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Can Helium-detonation model explain the observed diversity of type Ia supernovae?

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arXiv 2020年

作者： Li, Wenxiong Wang, Xiaofeng Bulla, Mattia Pan, Yen-Chen Wang, Lifan Mo, Jun Zhang, Jujia Wu, Chengyuan Zhang, Jicheng Zhang, Tianmeng Xiang, Danfeng Lin, Han Sai, Hanna Zhang, Xinghan Chen, Zhihao Yan, Shengyu Tsinghua University Beijing100084 China School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Beijing Planetarium Beijing Academy of Science and Technology Beijing100089 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China Nordita KTH Royal Institute of Technology Stockholm University Roslagstullsbacken 23 Stockholm106 91 Sweden Graduate Institute of Astronomy National Central University 300 Jhongda Road Zhongli Taoyuan32001 Taiwan George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy Texas A. & M. University Department of Physics and Astronomy 4242 TAMU College StationTX77843 United States Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing10101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China

We study a sample of 16 Type Ia supernovae (SNe Ia) having both spectroscopic and photometric observations within 2 − 3 days after the first light. The early B − V colors of such a sample tends to show a continuous distribution. For objects with normal ejecta velocity (NV), the C II λ6580 feature is always visible in the early spectra while it is absent or very weak in the high-velocity (HV) counterpart. Moreover, the velocities of the detached high-velocity features (HVFs) of Ca II NIR triplet (CaIR3) above the photosphere are found to be much higher in HV objects than in NV objects, with typical values exceeding 30,000 km s−1 at 2 − 3 days. We further analyze the relation between the velocity shift of late-time [Fe II] lines (v[Fe II]) and host galaxy mass. We find that all HV objects have redshifted v[Fe II] while NV objects have both blue- and redshifted v[Fe II]. It is interesting to point out that the objects with redshifted v[Fe II] are all located in massive galaxies, implying that HV and a portion of NV objects may have similar progenitor metallicities and explosion mechanisms. We propose that, with a geometric/projected effect, the He-detonation model may account for the similarity in birthplace environment and the differences seen in some SNe Ia, including B − V colors, C II feature, CaIR3 HVFs at early time and v[Fe II] in the nebular phase. Nevertheless, some features predicted by He-detonation simulation, such as the rapidly decreasing light curve, deviate from the observations, and some NV objects with blueshifted nebular v[Fe II] may involve other explosion mechanisms. © 2020, CC-BY.

关键词： Velocity

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

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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 ( ${\tau }_{\mathrm{in}}\propto {M}_{\mathrm{BH}}^{0.2{9}_{-0.06}^{+0.06}}{P}_{\mathrm{jet}}^{-0.{3}_{-0.03}^{+0.03}}$

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

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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

Erratum: Formation of millisecond pulsars with helium white dwarfs, ultra-compact X-ray binaries, and gravitational wave sources

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Monthly Notices of the Royal Astronomical Society 2021年第3期506卷 4446-4446页

作者： Chen, Hai-Liang Tauris, Thomas M Han, Zhanwen Chen, Xuefei Yunnan Observatories Chinese Academy of Sciences (CAS) Kunming 650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China Department of Physics and Astronomy Aarhus University Ny Munkegade 120 DK-8000 Aarhus C Denmark Aarhus Institute of Advanced Studies (AIAS) Aarhus University Høegh-Guldbergs Gade 6B DK-8000 Aarhus C Denmark University of the Chinese Academy of Sciences Yuquan Road 19 Shijingshan Block Beijing 100049 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing 100012 China

Convective overshooting in sdB stars using the k-ω model

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arXiv 2018年

作者： Li, Yan Chen, Xing-hao Xiong, He-ran Guo, Jun-jun Chen, Xue-fei Han, Zhan-wen Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China

Mixing in the convective core is quite uncertain in core helium burning stars. In order to explore the overshooting mixing beyond the convective core, we incorporated the k-ω proposed by Li (2012, 2017) into MESA, and investigated the overshooting mixing in evolution of sdB models. We found that the development of the convective core can be divided into three stages. When the radiative temperature gradient ∇rad monotonically decreases from the stellar center, the overshooting mixing presents a behaviour of exponential decay similar with Herwig (2000), and the overshooting distance is to make ∇rad ∇ad at the boundary of the convective core, in agreement with the prediction of the self-driving mechanism Castellani, Giannone & Renzini (1971a). When the radiative temperature gradient ∇rad shows a minimum value in the convective core, the convective core may be divided into two convection zones if the minimum value of ∇rad is smaller than the adiabatic temperature gradient ∇ad. For the single-zone case, the overshooting mixing still shows an exponential decay behaviour, but the overshooting distance is much smaller than in the initial stage. For the double-zone case, the overshooting mixing is similar to that of the single-case beyond the convective core, while it almost stops on both sides of the above convective shell. Our overshooting mixing scheme is similar to the maximal overshoot scheme of Constantino et al. (2015). In the final stage, continuous injection of fresh helium into the convective core by the overshooting mixing happens, which is similar to the"core breathing pulses" (Sweigart & Demarque 1973;Castellani et al. 1985). Copyright © 2018, The Authors. All rights reserved.

关键词： Mixing

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

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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

The enigmatic double-peaked stripped-envelope SN 2023aew

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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

Overshooting in the core helium burning stage of a 30Mostar using the k-ω model

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arXiv 2018年

作者： Li, Yan Chen, Xing-Hao Chen, Hai-Liang Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China

Overshooting and semiconvection are among the most uncertainties in the evolution of massive stars. Complete mixing over a certain distance beyond the convective boundary (Stothers & Chin 1985) and an exponentially decaying diffusion outside the convection zone (Herwig 2000) are commonly adopted for the overshoot mixing. Recently, Li (2012, 2017) developed the k-ω model, which can be used in both convection zones and overshooting regions. We incorporated it in calculations of 30Mostellar models. We find that in the main sequence stage, models with the k-ω model are almost identical to models with complete mixing in the overshooting region beyond the convective core, and the overshooting in the k-ω model is equivalent to an overshooting distance of about 0.15HP . In the post main sequence stage, we find that the overshooting below the bottom of the intermediate convection zone beyond the hydrogen-burning shell can significantly restrict the size of the hydrogendepleted core, and can penetrate effectively into the hydrogen-burning shell. These two effects are crucial for the evolution of the core helium burning stage. During the core helium burning stage, we find that the overshooting model based on the k-ω model results in a similar complete mixing region but a much wider partial mixing region than the overshooting model based on Herwig (2000). In particular, the overshooting distance in the core helium burning stage may be significantly smaller than that in the main sequence phase for massive stars. Copyright © 2018, The Authors. All rights reserved.

关键词： Mixing

Study of photometric phase curve:assuming a cellinoid ellipsoid shape for asteroid(106)Dione

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Research in Astronomy and Astrophysics 2017年第9期17卷 61-70页

作者： Yi-Bo Wang Xiao-Bin Wang Donald E Pray Ao Wang Yunnan Observatories Chinese Academy of SciencesKunming 650216China University of Chinese Academy of Sciences Beijing 100049China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650216China Center for Astronomical Mega-Science Chinese Academy of SciencesBeijing 100012China Sugarloaf Mountain Observatory South DeerfieldMA 01373USA

We carried out new photometric observations of asteroid （106） Dione at three apparitions （2004, 2012 and 2015） to understand its basic physical properties. Based on a new brightness model, new photometric observational data and published data of （106） Dione were analyzed to characterize the morphology of Dione＇s photometric phase curve. In this brightness model, a cellinoid ellipsoid shape and three-parameter （H, G1, G2） magnitude phase function system were involved. Such a model can not only solve the phase function system parameters of （106） Dione by considering an asymmetric shape of an asteroid, but also can be applied to more asteroids, especially those without enough photometric data to solve the convex shape. Using a Markov Chain Monte Carlo （MCMC） method, Dione＇s absolute magnitude of H = 7.66＋0.03-0.03 mag, and phase function parameters G1 = 0.682＋0.077-0.077 and G2 = 0.081＋0.042-0.042 were obtained. Simultaneously, Dione＇s simplistic shape, orientation of pole and rotation period were also determined preliminarily.

关键词： asteroids general photometric phase curve -- asteroids individual （106） Dione - techniques： photometric - Markov Chain Monte Carlo method