检索结果-内蒙古大学图书馆

The Effect of Metallicity on the Dynamical evolution of A Globular Cluster

Chinese Astronomy and Astrophysics 2015年第1期39卷 1-15页

作者： Zhuang, Yu-Long Zhang, Feng-Hui Yunnan Astronomical Observatory Chinese Academy of Sciences Kunming 650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 China University of Chinese Academy of Sciences Beijing 100049 China

The dynamical process and stellar evolution, as well as their mutual interaction will make important influences on the evolution of a globular cluster. As the matallicity may affect the track of stellar evolution, the associated variation of stellar mass loss rate will make influence on the dynamical process of the globular cluster as well. A series of N-body simulations are performed to study the effects of matallicity on the mass loss rate and radius of a globular cluster, and the reasons are analyzed. At the same time, the effects of large-mass stars and the cluster's initial number density distribution are also studied. In the simulations, the adopted initial number of member stars in the globular cluster model is N =50000, they move in the Galaxy-like gravitational potential, and their evolutions are also taken into consideration. The results indicate that because the low-matallicity stars have a faster evolutionary timescale, so in the early period the metal-poor globular cluster will have a higher mass loss, but at the same time its core collapse will be obviously delayed in time, hence after the core collapse its mass loss will be overtaken by the metal-rich globular cluster. In addition, as the evolution of large-mass star causes a larger mass loss, hence the existence of large-mass stars will make the matallicity even significantly influence on the early period expansion of the globular cluster, and the succeeding process of core collapse, besides, the influence of the cluster's initial number density distribution is also not negligible. © 2015.

关键词： evolution-methods General-stars Globular clusters Numerical

来源：评论

学校读者我要写书评

暂无评论

The Double Blue Straggler Sequence in NGC 2173: A Field Contamination Artifact?

引用

Research Notes of the AAS 2018年第4期2卷

作者： Chengyuan Li Licai Deng Richard de Grijs Dengkai Jiang Yu Xin Department of Physics and Astronomy Macquarie University Balaclava Road Sydney NSW 2109 Australia Department of Astronomy China West Normal University Nanchong 637002 People's Republic of China School of Astronomy and Space Science University of the Chinese Academy of Sciences 20A Datun Road Beijing 100012 People's Republic of China International Space Science Institute—Beijing 1 Nanertiao Zhongguancun Beijing 100190 People's Republic of China Yunnan Observatories Chinese Academy of Sciences Kunming 650216 People's Republic of China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650011 People's Republic of China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing 100012 People's Republic of China

来源：评论

学校读者我要写书评

暂无评论

Is BZB J1450+5201 the most distant gamma-ray BL Lacertae object?

引用

Research in Astronomy and Astrophysics 2015年第3期15卷 313-326页

作者： Neng-Hui Liao Jin-Ming Bai Jian-Guo Wang Hong-Tao Liu Jiu-Jia Zhang Ning Jiang Zun-Li Yuan Liang Chen Yunnan Observatories Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences University of Chinese Academy of Sciences Key Laboratory for Research in Galaxies and Cosmology University of Science and Technology of China Chinese Academy of Sciences Department of Astronomy University of Science and Technology of China Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical ObservatoryChinese Academy of Sciences

BL Lacertae （BL Lac） objects at high redshifts （z ≥ 2） are rarely detected. Through careful analysis of its Sloan Digital Sky Survey spectrum, BZB J1450＋5201 is confirmed to be a high-z BL Lac object with z ≥ 2.471 by identifying the Lyα 1216 and CIV 1548/1550 absorption lines. This indicates that BZB J1450＋5201 is the most distant BL Lac object discovered to date. Careful analysis of the five-year Fermi-LAT data of 2FGL J1451.0＋5159 shows that its γ-ray emission is robust with a confidence level of 6.2σ at 1-3 GeV and 6.7σ at 3-10 GeV. This analysis with the five-year data overcomes confusion with its bright neighbor, which is a problem when analyzing the two-year data. In addition, 2FGL J 1451.0＋5159 is confirmed to be associated with BZB J1450＋5201 using the five-year data. The analysis of multiwavelength data, from radio to γ-ray energies, indicates that BZB J1450＋5201 is an intermediate synchrotron peaked （ISP） source. Its multiwavelength properties are consistent with distributions of other ISP sources at lower redshifts in the second Fermi-LAT AGN catalog. The pure synchrotron self-Compton （SSC） model seems to be disfavored, but the scattering of weak external emission plus the SSC process can provide a satisfactory description of the broadband emission.

关键词： galaxies active -- BL Lacertae objects individual （BZB J1450＋5201）-- gamma rays galaxies -- radiation mechanisms non-thermal

来源：评论

学校读者我要写书评

暂无评论

Alma observation of ngc5135: The circumnuclear co(6-5) and dust continuum emission at 45 parsec resolution

arXiv

引用

arXiv 2018年

作者： Cao, Tianwen Lu, Nanyao Xu, C. Kevin Zhao, Yinghe Kalari, Venu Madhav Gao, Yu Charmandaris, Vassilis Santos, Tanio Diaz Van Der Werf, Paul Cao, Chen Wu, Hong Inami, Hanae Evans, Aaron Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China 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 Beijing100049 China Instituto de Astrofisica Pontificia Universidad Católica de Chile Av.Vicuña Mackenna 4860 Macul Santiago7820436 Chile Yunnan Observatories Chinese Academy of Sciences Kunming650011 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 Departamento de Astronoma Universidad de Chile Casilla 36-D Correo Central Santiago Chile Purple Mountain Observatory Key Lab of Radio Astronomy 8 YuanHua Road Nanjing210034 China Department of Physics University of Crete HeraklionGR-71003 Greece IAASARS National Observatory of Athens Pen-teliGR-15236 Greece Ncleo de Astronoma de la Facultad DeIngeniera Universidad Diego Portales Av. Ejercito Libertador 441 Santiago Chile Leiden Observatory Leiden University P.O. Box 9513 RA Leiden2300 Netherlands School of Space Science and Physics Shandong University Weihai Shandong264209 China Shandong Provincial Key Laboratory of Optical Astronomy Solar-Terrestrial Environment Weihai Shandong264209 China UMR 5574 Saint-Genis-Laval69230 France Department of Astronomy University of Virginia CharlottesvilleVA22903-2325 United States National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903-2475 United States

We present high-resolution (0.17'' × 0.14'') Atacama Large Millimeter/submillimeter Array (ALMA) observations of the CO(6{5) line, and 435 μm dust continuum emission within a ∼9"× 9" area centered on the nucleus of the galaxy NGC5135. NGC5135 is a well-studied luminous infrared galaxy that also harbors a Compton-thick active galactic nucleus (AGN). At the achieved resolution of 48 × 40 pc, the CO(6{5) and dust emissions are resolved into gas 'clumps" along the symmetrical dust lanes associated with the inner stellar bar. The clumps have radii between ∼45-180 pc and CO(6-5) line widths of ∼60-88 km s-1. The CO(6-5) to dust continuum ux ratios vary among the clumps and show an increasing trend with the [Fe ii]/Br-γ ratios, which we interpret as evidence for supernovadriven shocked gas providing a significant contribution to the CO(6-5) emission. The central AGN is undetected in continuum, nor in CO (6-5) if its line velocity width is no less than ∼40 km s-1. We estimate that the AGN contributes at most 1% of the integrated CO(6-5) flux of 512 ± 24 Jykm s-1within the ALMA field of view, which in turn accounts for ∼32% of the CO(6-5) flux of the whole galaxy. 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

Discovery of 16 New z ∼ 5.5 Quasars: Filling In The Redshift Gap of Quasar Color Selection

arXiv

引用

arXiv 2017年

作者： Yang, Jinyi Fan, Xiaohui Wu, Xue-Bing Wang, Feige Bian, Fuyan Yang, Qian McGreer, Ian D. Yi, Weimin Jiang, Linhua Green, Richard Yue, Minghao Wang, Shu Li, Zefeng Ding, Jiani Dye, Simon Lawrence, Andy Department of Astronomy School of Physics Peking University Beijing100871 China Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721 United States Research School of Astronomy and Astrophysics Australian National University Weston CreekACT2611 Australia Yunnan Observatories Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China School of Physics and Astronomy Nottingham University University Park NottinghamNG7 2RD United Kingdom Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom

We present initial results from the first systematic survey of luminous z ∼ 5.5 quasars. Quasars at z ∼ 5.5, the post-reionization epoch, are crucial tools to explore the evolution of intergalactic medium, quasar evolution and the early super-massive black hole growth. However, it has been very challenging to select quasars at redshifts 5.3 ≤ z ≤ 5.7 using conventional color selections, due to their similar optical colors to late-type stars, especially M dwarfs, resulting in a glaring redshift gap in quasar redshift distributions. We develop a new selection technique for z ∼ 5.5 quasars based on optical, near-IR and mid-IR photometric data from Sloan Digital Sky Survey (SDSS), UKIRT InfraRed Deep Sky Surveys - Large Area Survey (ULAS), VISTA Hemisphere Survey (VHS) and Wide field Infrared Survey Explorer (WISE). From our pilot observations in SDSS-ULAS/VHS area, we have discovered 15 new quasars at 5.3 ≤ z ≤ 5.7 and 6 new lower redshift quasars, with SDSS z band magnitude brighter than 20.5. Including other two z ∼ 5.5 quasars already published in our previous work, we now construct an uniform quasar sample at 5.3 ≤ z ≤ 5.7 with 17 quasars in a ∼ 4800 square degree survey area. For further application in a larger survey area, we apply our selection pipeline to do a test selection by using the new wide field J band photometric data from a preliminary version of the UKIRT Hemisphere Survey (UHS). We successfully discover the first UHS selected z ∼ 5.5 quasar. Subject headings: galaxies: active - galaxies:high-redshift - quasars: general - quasars: emission lines Copyright © 2017, 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

Warm molecular hydrogen in nearby, luminous infrared galaxies

arXiv

引用

arXiv 2018年

作者： Petric, Andreea O. Armus, Lee Flagey, Nicolas Guillard, Pierre Howell, Justin Inami, Hanae Charmandaris, Vassillis Evans, Aaron Stierwalt, Sabrina Diaz-Santos, Tanio Lu, Nanyao Spoon, Henrik Mazzarella, Joe Appleton, Phil Chan, Ben Chu, Jason Hand, Derek Privon, George Sanders, David Surace, Jason Xu, Kevin Zhao, Yinghe Institute for Astronomy 2680 Woodlawn Drive HonoluluHI96822 United States Canada-France-Hawaii Telescope 65-1238 Mamalahoa Highway KamuelaHI96743 United States Infrared Processing & Analysis Center California Institute of Technology MS 100-22 PasadenaCA91125 United States Institut d'Astrophysique de Paris 96 bis boulevard Arago Paris75014 France Universite de Lyon 92 Rue Pasteur Lyon69007 France Department of Physics University of Crete HeraklionGR-71003 Greece IAASARS National Observatory of Athens PenteliGR-15236 Greece Department of Astronomy University of Virginia CharlottesvilleVA22903 United States National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States Nucleo de Astronomia de la Facultad de Ingenieria Universitad Diego Portales Av. Ejercito Libertador 441 Santiago Chile Beijing100012 China China-Chile Joint Center for Astronomy Camino El Observatorio 1515 Las Condes Santiago Chile Department of Astronomy Cornell University 616A Space Science Building IthacaNY14853 United States Department of Physics and Astronomy University of Hawaii 200 W. Kawili St. HiloHI96720 United States Instituto de Astrofisica Facultad de Fisica Pontificia Universitad Catolica de Chile Casilla 306 Santiago22 Chile Yunnan Observatories CAS Kumming65011 China Key Laboratory for the Structure and Evolution of Celestial Objects CAS Kumming65011 China Purple Mountain Observatory CAS Nanjing210008 China

Mid-infrared molecular hydrogen (H2) emission is a powerful cooling agent in galaxy mergers and in radio galaxies;it is a potential key tracer of gas evolution and energy dissipation associated with mergers, star formation, and accretion onto supermassive black holes. We detect mid-IR H2line emission in at least one rotational transition in 91% of the 214 Luminous Infrared Galaxies (LIRGs) observed with Spitzer as part of the Great Observatories All-sky LIRG Survey (GOALS). We use H2excitation diagrams to estimate the range of masses and temperatures of warm molecular gas in these galaxies. We find that LIRGs in which the IR emission originates mostly from the Active Galactic Nuclei (AGN) have about 100K higher H2mass-averaged excitation temperatures than LIRGs in which the IR emission originates mostly from star formation. Between 10 and 15% of LIRGs have H2emission lines that are sufficiently broad to be resolved or partially resolved by the high resolution modules of Spitzer's Infrared Spectrograph (IRS). Those sources tend to be mergers and contain AGN. This suggests that a significant fraction of the H2line emission is powered by AGN activity through X-rays, cosmic rays, and turbulence. We find a statistically significant correlation between the kinetic energy in the H2gas and the H2to IR luminosity ratio. The sources with the largest warm gas kinetic energies are mergers. We speculate that mergers increase the production of bulk in-flows leading to observable broad H2profiles and possibly denser environments. 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 nearby evolved stars survey: I. JCMT/SCUBA-2 Sub-millimetre detection of the detached shell of U Antliae

arXiv

引用

arXiv 2019年

作者： Dharmawardena, Thavisha E. Kemper, Francisca Srinivasan, Sundar Scicluna, Peter Marshall, Jonathan P. Wouterloot, Jan G.A. Greaves, Jane Goldman, Steven R. van Loon, Jacco Th. Matsuura, Mikako McDonald, Iain He, Jinhua Zijlstra, Albert A. Toalá, Jesús A. Wallström, Sofia H.J. Kim, Hyosun Trejo, Alfonso Ventura, Paolo Lagadec, Eric Boyer, Martha L. Liu, Tie Rau, Gioia Izumiura, Hideyuki Cami, Jan Holland, Wayne Jones, Olivia Shinnaga, Hiroko Academia Sinica Institute of Astronomy and Astrophysics 11F of AS/NTU Astronomy-Mathematics Building No.1 Sec. 4 Roosevelt Rd Taipei10617 Taiwan Graduate Institute of Astronomy National Central University 300 Zhongda Road Zhongli Taoyuan32001 Taiwan European Southern Observatory Karl-Schwarzschild-Str. 2 Garching b. München85748 Germany Instituto de Radioastronomía y Astrofísica Universidad Nacional Autónoma de México Antigua Carretera a Pátzcuaro # 8701 Ex-Hda. San José de la Huerta MoreliaMichoacánC.P. 58089 Mexico East Asian Observatory 660 N A’ohoku Place HiloHI96720 United States School of Physics and Astronomy Cardiff University 4 The Parade CardiffCF24 3AA United Kingdom STScI 3700 San Martin Drive BaltimoreMD21218 United States Lennard-Jones Laboratories Keele University ST5 5BG United Kingdom Jodrell Bank Centre for Astrophysics Alan Turing Building University of Manchester ManchesterM13 9PL United Kingdom Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Chinese Academy of Sciences South America Center for Astronomy China-Chile Joint Center for Astronomy Camino El Observatorio #1515 Las Condes Santiago Chile Departamento de Astronomía Universidad de Chile Casilla 36-D Santiago Chile Laboratory for Space Research University of Hong Kong Pokfulam Road Hong Kong Institute of Astronomy KU Leuven Celestijnenlaan 200D bus 2401 Leuven3001 Belgium Korea Astronomy and Space Science Institute 776 Daedukdae-ro Yuseong-gu Daejeon34055 Korea Republic of INAF Osservatorio Astronomico di Roma Via Frascati 33 Monte Porzio Catone Roma00077 Italy Université Côte d’Azur Observatoire de la Côte d’Azur CNRS Lagrange France NASA/GSFC Code 667 Goddard Space Flight Center GreenbeltMD20071 United States CRESST II Department of Physics Catholic University of America WashingtonDC20064 United States Okayama Branch

We present the highest resolution single-dish submillimetre observations of the detached shell source U Antliae to date. The observations were obtained at 450 µm and 850 µm with SCUBA-2 instrument on the James Clerk Maxwell Telescope as part of the Nearby Evolved Stars Survey. The emission at 850 µm peaks at 4000 with hints of a second peak seen at ∼ 2000. The emission can be traced out to a radius of 5600 at a 3σ level. The outer peak observed at 850 µm aligns well with the peak observed at Herschel/PACS wavelengths. With the help of spectral energy distribution fitting and radiative transfer calculations of multiple-shell models for the circumstellar envelope, we explore the various shell structures and the variation of grain sizes along the in the circumstellar envelope. We determine a total shell dust mass of (2.0±0.3)×10−5 M☉ and established that the thermal pulse which gave rise to the detached shell occurred 3500 ± 500 years ago. Copyright © 2019, The Authors. All rights reserved.

关键词： Shells (structures)

来源：评论

学校读者我要写书评

暂无评论

The long-lived Type IIn SN 2015da: Infrared echoes and strong interaction within an extended massive shell

arXiv

引用

arXiv 2019年

作者： Tartaglia, L. Pastorello, A. Sollerman, J. Fransson, C. Mattila, S. Fraser, M. Taddia, F. Tomasella, L. Turatto, M. Morales-Garoffolo, A. Elias-Rosa, N. Lundqvist, P. Harmanen, J. Reynolds, T. Cappellaro, E. Barbarino, C. Nyholm, A. Kool, E. Ofek, E. Gao, X. Jin, Z. Tan, H. Sand, D.J. Ciabattari, F. Wang, X. Zhang, J. Huang, F. Li, W. Mo, J. Rui, L. Xiang, D. Zhang, T. Hosseinzadeh, G. Howell, D.A. McCully, C. Valenti, S. Benetti, S. Callis, E. Carracedo, A.S. Fremling, C. Kangas, T. Rubin, A. Somero, A. Terreran, G. Department of Astronomy and the Oskar Klein Centre Stockholm University AlbaNova Roslagstullsbacken 21 StockholmSE 114 21 Sweden INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy Tuorla Observatory Department of Physics and Astronomy FI 20014 University of Turku Finland School of Physics O’Brien Centre for Science North University College Dublin Belfield Dublin 4 Ireland Department of Applied Physics Universidad de Cádiz campus of Puerto Real Cádiz11510 Spain Campus UAB Camí de Can Magrans s/n Cerdanyola del Vallès Barcelona08193 Spain c/Gran Capità 2 – 4 Edif. Nexus 201 Barcelona08034 Spain Benoziyo Center for Astrophysics and the Helen Kimmel center for planetary science Weizmann Institute of Science Rehovot76100 Israel Xinjiang Astronomical Observatory 150 Science 1–Street Urumqi Xinjiang830011 China Xingming Observatory Mountain Nanshan Urumqi Xinjiang830011 China Graduate Institute of Astronomy National Central University 300 Zhongda Rd. Zhongli District Taoyuan City32001 Taiwan Department of Astronomy/Steward Observatory 933 North Cherry Avenue Rm. N204 TucsonAZ85721-0065 United States Osservatorio Astronomico di Monte Agliale Via Cune Motrone Borgo a Mozzano Lucca55023 Italy Physics Department and Tsinghua Center for Astrophysics Tsinghua University Beijing100084 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Department of Astronomy School of Physics and Astronomy Shanghai Jiaotong Univeristy Shanghai200240 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 Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138-1516 United States Las

We report the results of the first ∼ 4 years of spectroscopic and photometric monitoring of the Type IIn supernova SN 2015da (aka PSN J13522411+3941286, or iPTF16tu). The supernova exploded in the nearby spiral galaxy NGC 5337, in a relatively highly extinguished environment. SN 2015da shows prominent Balmer lines in emission with narrow components at all times and a slow rise to maximum. In addition, early observations performed by amateur astronomers give a very well–constrained explosion epoch. The observables are consistent with continuous interaction between the supernova ejecta and a dense and extended H–rich circumstellar medium. This is likely the mechanism powering the light curve, as confirmed by the analysis of the pseudo bolometric light curve, which gives a total radiated energy & 1051 erg. Modeling the light curve in the context of a supernova shock breakout through a dense circumstellar medium allowed us to infer the mass of the pre–existing gas to be > 8.2 M, with an extreme mass–loss rate for the progenitor star ' 0.4 − 0.8 M yr−1, suggesting that most of the circumstellar gas was produced during multiple eruptive events. Near– and mid–infrared observations reveal a flux excess in these domains, similar to those observed in SN 2010jl and other interacting transients, likely due to pre–existing radiatively–heated dust surrounding the supernova. By modeling the infrared excess, we infer a mass & 0.4 × 10−3 M for the dust. Copyright © 2019, 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

Long-term transit timing monitoring and homogenous study of WASP-32

引用

Research in Astronomy and Astrophysics 2015年第1期15卷 117-126页

作者： Lei-Lei Sun Sheng-Hong Gu Xiao-Bin Wang Andrew Collier Cameron Dong-Tao Cao Yi-Bo Wang Yue Xiang Ho-Keung Hui Chi-Tai Kwok Bill Yeung Kam-Cheung Leung Yunnan Observatories Chinese Academy of Sciences Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences University of Chinese Academy of Sciences School of Physics and Astronomy University of St Andrews North Haugh St Andrews Fife KY16 9SS UK Ho Koon Nature Education cum Astronomical Centre Hong Kong Astronomical Society

We report new photometric observations of the transiting exoplanetary system WASP-32 made by using CCD cameras at Yunnan Observatories and Ho Koon Nature Education cum Astronomical Centre, China from 2010 to 2012. Following our usual procedure, the observed data are corrected for systematic errors according to the coarse decorrelation and SYSREM algorithms so as to enhance the signal of the transit events. Combined with radial velocity data presented in the literature, our newly observed data and earlier photometric data in the literature are simultaneously analyzed to derive the physical parameters describing the system by employing the Markov chain Monte Carlo technique. The derived parameters are consistent with the result published in the original paper about WASP-32b, but the uncertainties of the new parameters are smaller than those in the original paper. Moreover, our modeling result supports a circular orbit for WASP-32b. Through the analysis of all available mid-transit times, we have refined the orbital period of WASP-32b; no evident transit timing variation is found in these transit events.

关键词： techniques： photometric transiting exoplanetary system individual： WASP-32

来源：评论

学校读者我要写书评

暂无评论

19 low mass hypervelocity star candidates from the first data release of the LAMOST survey

引用

Research in Astronomy and Astrophysics 2015年第8期15卷 1364-1377页

作者： Yin-Bi Li A-Li Luo Gang Zhao You-Jun Lu Peng Wei Bing Du Xiang Li Yong-Heng Zhao Zhan-Wen Han Bo Wang Yue Wu Yong Zhang Yong-Hui Hou Yue-Fei Wang Ming Yang Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China State Key Laboratory of High-end Server & Storage Technology Jinan 250510 China Key Laboratory for the Structure and Evolution of Celestial Objects Yunnan Observatories Chinese Academy of Sciences Kunming 650216 China Nanjing Institute of Astronomical Optics & Technology National Astronomical Observatories Chinese Academy of Sciences Nanjing 210042 China

Hypervelocity stars are believed to be ejected out from the Galactic center through dynamical interactions between（binary） stars and the central supermassive black hole（s）. In this paper, we report 19 low mass F/G/K type hypervelocity star candidates from over one million stars found in the first data release of the LAMOST regular survey. We determine the unbound probability for each candidate using a MonteCarlo simulation by assuming a non-Gaussian proper-motion error distribution, and Gaussian heliocentric distance and radial velocity error distributions. The simulation results show that all the candidates have unbound possibilities over 50% as expected,and one of them may even exceed escape velocity with over 90% probability. In addition, we compare the metallicities of our candidates with the metallicity distribution functions of the Galactic bulge, disk, halo and globular clusters, and conclude that the Galactic bulge or disk is likely the birth place for our candidates.

关键词： stars： low-mass—stars： kinematics and dynamics—Galaxy： abundances—stars： fundamental parameters—stars： distances

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：