检索结果-内蒙古大学图书馆

arXiv 2017年

作者： Lu, Nanyao Zhao, Yinghe Díaz-Santos, Tanio Xu, C. Kevin Gao, Yu Armus, Lee Isaak, Kate G. Mazzarella, Joseph M. van der Werf, Paul P. Appleton, Philip N. Charmandaris, Vassilis Evans, Aaron S. Howell, Justin Iwasawa, Kazushi Leech, Jamie Lord, Steven Petric, Andreea O. Privon, George C. Sanders, David B. Schulz, Bernhard Surace, Jason A. Beijing100012 China South American Center for Astronomy CAS Camino El Observatorio 1515 Las Condes Santiago Chile Infrared Processing and Analysis Center California Institute of Technology MS 100-22 PasadenaCA91125 United States Yunnan Observatories CAS Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kunming650011 China Purple Mountain Observatory CAS Nanjing210008 China Nucleo de Astronomia de la Facultad de Ingenieria Universidad Diego Portales Av. Ejercito Libertador 441 Santiago Chile Spitzer Science Center California Institute of Technology MS 220-6 PasadenaCA91125 United States Keplerlaan 1 Noordwijk2201 AZ Netherlands Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands Department of Physics University of Crete HeraklionGR-71003 Greece IAASARS National Observatory of Athens PenteliGR-15236 Greece Department of Astronomy University of Virginia 530 McCormick Road CharlottesvilleVA22904 United States National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States Martí i Franqués 1 Barcelona08028 Spain ICREA Pg. Lluís Companys 23 Barcelona08010 Spain Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom SETI Institute 189 Bernardo Ave Suite 100 Mountain ViewCA94043 United States Gemini Observatory Northern Operations Center 670 N. Aohoku Place HiloHI96720 Departamento de Astronomía Universidad de Concepción Casilla 160-C Concepción Chile Pontificia Universidad Católica de Chile Instituto de Astrofisica Casilla 306 Santiago 22 Chile University of Hawaii Institute for Astronomy 2680 Woodlawn Drive HonoluluHI96822 United States

We describe a Herschel Space Observatory 194-671 µm spectroscopic survey of a sample of 121 local luminous infrared galaxies and report the fluxes of the CO J to J−1 rotational transitions for 4 ≤ J ≤ 13, the [N ii] 205 µm line, the [C i] lines at 609 and 370 µm, as well as additional and usually fainter lines. The CO spectral line energy distributions (SLEDs) presented here are consistent with our earlier work, which was based on a smaller sample, that calls for two distinct molecular gas components in general: (i) a cold component, which emits CO lines primarily at J 4 and likely represents the same gas phase traced by CO (1−0), and (ii) a warm component, which dominates over the mid-J regime (4 10. The flux ratios of the two [C i] lines imply modest excitation temperatures of 15 to 30 K;the [C i] 370 µm line scales more linearly in flux with CO (4−3) than with CO (7−6). These findings suggest that the [C i] emission is predominately associated with the gas component defined in (i) above. Our analysis of the stacked spectra in different far-infrared (FIR) color bins reveals an evolution of the SLED of the rotational transitions of H2O vapor as a function of the FIR color in a direction consistent with infrared photon pumping. Copyright © 2017, The Authors. All rights reserved.

关键词： Molecules

来源：评论

学校读者我要写书评

暂无评论

Substellar objects around the sdB eclipsing Binaries

引用

Journal of Physics: Conference Series 2016年第7期728卷

作者： Liying Zhu Shengbang Qian Wenping Liao Ergang Zhao Linjia Li Yunnan Observatories Chinese Academy of Sciences (CAS) P.O. Box 110 650011 Kunming P. R. China Key laboratory of the structure and evolution of celestial objects Chinese Academy of Sciences P.O. Box 110 650011 Kunming P. R. China University of the Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block 100049 Beijing P. R. China

The sdB-type eclipsing binary consists a very hot subdwarf B (sdB) type primary and a low mass secondary with short period. They are detached binaries and show very narrow eclipse profiles, which benefits the determination of the precise eclipse times. With the precise times of light minimum, we can detected small mass objects around them by analyzing the observed-calculated (O-C) curve based on the light time effect. For searching the substellar objects orbiting around the binaries, we have monitored sdB-type eclipsing binaries for decades. A group of brown dwarfs and planets have been detected since then. In the present paper, we focus on the target NSVS07826147, which may be another exoplanet host candidate among the group of the sdB-type eclipsing binaries.

关键词：

来源：评论

学校读者我要写书评

暂无评论

JINGLE, a JCMT legacy survey of dust and gas for galaxy evolution studies: I. Survey overview and first results

arXiv

引用

arXiv 2018年

作者： Saintonge, Amélie Wilson, Christine D. Xiao, Ting Lin, Lihwai Hwang, Ho Seong Tosaki, Tomoka Bureau, Martin Cigan, Phillip J. Clark, Christopher J.R. Clements, David L. de Looze, Ilse Dharmawardena, Thavisha Gao, Yang Gear, Walter K. Greenslade, Joshua Lamperti, Isabella Lee, Jong Chul Li, Cheng Michalowski, Michal J. Mok, Angus Pan, Hsi-An Sansom, Anne E. Sargent, Mark Smith, Matthew W.L. Williams, Thomas Yang, Chentao Zhu, Ming Accurso, Gioacchino Barmby, Pauline Bourne, Nathan Brinks, Elias Brown, Toby Chung, Aeree Chung, Eun Jung Cibinel, Anna Coppin, Kristen Davies, Jonathan Davis, Timothy A. Eales, Steve Fanciullo, Lapo Fang, Taotao Gao, Yu Glass, David H.W. Gomez, Haley L. Greve, Thomas He, Jinhua Ho, Luis C. Huang, Feng Jeong, Hyunjin Jiang, Xuejian Jiao, Qian Kemper, Francisca Kim, Ji Hoon Kim, Minjin Kim, Taehyun Ko, Jongwan Kong, Xu Lacaille, Kevin Lacey, Cedric G. Lee, Bumhyun Lee, Joon Hyeop Lee, Wing-Kit Masters, Karen Oh, Se-Heon Papadopoulos, Padelis Park, Changbom Park, Sung-Joon Parsons, Harriet Rowlands, Kate Scicluna, Peter Scudder, Jillian M. Sethuram, Ramya Serjeant, Stephen Shao, Yali Sheen, Yun-Kyeong Shi, Yong Shim, Hyunjin Smith, Connor M.A. Spekkens, Kristine Tsai, An-Li Urquhart, Sheona Verma, Aprajita Violino, Giulio Viti, Serena Wake, David Wang, Junfeng Wouterloot, Jan Yang, Yujin Yim, Kijeong Yuan, Fangting Zheng, Zheng Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Department of Physics and Astronomy McMaster University HamiltonONL8S 4M1 Canada Department of Physics Zhejiang University HangzhouZhejiang310027 China Institute of Astronomy and Astrophysics Academia Sinica P.O. Box 23-141 Taipei10617 Taiwan School of Physics Korea Institute for Advanced Study 85 Hoegiro Dongdaemun-gu Seoul02455 Korea Republic of Joetsu University of Education Yamayashiki-machi Joetsu Niigata943-8512 Japan Department of Physics Royal Military College of Canada PO Box 17000 Station Forces KingstonONK7K 7B4 Department of Astronomy Institute of Theoretical Physics and Astrophysics Xiamen University Xiamen361005 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210008 China Key Laboratory of Radio Astronomy Chinese Academy of Sciences Nanjing210008 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan observatories Chinese Academy of Sciences P.O. Box 110 KunmingYunnan Province650011 China Camino El Observatorio 1515 Las Condes Santiago Chile Departamento de Astronomia Universidad de Chile Casilla 36-D Santiago Chile National Astronomical Observatory of China 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for Research in Galaxies and Cosmology Department of Astronomy University of Science and Technology of China Hefei230026 China Sterrenkundig Observatorium Universiteit Gent Krijgslaan 281 S9 GentB9000 Belgium Subaru Telescope National Astronomical Observatory of Japan 650 North A’ohoku Place HiloHI96720 United States Department of Astronomy Yonsei University 50 Yonsei-ro Seodaemun-gu Seoul03722 Korea Republic of Korea Astronomy and Space Science Institute 776 Daedeokdae-ro Yuseong-gu Daejeon34055 Korea Republic of National Central University No. 300 Zhongda Rd. Zhongli District Taoyuan City32001 Taiwan Department of Physic

JINGLE is a new JCMT legacy survey designed to systematically study the cold interstellar medium of galaxies in the local Universe. As part of the survey we perform 850µm continuum measurements with SCUBA-2 for a representative sample of 193 Herschel-selected galaxies with M∗ > 109M , as well as integrated CO(2-1) line fluxes with RxA3m for a subset of 90 of these galaxies. The sample is selected from fields covered by the Herschel-ATLAS survey that are also targeted by the MaNGA optical integral-field spectroscopic survey. The new JCMT observations combined with the multi-wavelength ancillary data will allow for the robust characterization of the properties of dust in the nearby Universe, and the benchmarking of scaling relations between dust, gas, and global galaxy properties. In this paper we give an overview of the survey objectives and details about the sample selection and JCMT observations, present a consistent 30 band UV-to-FIR photometric catalog with derived properties, and introduce the JINGLE Main Data Release (MDR). Science highlights include the non-linearity of the relation between 850µm luminosity and CO line luminosity (log LCO(2−1) = 1.372 log L850-1.376), and the serendipitous discovery of candidate z > 6 galaxies. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

来源：评论

学校读者我要写书评

暂无评论

The white dwarf binary pathways survey - II. Radial velocities of 1453 FGK stars with white dwarf companions from LAMOST DR 4

arXiv

引用

arXiv 2017年

作者： Rebassa-Mansergas, A. Ren, J.J. Irawati, P. García-Berro, E. Parsons, S.G. Schreiber, M.R. Gänsicke, B.T. Rodríguez-Gil, P. Liu, X. Manser, C. Palomo-Nevado, S. Jiménez-Ibarra, F. Costero, R. Echevarría, J. Michel, R. Zorotovic, M. Hollands, M. Han, Z. Luo, A. Villaver, E. Kong, X. Departament de Física Universitat Politècnica de Catalunya c/Esteve Terrades 5 Castelldefels08860 Spain Institute for Space Studies of Catalonia c/Gran Capità 2–4 Edif. Nexus 201 Barcelona08034 Spain National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China National Astronomical Research Institute of Thailand 191 Siriphanich Building Huay Kaew Road Chiang Mai50200 Thailand Deparment of Physics & Astronomy University of Sheffield SheffieldS3 7RH United Kingdom Instituto de Física y Astronomía Universidad de Valparaíso Avenida Gran Bretaña 1111 Valparaíso Chile Millenium Nucleus"Protoplanetary Disks in ALMA Early Science" Universidad de Valparaíso Avenida Gran Bretaña 1111 Valparaíso Chile Department of Physics University of Warwick CoventryCV4 7AL United Kingdom Instituto de Astrofísica de Canarias c/ Vía Láctea s/n La Laguna TenerifeE-38205 Spain Universidad de La Laguna Departamento de Astrofísica La Laguna TenerifeE- 38206 Spain Department of Astronomy Peking University Beijing100871 China Instituto de Astronomía Universidad Nacional Autónoma de México Ciudad Universitaria 70-264 México D.F.C.P. 04510 Mexico Instituto de Astronomía Universidad Nacional Autónoma de México 877 Ensenada Baja CaliforniaC.P.22830 Mexico Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan observatories Chinese Academy of Sciences P.O. Box 110 KunmingYunnan Province650011 China Departamento de Física Teórica Universidad Autónoma de Madrid CantoblancoMadrid28049 Spain

We present the second paper of a series of publications aiming at obtaining a better understanding regarding the nature of type Ia supernovae (SN Ia) progenitors by studying a large sample of detached F, G and K main sequence stars in close orbits with white dwarf companions (i.e. WD+FGK binaries). We employ the LAMOST (Large Sky Area Multi-Object Fibre Spectroscopic Telescope) data release 4 spectroscopic data base together with GALEX (Galaxy evolution Explorer) ultraviolet fluxes to identify 1,549 WD+FGK binary candidates (1,057 of which are new), thus doubling the number of known sources. We measure the radial velocities of 1,453 of these binaries from the available LAMOST spectra and/or from spectra obtained by us at a wide variety of different telescopes around the globe. The analysis of the radial velocity data allows us to identify 24 systems displaying more than 3σ radial velocity variation that we classify as close binaries. We also discuss the fraction of close binaries among WD+FGK systems, which we find to be ∼10 per cent, and demonstrate that high-resolution spectroscopy is required to efficiently identify double-degenerate SN Ia progenitor candidates. Copyright © 2017, The Authors. All rights reserved.

关键词： Velocity

来源：评论

学校读者我要写书评

暂无评论

The MALATANG Survey: the Lgas − LIR correlation on sub-kiloparsec scale in six nearby star-forming galaxies as traced by HCN J = 4 → 3 and HCO+ J = 4 → 3

arXiv

引用

arXiv 2018年

作者： Tan, Qing-Hua Gao, Yu Zhang, Zhi-Yu Greve, Thomas R. Jiang, Xue-Jian Wilson, Christine D. Yang, Chen-Tao Bemis, Ashley Chung, Aeree Matsushita, Satoki Shi, Yong Ao, Yi-Ping Brinks, Elias Currie, Malcolm J. Davis, Timothy A. de Grijs, Richard Ho, Luis C. Imanishi, Masatoshi Kohno, Kotaro Lee, Bumhyun Parsons, Harriet Rawlings, Mark G. Rigopoulou, Dimitra Rosolowsky, Erik Bulger, Joanna Chen, Hao Chapman, Scott C. Eden, David Gear, Walter K. Gu, Qiu-Sheng He, Jin-Hua Jiao, Qian Liu, Dai-Zhong Liu, Li-Jie Li, Xiao-Hu Michalowski, Michal J. Nguyen-Luong, Quang Qiu, Jian-Jie Smith, Matthew W.L. Violino, Giulio Wang, Jian-Fa Wang, Jun-Feng Wang, Jun-Zhi Yeh, Sherry Zhao, Ying-He Zhu, Ming Purple Mountain Observatory Key Laboratory for Radio Astronomy Chinese Academy of Sciences 8 Yuanhua Road Nanjing210034 China Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom ESO Karl-Schwarzschild-Str.2 GarchingD-85748 Germany Department of Physics and Astronomy University College London Gower Street LondonWC1E6BT United Kingdom Department of Physics and Astronomy McMaster University HamiltonONL8S 4M1 Canada Institut d’Astrophysique Spatiale CNRS Univ. Paris-Sud Université Paris-Saclay Bât. 121 Orsay Cedex91405 France European Southern Observatory Alonso de Córdova 3107 Casilla 19001 Vitacura Santiago Chile Department of Astronomy Yonsei University 50 Yonsei-ro Seodaemun-gu Seoul03722 Korea Republic of Academia Sinica Institute of Astronomy and Astrophysics P.O. Box 23-141 Taipei10617 Taiwan School of Astronomy and Space Science Nanjing University Nanjing210093 China National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo181-8588 Japan Centre for Astrophysics Research University of Hertfordshire College Lane HatfieldAL10 9AB United Kingdom RAL Space Rutherford Appleton Laboratory Harwell Campus Didcot OxfordshireOX11 0QX United Kingdom School of Physics and Astronomy Cardiff University Queen’s Buildings The Parade CardiffCF24 3AA United Kingdom Kavli Institute for Astronomy & Astrophysics Department of Astronomy Peking University Yi He Yuan Lu 5 Hai Dian District Beijing100871 China Department of Physics and Astronomy Macquarie University Balaclava Road North RydeNSW2109 Australia International Space Science Institute–Beijing 1 Nanertiao Zhongguancun Hai Dian District Beijing100190 China Institute of Astronomy Graduate School of Science University of Tokyo Osawa Mitaka Tokyo181-0015 Japan Research Center for the Early Universe Graduate School of Science University of Tokyo 7-3-1 Hongo Bunkyo-ku Tokyo113-0033 Japan East Asian Obse

We present HCN J = 4 → 3 and HCO+ J = 4 → 3 maps of six nearby star-forming galaxies, NGC 253, NGC 1068, IC 342, M82, M83, and NGC 6946, obtained with the James Clerk Maxwell Telescope as part of the MALATANG survey. All galaxies were mapped in the central 2′ × 2′ region at 14′′ (FWHM) resolution (corresponding to linear scales of ∼ 0.2 − 1.0 kpc). The LIR − L′dense relation, where the dense gas is traced by the HCN J = 4 → 3 and the HCO+ J = 4 → 3 emission, measured in our sample of spatially-resolved galaxies is found to follow the linear correlation established globally in galaxies within the scatter. We find that the luminosity ratio, LIR/L′dense, shows systematic variations with LIR within individual spatially resolved galaxies, whereas the galaxy-integrated ratios vary little. A rising trend is also found between LIR/L′dense ratio and the warm-dust temperature gauged by the 70 µm/100 µm flux ratio. We find the luminosity ratios of IR/HCN(4-3) and IR/HCO+(4-3), which can be taken as a proxy for the efficiency of star formation in the dense molecular gas (SFEdense), appears to be nearly independent of the dense-gas fraction (fdense) for our sample of galaxies. The SFE of the total molecular gas (SFEmol) is found to increase substantially with fdense when combining our data with that on local (ultra)luminous infrared galaxies and high-z quasars. The mean L′HCN(4−3)/L′HCO+(4−3) line ratio measured for the six targeted galaxies is 0.9±0.6. No significant correlation is found for the L′HCN(4−3)/L′HCO+(4−3) ratio with the SFR as traced by LIR, nor with the warm-dust temperature, for the different populations of galaxies. Copyright © 2018, The Authors. All rights reserved.

关键词： Galaxies

来源：评论

学校读者我要写书评

暂无评论

A tale of two transients: GW170104 and GRB170105A

arXiv

引用

arXiv 2017年

作者： Bhalerao, V. Kasliwal, M.M. Bhattacharya, D. Corsi, A. Aarthy, E. Adams, S.M. Blagorodnova, N. Cantwell, T. Cenko, S.B. Fender, R. Frail, D. Itoh, R. Jencson, J. Kawai, N. Kong, A.K.H. Kupfer, T. Kutyrev, A. Mao, J. Mate, S. Mithun, N.P.S. Mooley, K. Perley, D.A. Perrott, Y.C. Quimby, R.M. Rao, A.R. Singer, L.P. Sharma, V. Titterington, D.J. Troja, E. Vadawale, S.V. Vibhute, A. Vedantham, H. Veilleux, S. Department of Physics Indian Institute of Technology Bombay Mumbai400076 India Cahill Center for Astronomy and Astrophysics California Institute of Technology PasadenaCA91125 United States Inter-University Centre for Astronomy and Astrophysics P. O. Bag 4 Ganeshkhind Pune411007 India Department of Physics and Astronomy Texas Tech University Box 1051 LubbockTX79409-1051 United States Physical Research Laboratory Ahmedabad India University of Manchester Alan Turing Building Oxford Road ManchesterM13 9PL United Kingdom Astrophysics Science Division NASA Goddard Space Flight Center 8800 Greenbelt Road GreenbeltMD20771 United States Joint Space-Science Institute University of Maryland College ParkMD20742 United States Centre for Astrophysical Surveys University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom National Radio Astronomy Observatory P.O. Box O SocorroNM87801 United States Department of Physics Tokyo Institute of Technology 2-12-1 Ookayama Meguro-ku Tokyo152-8551 Japan Institute of Astronomy Department of Physics National Tsing Hua University Hsinchu30013 Taiwan Astrophysics Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Department of Astronomy University of Maryland College ParkMD20742 United States Yunnan Observatories Chinese Academy of Sciences Kunming Yunnan Province650011 China Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Juliane Maries Vej 30 København Ø2100 Denmark Department of Astronomy San Diego State University Tata Institute of Fundamental Research Homi Bhabha Road Mumbai India Astrophysics Group Cavendish Laboratory 19 J. J. Thomson Avenue CambridgeCB3 0HE United Kingdom Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Bei

We present multi-wavelength follow-up campaigns by the AstroSat-CZTI and GROWTH collaborations to search for an electromagnetic counterpart to the gravitational wave event GW170104. At the time of the GW170104 trigger, the AstroSat CZTI field-of-view covered 50.3% of the sky localization. We do not detect any hard X-ray (>100 keV) signal at this time, and place an upper limit of ≈ 4.5×10−7 erg cm−2 s−1 for a 1 s timescale. Separately, the ATLAS survey reported a rapidly fading optical source dubbed ATLAS17aeu in the error circle of GW170104. Our panchromatic investigation of ATLAS17aeu shows that it is the afterglow of an unrelated long, soft GRB 170105A, with only a fortuitous spatial coincidence with GW170104. We then discuss the properties of this transient in the context of standard long GRB afterglow models. Copyright © 2017, The Authors. All rights reserved.

关键词： Gravitational effects

来源：评论

学校读者我要写书评

暂无评论

Radio observations of the fine structure inside a post-CME current sheet

引用

Research in Astronomy and Astrophysics 2014年第7期14卷 843-854页

作者： Guan-Nan Gao Min Wang Jun Lin Ning Wu Cheng-Ming Tan Berhard Kliem Yang Su Yunnan Observatories Chinese Academy of Sciences University of Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences Key Laboratory of Solar Activity National Astronomical ObservatoriesChinese Academy of Sciences School of Tourism and Geography Yunnan Normal University Institute of Physics and Astronomy University of Potsdam IGAM-Kanzelhhe Observatory Institute of PhysicsUniversity of GrazUniversittsplatz 58010 GrazAustria

A solar radio burst was observed in a coronal mass ejection/flare event by the Solar Broadband Radio Spectrometer at the Huairou Solar Observing Station on2004 December 1. The data exhibited various patterns of plasma motions, suggestive of the interaction between sunward moving plasmoids and the flare loop system during the impulsive phase of the event. In addition to the radio data, the associated whitelight, Hα, extreme ultraviolet light, and soft and hard X-rays were also studied.

关键词： Sun： coronal mass ejections （CMEs）-- Sun： flares -- Sun： solar radio bursts -- Sun： magnetic reconnection

来源：评论

学校读者我要写书评

暂无评论

Characteristics of Double Gamma-Ray Bursts

引用

Chinese Physics Letters 2014年第11期31卷 163-165页

作者：刘彤孙谋远侯书进李昂张富文顾为民卢炬甫 Department of Astronomy and Institute of Theoretical Physics and Astrophysics Xiamen University Xiamen 361005 Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 State Key Laboratory of Theoretical Physics Institute of Theoretical Physics Chinese Academy of Sciences Beijing 100190 Department of Astronomy and Astrophysics and Institute for Gravitation and the Cosmos Pennsylvania State University University Park PA 16802 USA College of Physics and Electronic Engineering Nanyang Normal University Nanyang 473061 College of Science Guilin University of Technology Guilin 541004

Double gamma-ray bursts （DGRBs） have two well-separated sub-bursts in the main prompt emission and the typical time interval between them is in the hundreds of seconds. Among DGRBs, gamma-ray bursts （DGRBs） 110801A and 120716A are the ones with known redshifts. However, unlike GRB 110801A, we show that the two sub-bursts of GRB 120716A is severally similar to the short- and long-duration GRBs, thus it is difficult to explain the origin of GRB 120716A by the popular models on the central engine of GRBs. We suggest that some mechanisms of x-ray flares in GRBs, i.e., a post-merger millisecond pulsars or the jet precession in a black hole hyperaccretion system may produce the DGRB.

关键词： GAMMA ray bursts RED shift X-rays LIGHT curves PHYSICS research

来源：评论

学校读者我要写书评

暂无评论

FIRST PHOTOMETRIC INVESTIGATION of the SOLAR-TYPE CONTACT BINARY GSC 1537-1557

引用

Astronomical Journal 2015年第1期150卷

作者： Xiang, F.-Y. Xiao, T.-Y. Zhang, B. Shi, X.-D. Physics Department Xiangtan University Funan Province Xiangtan 411105 China Yunnan Observatories Chinese Academy of Sciences (CAS) P.O. Box 110 Kunming 650011 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P.O. Box 110 Kunming 650011 China University of the Chinese Academy of Sciences Yuquan Road 19# Beijing 100049 China

By analyzing Rc and Ic light curves of the short-period solar-type eclipsing binary GSC 1537-1557 we discovered that it is a shallow contact binary with a degree of contact factor of . Photometric solutions reveal tha... 详细信息

By analyzing R_c and I_c light curves of the short-period solar-type eclipsing binary GSC 1537-1557 we discovered that it is a shallow contact binary with a degree of contact factor of . Photometric solutions reveal that GSC 1537-1557 is a W-type system with a mass ratio of where the less massive component (the primary star) is about 110 K hotter than the more massive one (the secondary star). The asymmetry and variation of the light curves were explained as the activity of spots on the solar-type component stars. By investigating all of the available times of light minima, we found that the observed-calculated (O-C) curve shows a cyclic variation with a small amplitude of 0.00335 days and a period of 8.1 years. The small-amplitude cyclic change in the curve was analyzed for the light-travel time effect via the presence of an extremely cool stellar companion. The mass of the third body was determined to be when is adopted for GSC 1537-1557. The semimajor axis of the outer obit is AU. © 2015. The American Astronomical Society. All rights reserved..

关键词： accretion, accretion disks BL Lacertae objects: general galaxies: active galaxies: jets quasars: general

来源：评论

学校读者我要写书评

暂无评论

Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star

arXiv

引用

arXiv 2017年

作者： Arcavi, Iair Howell, D. Andrew Kasen, Daniel Bildsten, Lars Hosseinzadeh, Griffin McCully, Curtis Wong, Zheng Chuen Katz, Sarah Rebekah Gal-Yam, Avishay Sollerman, Jesper Taddia, Francesco Leloudas, Giorgos Fremling, Christoffer Nugent, Peter E. Horesh, Assaf Mooley, Kunal Rumsey, Clare Cenko, S. Bradley Graham, Melissa L. Perley, Daniel A. Nakar, Ehud Shaviv, Nir J. Bromberg, Omer Shen, Ken J. Ofek, Eran O. Cao, Yi Wang, Xiaofeng Huang, Fang Rui, Liming Zhang, Tianmeng Li, Wenxiong Li, Zhitong Zhang, Jujia Valenti, Stefano Guevel, David Shappee, Benjamin Kochanek, Christopher S. Holoien, Thomas W.-S. Filippenko, Alexei V. Fender, Rob Nyholm, Anders Yaron, Ofer Kasliwal, Mansi M. Sullivan, Mark Blagorodnova, Nadja Walters, Richard S. Lunnan, Ragnhild Khazov, Danny Andreoni, Igor Laher, Russ R. Konidaris, Nick Wozniak, Przemek Bue, Brian Las Cumbres Observatory GoletaCA93117 United States Kavli Institute for Theoretical Physics University of California Santa BarbaraCA93106 United States Department of Physics University of California Santa BarbaraCA93106 United States Nuclear Science Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Department of Physics University of California BerkeleyCA94720 United States Department of Astronomy University of California BerkeleyCA94720-3411 United States Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot76100 Israel The Oskar Klein Centre Department of Astronomy Stockholm University AlbaNova StockholmSE-10691 Sweden Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Juliane Maries vej 30 Copenhagen2100 Denmark Computational Research Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Racah Institute of Physics Hebrew University of Jerusalem Jerusalem91904 Israel Department of Physics Astrophysics University of Oxford Denys Wilkinson Building OxfordOX1 3RH United Kingdom Astrophysics Group Cavendish Laboratory 19 J. J. Thomson Avenue CambridgeCB3 0HE United Kingdom Astrophysics Science Division NASA Goddard Space Flight Center Code 661 GreenbeltMD20771 United States Joint Space-Science Institute University of Maryland College ParkMD20742 United States Department of Astronomy University of Washington Box 351580 U.W. SeattleWA98195-1580 United States Astrophysics Research Institute Liverpool John Moores University IC2 Liverpool Science Park 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Raymond and Beverly Sackler School of Physics and Astronomy Tel Aviv University Tel Aviv69978 Israel eScience Institute University of Washington Box 351570 U.W. SeattleWA98195-1580 United States Tsinghua University Beijing100084 China Key Laboratory of Optical Astronomy National Astronomical Observatories of China Chinese

Every supernova hitherto observed has been considered to be the terminal explosion of a star. Moreover, all supernovae with absorption lines in their spectra show those lines decreasing in velocity over time, as the ejecta expand and thin, revealing slower moving material that was previously hidden. In addition, every supernova that exhibits the absorption lines of hydrogen has one main light-curve peak, or a plateau in luminosity, lasting approximately 100 days before declining1. Here we report observations of iPTF14hls, an event that has spectra identical to a hydrogen-rich core-collapse supernova, but characteristics that differ extensively from those of known supernovae. The light curve has at least five peaks and remains bright for more than 600 days;the absorption lines show little to no decrease in velocity;and the radius of the line-forming region is more than an order of magnitude bigger than the radius of the photosphere derived from the continuum emission. These characteristics are consistent with a shell of several tens of solar masses ejected by the star at supernova-level energies a few hundred days before a terminal explosion. Another possible eruption was recorded at the same position in 1954. Multiple energetic pre-supernova eruptions are expected to occur in stars of 95–130 solar masses, which experience the pulsational pair instability2, 3, 4, 5. That model, however, does not account for the continued presence of hydrogen, or the energetics observed here. Another mechanism for the violent ejection of mass in massive stars may be required. Copyright © 2017, The Authors. All rights reserved.

关键词： Supernovae

来源：评论

学校读者我要写书评

暂无评论

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案：

请选择收藏分类：

通借通还

建议与咨询 留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

时间限定

文献类型

馆藏选择

核心期刊

语言

文献类型

帮助

文字说明：

检索规则说明：

检索范例：

分类表

所选分类

限定检索结果

文献类型

馆藏范围

日期分布

学科分类号

主题

机构

作者

语言

请选择保存的检索档案： 新增检索档案 确定 取消

请选择收藏分类： 新增自定义分类 确定 取消

通借通还

建议与咨询留下您的常用邮箱和电话号码，以便我们向您反馈解决方案和替代方法

请选择保存的检索档案：

请选择收藏分类：