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Asteroseismology of the DBV star CBS 114

Research in Astronomy and Astrophysics 2016年第8期16卷 17-24页

作者： Yan-Hui Chen Institute of Astrophysics Chuxiong Normal University School of Physics and Electronical Science Chuxiong Normal University Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences

Asteroseismology is a unique and powerful tool to investigate the internal structure of stars. CBS 114 is the sixth known pulsating DBV star. It was observed by Handler, Metcalfe, ＆ Wood at the South African Astronomical Observatory over three weeks in 2001. Then, it was observed by Metcalfe et al. for seven nights （2004 Feb. 19-25） on the 1.8 m telescope at the Bohyunsan Optical Astronomy Observatory and seven nights （2004 Feb. 21-27） on the 2.1 m telescope at the McDonald Observatory. Totally two triplets, four doublets, and five singlets were identified. The frequency splitting values are very different, from 5.2 *** to 11.9 ~tHz, which may reflect differential rotations. We evolve grids of white dwarf models by MESA. Cores, added with He/C envelopes, of those white dwarf models are inserted into WDEC to evolve grids of DBV star models. With those DBV star models, we calculate eigenperiods. Those calculated periods are used to fit observed periods. A best-fitting model is selected. The parameters are T^ff ----- 25 000 K, M, = 0.740 MG and log（MHe/M,） = -4.5. With the relatively large stellar mass, the effective temperature is close to the previous spectroscopic result. In addition, kinetic energy distributions are calculated for the best-fitting model. We find that the observed modes with large frequency splitting values are fitted by the calculated modes with a large amount of kinetic energy distributed in the C/O core. After preliminary analysis, we suggest that the C/O core may rotate at least two times faster than the helium layer for CBS 114.

关键词： stars： oscillations （including pulsations） -- stars： individual （CBS 114） -- white dwarfs

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

arXiv

引用

arXiv 2022年

作者： Sai, Hanna Wang, Xiaofeng Elias-Rosa, Nancy Yang, Yi Zhang, Jujia Lin, Weili Mo, Jun Piro, Anthony L. Zeng, Xiangyun Andrea, Reguitti Brown, Peter Burns, Christopher R. Cai, Yongzhi Fiore, Achille Hsiao, Eric Y. Isern, Jordi Itagaki, K. Li, Wenxiong Li, Zhitong Pessi, Priscila J. Phillips, M.M. Schuldt, Stefan Shahbandeh, Melissa Stritzinger, Maximilian D. Tomasella, Lina Vogl, Christian Wang, Bo Wang, Lingzhi Wu, Chengyuan Yang, Sheng Zhang, Jicheng Zhang, Tianmeng Zhang, Xinghan Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China INAF - Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 Padova35122 Italy Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain Department of Astronomy University of California BerkeleyCA94720-3411 United States Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Carnegie Observatories 813 Santa Barbara Street PasadenaCA91101 United States Center for Astronomy and Space Sciences China Three Gorges University Yichang443000 China Departamento de Ciencias Físicas Universidad Andrés Bello Avda. República 252 Santiago8320000 Chile Millennium Institute of Astrophysics Nuncio Monsenor Sótero Sanz 100 Providencia Santiago8320000 Chile George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy Texas A. & M. University 4242 TAMU College StationTX77843 United States Department of Physics Florida State University 77 Chieftan Way TallahasseeFL32306 United States c/Gran Capitá 2-4 Edif. Nexus 201 Barcelona08034 Spain Itagaki Astronomical Observatory Yamagata Yamagata990-2492 Japan The School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata Paseo del Bosque S/N La PlataB1900FWA Argentina Carnegie Observatories Las Campanas Observatory Colina El Pino Casilla 601 Chile Max-Planck-Institut für Astrophysik Karl-Schwarzschild Str. 1 G

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

关键词： Supernovae

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A comprehensive bayesian discrimination of the simple stellar population model, star formation history and dust attenuation law in the spectral energy distribution modeling of galaxies

arXiv

引用

arXiv 2018年

作者： Han, Yunkun Han, Zhanwen Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 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 396 Yangfangwang Guandu District Kunming650216 China

When modeling and interpreting the spectral energy distributions (SEDs) of galaxies, the simple stellar population (SSP) model, star formation history (SFH) and dust attenuation law (DAL) are three of the most important components. However, each of them carries significant uncertainties which have seriously limited our ability to reliably recover the physical properties of galaxies from the analysis of their SEDs. In this paper, we present a Bayesian framework to deal with these uncertain components simultaneously. Based on the Bayesian evidence, a quantitative implement of the principle of Occam's razor, the method allows a more objective and quantitative discrimination among the different assumptions about these uncertain components. With a Ks-selected sample of 5467 lowredshift (mostly with z . 1) galaxies in the COSMOS/UltraVISTA field and classified into passively evolving galaxies (PEGs) and star-forming galaxies (SFGs) with UVJ diagram, we present a Bayesian discrimination of a set of 16 SSP models from five research groups (BC03 and CB07, M05, GALEV, Yunnan-II, BPASS V2.0), five forms of SFH (Burst, Constant, Exp-dec, Exp-inc, Delayed-t), and four kinds of DAL (Calzetti law, MW, LMC, SMC). We show that the results obtained with the method are either obvious or understandable in the context of galaxy physics. We conclude that the Bayesian model comparison method, especially that for a sample of galaxies, is very useful for discriminating the different assumptions in the SED modeling of galaxies. The new version of the BayeSED code, which is used in this work, is publicly available at https://***/hanyk/bayesed/. Copyright © 2018, The Authors. All rights reserved.

关键词： Spectroscopy

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Binary population synthesis for the core-degenerate scenario of SN ia progenitors

Binary population synthesis for the core-degenerate scenario...

引用

2017 AGB-Supernovae Mass Transition

作者： Wang, B. 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 20A Datun Road Chaoyang District Beijing100012 China

The core-degenerate (CD) scenario has been proposed as an alternative way for the production of type Ia supernovae (SNe Ia). In this scenario, SNe Ia are formed at the final stage of common-envelope evolution from a merger of a carbon-oxygen white dwarf (CO WD) with the CO core of an asymptotic giant branch companion. However, the birthrates of SNe Ia from this scenario are still not well determined. In this work, we performed a detailed investigation on the CD scenario based on a binary population synthesis (BPS) approach. The SN Ia delay times for this scenario are mainly in the range of ∼90 Myr−2200 Myr, contributing to the observed SNe Ia with short and intermediate delay times. The Galactic birthrates of SNe Ia from this scenario range from ∼4.6×10−5yr−1 to ∼4.3×10−4yr−1, accounting for ∼2−14% of total SNe Ia. Especially, SNe Ia with circumstellar material from this scenario contribute to ∼1−10% of total SNe Ia, which means that the CD scenario can reproduce the observed birthrates of SNe Ia like PTF 11kx. © SAIt 2017.

关键词： White dwarfs

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

arXiv

引用

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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Resolved neutral carbon emission in nearby galaxies: [C i] lines as total molecular gas tracers

arXiv

引用

arXiv 2019年

作者： Jiao, Qian Zhao, Yinghe Lu, Nanyao Gao, Yu Salak, Dragan Zhu, Ming Zhang, Zhiyu Jiang, Xuejian Tan, Qinghua Nanjing210008 China Yunnan Observatories & Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650011 China Center for Astronomical Mega-Science CAS 20A Datun Road Chaoyang District Beijing100012 China Camino El Observatorio 1515 Las Condes Santiago Chile National Astronomical Observatories & Key Lab of Radio Astronomy CAS Beijing100012 China School of Science and Technology Kwansei Gakuin University 2-1 Gakuen SandaHyogo669-1337 Japan Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom ESO Karl Schwarzschild Strasse 2 Garching MunichD-85748 Germany

We present maps of atomic carbon [C i] (3P1 → 3P0) and [C i] (3P2 → 3P1) emission (hereafter [C i] (1−0) and [C i] (2−1), respectively) at a linear resolution ∼ 1 kpc scale for a sample of one Hii, six LINER, three Seyfert and five starburst galaxies observed with the Herschel Space Observatory. We compare spatial distributions of two [C i] lines with that of CO J = 1 → 0 (hereafter CO (1−0)) emission, and find that both [C i] lines distribute similarly to CO (1−0) emission in most galaxies. We present luminosity ratio maps of L0[CI](1−0)/L0CO(1−0), L0[CI](2−1)/L0CO(1−0), L0[CI](2−1)/L0[CI](1−0) (hereafter R[CI]) and 70-to-160 µm far-infrared color of f70/f160. L0[CI](2−1)/L0CO(1−0), R[CI] and f70/f160 are centrally peaked in starbursts;whereas remain relatively constant in LINERs, indicating that star-forming activity can enhance carbon emission, especially for [C i] (2−1). We explore the correlations between the luminosities of CO (1−0) and [C i] lines, and find that L0CO(1−0) correlates tightly and almost linearly with both L0[CI](1−0) and L0[CI](2−1), suggesting that [C i] lines, similar as CO (1−0), can trace total molecular gas in Hii, LINER, Seyfert and starburst galaxies on kpc scales. We investigate the dependence of L0[CI](1−0)/L0CO(1−0), L0[CI](2−1)/L0CO(1−0) and [C i] excitation temperature of Tex on dust temperature of Tdust, and find non-correlation, a weak and modest correlation, respectively. The ratio of L0[CI](1−0)/L0CO(1−0) stays smooth distribution in most galaxies, indicating that the conversion factor of [C i] (1−0) luminosity to H2 mass (X[CI](1−0)) changes with CO (1−0) conversion factor (αCO) proportionally. Under optically thin and local thermodynamical equilibrium (LTE) assumptions, we derive a galaxy-wide average carbon excitation temperature of Tex ∼ 19.7 ± 0.5 K and an average neutral carbon abundance of X[CI]/X[H2] ∼ 2.5 ± 1.0 × 10−5 in our resolved sample, which is comparable to the usually adopted value of 3 × 10−5, but ∼ 3 times low

关键词： Galaxies

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Multi-wavelength observations of the BL Lac object Fermi J1544-0649: One year after its awakening

arXiv

引用

arXiv 2020年

作者： Tam, P.H.T. Pal, P.S. Cui, Y.D. Jiang, N. Sotnikova, Y. Yang, C.W. Wang, L.Z. Tang, B.T. Li, Y.B. Mao, J. Kong, A.K.H. Zhong, Z.H. Ding, J. Mufakharov, T. Fan, J.F. Dou, L.M. Shen, R.F. Ai, Y.L. School of Physics and Astronomy Sun Yat-sen University Guangzhou510275 China CAS Key Laboratory for Researches in Galaxies and Cosmology University of Sciences and Technology of China Hefei Anhui230026 China Special Astrophysical Observatory Russian Academy of Sciences Nizhnij Arkhyz369167 Russia Polar Research Institute of China 451 Jinqiao Road Shanghai200136 China Chinese Academy of Sciences South America Center for Astronomy China-Chile Joint Center for Astronomy Camino El Observatorio #1515 Las Condes Santiago Chile Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Institute of Astronomy National Tsing Hua University 101 Section 2. Kuang-Fu Road Hsinchu30013 Taiwan Department of Astronomy & Astrophysics University of California Santa Cruz 1156 High Street Santa CruzCA95060 United States Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Kazan Federal University 18 Kremlyovskaya St. Kazan420008 Russia Center for Astrophysics Guangzhou University Guangzhou510006 China

We report observations of a transient source Fermi J1544-0649 from radio to γrays. Fermi J1544-0649 was discovered by the Fermi-LAT in May 2017. Followup Swift-XRT observations revealed three flaring episodes through March 2018, and the peak X-ray flux is about 103 higher than the ROSAT all-sky survey (RASS) flux upper limit. Optical spectral measurements taken by the Magellan 6.5-m telescope and the Lick-Shane telescope both show a largely featureless spectrum, strengthening the BL Lac interpretation first proposed by Bruni et al. (2018). The optical and mid-infrared (MIR) emission goes to a higher state in 2018, when the flux in high energies goes down to a lower level. Our RATAN-600m measurements at 4.8 GHz and 8.2 GHz do not indicate any significant radio flux variation over the monitoring seasons in 2017 and 2018, nor deviate from the archival NVSS flux level. During GeV flaring times, the spectrum is very hard (Γγ ∼1.7) in the GeV band and at times also very hard ((ΓX 2) in the X-rays, similar to a high-synchrotron-peak (or even an extreme) BL Lac object, making Fermi J1544-0649 a good target for ground-based Cherenkov telescopes. Copyright © 2020, The Authors. All rights reserved.

关键词： Surveys

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The birthrates of SNe Ia in globular clusters

引用

Proceedings of the International Astronomical Union 2017年第S316期12卷 343-344页

作者： Bo Wang Dongdong Liu Yunnan Observatories Chinese Academy of Sciences Kunming 650216 China (email: wangbo@***) Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650216 China

Globular clusters has been proposed as testbeds for type Ia supernovae (SNe Ia). In this work, using a detailed binary population synthesis approach, we studied the birthrates of SNe Ia from various progenitor models in globular clusters, including the single-degenerate model, the double-degenerate model and the Sub-Chandrasekhar model. Here, a single starburst with a total mass of 106M⊙ is assumed.

关键词： binaries: close supernovae: general white dwarfs

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SN 2020pvb: a Type IIn-P supernova with a precursor outburst

arXiv

引用

arXiv 2024年

作者： Elias-Rosa, Nancy Brennan, Seán J. Benetti, Stefano Cappellaro, Enrico Pastorello, Andrea Kozyreva, Alexandra Lundqvist, Peter Fraser, Morgan Anderso, Joseph P. Cai, Yong-Zhi Chen, Ting-Wan Dennefeld, Michel Gromadzki, Mariusz Gutiérrez, Claudia P. Ihanec, Nada Inserra, Cosimo Kankare, Erkki Kotak, Rubina Mattila, Seppo Moran, Shane Müller-Bravo, Tomás E. Pessi, Priscila J. Pignata, Giuliano Reguitti, Andrea Reynolds, Thomas M. Smartt, Stephen J. Smith, Ken Tartaglia, Leonardo Valerin, Giorgio de Boer, Thomas Chambers, Kenneth Gal-Yam, Avishay Gao, Hua Geier, Stefan Mazzali, Paolo A. Nicholl, Matt Ragosta, Fabio Rest, Armin Yaron, Ofer Young, David R. INAF – Osservatorio Astronomico di Padova vicolo dell’Osservatorio 5 PadovaI-35122 Italy Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Ireland Heidelberger Institut für Theoretische Studien Schloss-Wolfsbrunnenweg 35 Heidelberg69118 Germany European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago Chile Nuncio Monseñor Sótero Sanz 100 Off. 104 Providencia Santiago Chile 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 98bis Boulevard Arago ParisF-75014 France Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warszawa00-478 Poland BarcelonaE-08034 Spain Cardiff Hub for Astrophysics Research and Technology School of Physics & Astronomy Cardiff University Queens Buildings The Parade CardiffCF24 3AA United Kingdom Tuorla Observatory Department of Physics and Astronomy University of Turku FI-20014 Finland Turku Collegium for Science Medicine and Technology University of Turku TurkuFI-20014 Finland School of Sciences European University Cyprus Diogenes street Engomi Nicosia1516 Cyprus Instituto de Alta Investigación Universidad de Tarapacá Casilla 7D Arica Chile MerateI-23807 Italy Cosmic DAWN centre Niels Bohr Institute University of Copenhagen Jagtvej 128 København N2200 Denmark Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Astrophysics Research Centre School of Mathematics and Physics Queen’s University Be

We present photometric and spectroscopic data sets for SN 2020pvb, a Type IIn-P supernova (SN) similar to SNe 1994W, 2005cl, 2009kn and 2011ht, with a precursor outburst detected (PS1 w-band ∼ -13.8 mag) around four months before the B-band maximum light. SN 2020pvb presents a relatively bright light curve peaking at MB = -17.95 ± 0.30 mag and a plateau lasting at least 40 days before it went in solar conjunction. After this, the object is no longer visible at phases > 150 days above -12.5 mag in the B-band, suggesting that the SN 2020pvb ejecta interacts with a dense spatially confined circumstellar envelope. SN 2020pvb shows in its spectra strong Balmer lines and a forest of Fe ii lines with narrow P Cygni profiles. Using archival images from the Hubble Space Telescope, we constrain the progenitor of SN 2020pvb to have a luminosity of log(L/L☉) 5.4, ruling out any single star progenitor over 50 M☉. All in all, SN 2020pvb is a Type IIn-P whose progenitor star had an outburst ∼ 0.5 yr before the final explosion, the material lost during this outburst is probably playing a role in shaping the physical properties of the supernova. Copyright © 2024, The Authors. All rights reserved.

关键词： Supernovae

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Erratum: 'The Escape of the Hydrogen-rich Atmosphere of Exoplanets: Mass-loss Rates and the Absorptions of Stellar Lyα' (2019, ApJ, 880, 90)

引用

The Astrophysical Journal 2019年第2期883卷

作者： Dongdong Yan Jianheng Guo Yunnan Observatories Chinese Academy of Sciences P.O. Box 110 Kunming 650011 People's Republic of China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing People's Republic of China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming 650011 People's Republic of China

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