检索结果-内蒙古大学图书馆

arXiv 2020年

作者： Zhang, Jujia Wang, Xiaofeng Vinkó, József Zhai, Qian Zhang, Tianmeng Filippenko, Alexei V. Brink, Thomas G. Zheng, WeiKang Wyrzykowski, Lukasz Mikolajczyk, Przemyslaw Huang, Fang Rui, Liming Mo, Jun Sai, Hanna Zhang, Xinhan Wang, Huijuan DerKacy, James M. Baron, Eddie Sárneczky, K. Bódi, A. Csörnyei, G. Hanyecz, O. Ignácz, B. Kalup, Cs. Kriskovics, L. Könyves-Tóth, R. Ordasi, A. Pál, A. Sódor, Á. Szakáts, R. Vida, K. Zsidi, G. Kunming650216 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650216 China Center for Astronomical Mega-Science CAS 20A Datun Road Chaoyang District Beijing100012 China Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 China Konkoly Observatory CSFK Konkoly-Thege M. ut 15-17 Budapest1121 Hungary ELTE Eötvös Loránd University Institute of Physics Pázmány Péter sétány 1/A Budapest1117 Hungary Department of Optics and Quantum Electronics University of Szeged Dóm tér 9 Szeged6720 Hungary Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China School of Astronomy and Space Science University of Chinese Academy of Sciences Beijing101408 China Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Astronomical Institute University of Wroclaw M. Kopernika 11 Wroclaw51-622 Poland Department of Astronomy Shanghai Jiao Tong University Shanghai200240 China Homer L. Dodge Department of Physics and Astronomy University of Oklahoma NormanOK73019 United States ELTE Eötvös Loránd University Department of Astronomy Pázmány Péter sétány 1/A Budapest1117 Hungary MTA CSFK Lendület Near-Field Cosmology Research Group Konkoly Observatory Budapest1121 Hungary European Southern Observatory Karl-Schwarzschild-Strasse 2 Garching bei München85748 Germany

We present extensive observations of SN 2018zd covering the first ∼ 450 d after the explosion. This SN shows a possible shock-breakout signal ∼ 3.6 hr after the explosion in the unfiltered light curve, and prominent flash-ionisation spectral features within the first week. The unusual photospheric temperature rise (rapidly from ∼ 12, 000 K to above 18,000 K) within the earliest few days suggests that the ejecta were continuously heated. Both the significant temperature rise and the flash spectral features can be explained with the interaction of the SN ejecta with the massive stellar wind (0.18+−000510 M), which accounts for the luminous peak (Lmax = [1.36±0.63]×1043 erg s−1) of SN 2018zd. The luminous peak and low expansion velocity (v ≈ 3300 km s−1) make SN 2018zd to be like a member of the LLEV (luminous SNe II with low expansion velocities) events originated due to circumstellar interaction. The relatively fast post-peak decline allows a classification of SN 2018zd as a transition event morphologically linking SNe IIP and SNe IIL. In the radioactive-decay phase, SN 2018zd experienced a significant flux drop and behaved more like a low-luminosity SN IIP both spectroscopically and photometrically. This contrast indicates that circumstellar interaction plays a vital role in modifying the observed light curves of SNe II. Comparing nebular-phase spectra with model predictions suggests that SN 2018zd arose from a star of ∼ 12 M . Given the relatively small amount of 56Ni (0.013 − 0.035M), the massive stellar wind, and the faint X-ray radiation, the progenitor of SN 2018zd could be a massive asymptotic giant branch star which collapsed owing to electron capture. Copyright © 2020, The Authors. All rights reserved.

关键词： Expansion

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MULTI-WAVELENGTH OBSERVATIONS OF A NEW REDBACK MILLISECOND PULSAR CANDIDATE: 3FGL J0954.8−3948

arXiv

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arXiv 2018年

作者： Li, Kwan-Lok Hou, Xian Strader, Jay Takata, Jumpei Kong, Albert K.H. Chomiuk, Laura Swihart, Samuel J. Hui, Chung Yue Cheng, K.S. Department of Physics and Astronomy Michigan State University East LansingMI48824 United States Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China School of physics Huazhong University of Science and Technology Wuhan430074 China Institute of Astronomy National Tsing Hua University Hsinchu30013 Taiwan Department of Astronomy and Space Science Chungnam National University Daejeon34134 Korea Republic of Department of Physics University of Hong Kong Pokfulam Road Hong Kong

We present a multi-wavelength study of the unassociated Fermi-LAT source, 3FGL J0954.8−3948, which is likely the γ-ray counterpart of a 9.3-hour binary in the field. With more than 9 years of Pass 8 LAT data, we updated the γ-ray spectral properties and the LAT localization of the γ-ray source. While the binary lies outside the cataloged 95% error ellipse, the optimized LAT ellipse is 0.1 degrees closer and encloses the binary. The system is likely spectrally hard in X-rays (photon index ΓX = 1.4−+11..20) with orbital modulations detected in optical, UV, and possibly X-rays. A steep spectrum radio counterpart (spectral index α ≈ −1.6) is also found in the TIFR GMRT Sky Survey (TGSS), implying that it is a pulsar system. We obtained a series of SOAR and Gemini spectroscopic observations in 2017/2018, which show a low-mass secondary orbiting in a close circular orbit with K2 = 272 ± 4 km s−1 under strong irradiation by the primary compact object. All the observations as well as the modelling of the X/γ-ray high-energy emission suggest that 3FGL J0954.8−3948 is a redback millisecond pulsar in a rotation-powered state. Copyright © 2018, The Authors. All rights reserved.

关键词： Pulsars

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ALMA [N ii ] 205 µm Imaging Spectroscopy of the Lensed Submillimeter galaxy ID 141 at redshift 4.24

arXiv

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arXiv 2020年

作者： Cheng, Cheng Cao, Xiaoyue Lu, Nanyao Li, Ran Yang, Chentao Rigopoulou, Dimitra Charmandaris, Vassilis Gao, Yu Xu, Cong Kevin van der Werf, Paul Santos, Tanio Diaz Privon, George C. Zhao, Yinghe Cao, Tianwen Dai, Y. Sophia Huang, Jia-Sheng Sanders, David Wang, Chunxiang Wang, Zhong Zhu, Lei National Astronomical Observatories Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100101 China China-Chile Joint Center for Astronomy Camino El Observatorio 1515 Las Condes Santiago Chile Instituto de Física y Astronomía Universidad de Valparaíso Avda. Gran Bretaña 1111 Valparaíso Chile 20A Datun Road Chaoyang District Beijing100012 China School of Astronomy and Space Science University of Chinese Academy of Science 19 A Yuquan Rd Shijingshan District Beijing100049 China European Southern Observatory Alonso de CÃşrdova 3107 Casilla 19001 Vitacura Santiago Chile Astrophysics Department University of Oxford OxfordOX1 3RH United Kingdom Department of Physics University of Crete HeraklionGR-71003 Greece Institute of Astrophysics FORTH HeraklionGR-71110 Greece Department of Astronomy Xiamen University XiamenFujian361005 China Nanjing210033 China Leiden Observatory Leiden University P.O. Box 9513 Leiden2300 RA Netherlands Nucleo de Astronomia de la Facultad de Ingenieria Universidad Diego Portales Av. Ejercito Libertador 441 Santiago Chile Department of Astronomy University of Florida 211 Bryant Space Sciences Center GainesvilleFL32611 United States Yunnan Observatories Chinese Academy of Sciences Kun-ming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science CAS 20A Datun Road Chaoyang District Beijing100012 China Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States

We present the Atacama Large Millimeter/submillimeter Array (ALMA) observation of the Submillimeter galaxy (SMG) ID 141 at z=4.24 in the [N ii ] 205 µm line (hereafter [N ii ]) and the underlying continuum at (rest-frame) 197.6 µm. Benefiting from lensing magnification by a galaxy pair at z=0.595, ID 141 is one of the brightest z > 4 SMGs. At the angular resolutions of ∼ 1.2″ to 1.5″ (1″∼6.9 kpc), our observation clearly separates, and moderately resolves the two lensed images in both continuum and line emission at S/N > 5 . Our continuum-based lensing model implies an averaged amplification factor of ∼ 5.8 and reveals that the de-lensed continuum image has the Sérsic index'0.95 and the Sérsic radius of ∼0.1800 (∼1.24 kpc). Furthermore, the reconstructed [N ii ] velocity field in the source plane is dominated by a rotation component with a maximum velocity of ∼300 km/s at large radii, indicating a dark matter halo mass of ∼1012M. This, together with the reconstructed velocity dispersion field being smooth and modest in value ( Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

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He-accreting carbon-oxygen white dwarfs and type Ia supernovae

arXiv

引用

arXiv 2017年

作者： Wang, Bo Podsiadlowski, Philipp Han, Zhanwen Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories CAS Kunming650216 China Center for Astronomical Mega-Science CAS Beijing100012 China Department of Astronomy Oxford University OxfordOX1 3RH United Kingdom

He accretion onto carbon-oxygen white dwarfs (COWDs) plays a fundamental role when studying the formation of type Ia supernovae (SNe Ia). Employing the MESA stellar evolution code, we calculated the long-term evolution of He-accreting CO WDs. Previous studies usually supposed that a WD can grow in mass to the Chandrasekhar limit in the stable He burning region and finally produce a SN Ia. However, in this study we find that off-centre carbon ignition occurs in the stable He burning region if the accretion rate is above a critical value (∼2.05 × 10-6Moyr-1), resulting in accretion-induced collapse rather than a SN Ia. If the accretion rate is below the critical value, explosive carbon ignition will eventually happen in the centre producing a SN Ia. Taking into account the possibility of off-centre carbon ignition, we have re-determined the initial parameter space that produces SNe Ia in the He star donor channel, one of the promising channels to produce SNe Ia in young populations. Since this parameter space is smaller than was found in the previous study ofWang et al. (2009), the SN Ia rates are also correspondingly smaller. We also determined the chemical abundance profile of the He-accreting WDs at the moment of explosive carbon ignition, which can be used as initial input for SN Ia explosion models. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

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Revealing two radio active galactic nuclei extremely near PSR J0437-4715

arXiv

引用

arXiv 2018年

作者： Li, Zhixuan Yang, Jun An, Tao Paragi, Zsolt Deller, Adam Reynolds, Cormac Hong, Xiaoyu Wang, Jiancheng Ding, Hao Xia, Bo Yan, Zhen Guo, Li Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan650216 China Department of Space Earth and Environment Chalmers University of Technology Onsala Space Observatory OnsalaSE-43992 Sweden Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai200030 China Postbus 2 DwingelooNL-7990 AA Netherlands Centre for Astrophysics & Supercomputing Swinburne University of Technology John St HawthornVIC3122 Australia CSIRO Astronomy and Space Science KensingtonWA6151 Australia University of Chinese Academy of Sciences 19A Yuquan Road Shijingshan District Beijing100049 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 Key Laboratory of Radio Astronomy Chinese Academy of Sciences Nanjing210009

Newton's gravitational constant G may vary with time at an extremely low level. The time variability of G will affect the orbital motion of a millisecond pulsar in a binary system and cause a tiny difference between the orbital period-dependent measurement of the kinematic distance and the direct measurement of the annual parallax distance. PSR J0437-4715 is the nearest millisecond pulsar and the brightest at radio. To explore the feasibility of achieving a parallax distance accuracy of one light-year, comparable to the recent timing result, with the technique of differential astrometry, we searched for compact radio sources quite close to PSR J0437-4715. Using existing data from the Very Large Array and the Australia Telescope Compact Array, we detected two sources with flat spectra, relatively stable flux densities of 0.9 and 1.0 mJy at 8.4 GHz and separations of 13 and 45 arcsec. With a network consisting of the Long Baseline Array and the Kunming 40-m radio telescope, we found that both sources have a point-like structure and a brightness temperature of >107K. According to these radio inputs and the absence of counterparts in the other bands, we argue that they are most likely the compact radio cores of extragalactic active galactic nuclei rather than Galactic radio stars. The finding of these two radio active galactic nuclei will enable us to achieve a sub-pc distance accuracy with the in-beam phase-referencing very-long-baseline interferometric observations and provide one of the most stringent constraints on the time variability of G in the near future. Copyright © 2018, The Authors. All rights reserved.

关键词： Geometrical optics

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Multi-color blackbody emission in GRB 081221

arXiv

引用

arXiv 2018年

作者： Hou, Shu-Jin Zhang, Bin-Bin Meng, Yan-Zhi Wu, Xue-Feng Liang, En-Wei Lu, Hou-Jun Liu, Tong Liang, Yun-Feng Lin, Lin Lu, Rui-Jing Huang, Jin-Shu Zhang, Bing College of Physics and Electronic Engineering Nanyang Normal University Nanyang Henan473061 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008 China Department of Physics GXU-NAOC Center for Astrophysics and Space Sciences Guangxi University Nanning530004 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China School of Astronomy and Space Science Nanjing University Nanjing210093 China Key Laboratory of Modern Astronomy and Astrophysics Nanjing University Ministry of Education China Department of Astronomy Xiamen University Xiamen Fujian361005 China Department of Astronomy Beijing Normal University Beijing100875 China Department of Physics and Astronomy University of Nevada Las VegasNV89154 United States

The radiation mechanism of the prompt emission of gamma-ray bursts (GRBs) remains an open question. Although their spectra are usually well fitted with the empirical Band function, which is widely believed to be fully nonthermal and interpreted as an optically thin synchrotron emission, accumulating evidence shows that a thermal component actually exists. In this paper, a multicolor blackbody (mBB) model is proposed for the time-integrated spectrum of GRB 081221 by assuming a power-law distribution of the thermal luminosities with temperature, which manifests photospheric emissions from a different radius and/or angle. The effects of the minimum temperature kTmin, the maximum temperature kTmax and the power law index m of the luminosity distribution of an mBB are discussed. The fitting to the time-integrated spectrum during the bright phase (from 20s to 30s since the trigger) of GRB 081221 by the mBB model yields kTmin = 4.4± 0.3 keV, kTmax = 57.0 +1.6-1.4 keV, and m =-0.46+0.05-0.06. When the time bin is small enough, the time-resolved spectra of GRB 081221 are well fitted with a series of single-temperature blackbodies. Our results imply the prompt emission of GRB 081221 is dominated by the photosphere emission and its time-integrated spectrum is a superposition of pure blackbody components at different times, indicating that some empirical Band spectra may be interpreted as mBB if the temperature is widely distributed. Copyright © 2018, The Authors. All rights reserved.

关键词： Gamma rays

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Photometric Investigation of the Contact Binary GU Ori with High Metallicity

arXiv

引用

arXiv 2018年

作者： Zhou, X. Qian, S.-B. Soonthornthum, B. Poshyachinda, S. Zhu, L.-Y. Liu, N.-P. Sarotsakulchai, T. Fang, X.-H. P.O. Box 110 Kunming650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang Dis-trict Beijing100012 China University of the Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China National Astronomical Research Institute of Thailand 260 Moo 4 T. Donkaew A. MaerimChiangmai50180 Thailand

GU Ori was observed with the 1m telescope at Yunnan Observatories in 2005. To determine its physical properties, the Wilson-Devinney program is used. The results reveal that GU Ori is a W-subtype shallow contact binary with a more massive but cooler star 2. The mass of its two component stars are estimated to be M1 = 0.45M☉, M2 = 1.05M☉. The O’Connell effect was reported to be negative on the light curves observed in 2005. However, it changed to a positive one on the light curves observed from 2011 to 2012. The mean surface temperatures of star 2 (T2) determined by the two sets of light curves were different, which may result from stellar activities. The O - C diagram shows that the period of GU Ori is decreasing at a rate of dP/dt = −6.24 × 10−8day · year−1, which may be caused by mass transfer from star 2 to star 1 with a rate of dMdt2 = −2.98 × 10−8M☉/year. GU Ori is a contact binary with quite high metallicity. Copyright © 2018, The Authors. All rights reserved.

关键词： Photometry

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Massive stars, successes and challenges

引用

Proceedings of the International Astronomical Union 2016年第S329期12卷 3-14页

作者： Meynet, Georges Maeder, André Georgy, Cyril Ekström, Sylvia Eggenberger, Patrick Barblan, Fabio Song, Han Feng Department of Astronomy University of Geneva Switzerland College of Science Guizhou University Guiyang Guizhou Province 550025 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China

We give a brief overview of where we stand with respect to some old and new questions bearing on how massive stars evolve and end their lifetime. We focus on the following key points that are further discussed by other contributions during this conference: convection, mass losses, rotation, magnetic field and multiplicity. For purpose of clarity, each of these processes are discussed on its own but we have to keep in mind that they are all interacting between them offering a large variety of outputs, some of them still to be discovered. Copyright © International Astronomical Union 2017.

关键词： convection magnetic field mass loss Massive stars multiplicity rotation

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DE CVn: An eclipsing post-common envelope binary with a circumbinary disk and a giant planet

arXiv

引用

arXiv 2018年

作者： Han, Z.-T. Qian, S.-B. Zhu, L.-Y. Zhi, Q.-J. Dong, A.-J. Soonthornthum, B. Poshyachinda, S. Sarotsakulchai, T. Fang, X.-H. Wang, Q.-S. Voloshina, Irina P. O. Box 110 Kunming650216 China Guizhou Provincial Key Laboratory of Radio Data Processing School of Physics and Electronic Sciences Guizhou Normal University Guiyang550001 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China National Astronomical Research Institute of Thailand Ministry of Science and Technology Bangkok Thailand Sternberg Astronomical Institute Moscow State University Universitetskij prospect 13 Moscow119992 Russia

We present a timing analysis of the eclipsing post-common envelope binary (PCEB) DE CVn. Based on new CCD photometric observations and the published data, we found that the orbital period in DE CVn has a cyclic period oscillation with an amplitude of 28.08 s and a period of 11.22 years plus a rapid period decrease at a rate of P = -3.35 × 10-11ss-1. According to the evolutionary theory, secular period decreases in PCEBs arise from angular momentum losses (AMLs) driven by gravitational radiation (GR) and magnetic braking (MB). However, the observed orbital decay is too fast to be produced by AMLs via GR and MB, indicating that there could be other AML mechanism. We suggest that a circumbinary disk around DE CVn may be responsible for the additional AML. The disk mass was derived as a few × 10-4-10-3Mo, which is in agreement with that inferred from previous studies in the order of magnitude. The cyclic change is most likely result of the gravitational perturbation by a circumbinary object due to the Applegate's mechanism fails to explain such a large period oscillation. The mass of the potential third body is calculated as M3sin i′ = 0.011(±0.003)Mo. Supposing the circumbinary companion and the eclipsing binary is coplanar, its mass would correspond to a giant planet. This hypothetical giant planet is moving in a circular orbit of radius ∼ 5.75(±2.02) AU around its host star. Copyright © 2018, The Authors. All rights reserved.

关键词： Gravitation

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TY Pup: a low-mass-ratio and deep contact binary as a progenitor candidate of luminous red novae

arXiv

引用

arXiv 2018年

作者： Sarotsakulchai, T. Qian, S.-B. Soonthornthum, B. Zhou, X. Zhang, J. Reichart, D.E. Haislip, J.B. Kouprianov, V.V. Poshyachinda, S. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Rd. Chaoyang District Beijing100012 China University of Chinese Academy of Sciences 19 A Yuquan Rd. Shijingshan Beijing100049 China National Astronomical Research Institute of Thailand Ministry of Science and Technology Bangkok Thailand Department of Physics and Astronomy University of North Carolina CB #3255 Chapel HillNC27599 United States

TY Pup is a well-known bright eclipsing binary with an orbital period of 0.8192 days. New light curves in B, V, (RI)C bands were obtained with the 0.61-m reflector robotic telescope (PROMPT-8) at CTIO in Chile during 2015 and 2017. By analysing those photometric data with the W-D method, it is found that TY Pup is a low-mass-ratio (q ∼ 0.184) and deep contact binary with a high fill-out factor (84.3 %). An investigation of all available times of minimum light including three new ones obtained with the 60-cm and the 1.0-m telescopes at Yunnan Observatories in China indicates that the period change of TY Pup is complex. An upward parabolic variation in the O − C diagram is detected to be superimposed on a cyclic oscillation. The upward parabolic change reveals a long-term continuous increase in the orbital period at a rate of dP/dt = 5.57(±0.08) × 10−8 d yr−1. The period increase can be explained by mass transfer from the less massive component (M2 ∼ 0.3M☉) to the more massive one (M1 ∼ 1.65M☉). The binary will be merging when it meets the criterion that the orbital angular momentum is less than 3 times the total spin angular momentum, i.e., Jorb rot. This suggests that the system will finally merge into a rapid-rotating single star and may produce a luminous red nova. The cyclic oscillation in the O − C diagram can be interpreted by the light-travel time effect (LITE) via the presence of a third body. Copyright © 2018, The Authors. All rights reserved.

关键词： Stars

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