time data analysis pipeline, the "X-ray Binary New Early Warning System (XB-NEWS)" which aims to detect and announce new X-ray binary outbursts within a day of first optical detection. This will allow us to trigger X-ray and multi-wavelength campaigns during the very early stages of outbursts, to constrain the outburst triggering mechanism. Copyright © 2019, The Authors. All rights reserved.

关键词： Stars

Study of photometric phase curve with new brightness model:refining phase function system parameters of asteroid(107)Camilla

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Research in Astronomy and Astrophysics 2016年第9期16卷 117-122页

作者： Yi-Bo Wang Xiao-Bin Wang Ao Wang Yunnan Observatories Chinese Academy of SciencesKunming 650011China University of Chinese Academy of Sciences Beijing 100049China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650011China

We characterize the morphology of the photometric phase curve model of an asteroid with a three- parameter magnitude phase function H - G1 - G2 system by considering the effect of brightness variation arising from a triaxial ellipsoid representing the asteroid＇s shape. Applying this new model and a Markov Chain Monte Carlo method, we refine the photometric phase curve of asteroid （107） Camilla and obtain its absolute magnitude H = 7.026-0.054^＋0.052 mag, and phase function parameters G1=0.489-0.044^＋0.043 and G2 = 0.259-0.023^＋***, we also determine （107） Camilla＇s orientation of pole （74.1°-4.5°^＋4.3°,50.2°-5.0°^＋5.4°）. with rotational period of 4.843928-0.000001^＋0.000001 h, and axial ratios a/b ： 1.409-0.020^＋0.020 And b/c =1.249-0.060^＋0.063. Furthermore, according to the values of phase function parameters G1 and G2, we infer that asteroid （107） Camilla is an X-type asteroid.

关键词： minor planets, asteroids general phase curve -- minor planets, asteroids individual （107）Camilla -- techniques photometric