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Driving factors behind multiple populations

Science China(Physics,Mechanics & astronomy) 2024年第5期67卷 172-181页

作者： Ruoyun Huang Baitian Tang Chengyuan Li Doug Geisler Mario Mateo Ying-Yi Song Holger Baumgardt Julio A.Carballo-Bello Yue Wang Jundan Nie Bruno Dias JoséG.Fernández-Trincado School of Physics and astronomy Sun Yat-sen UniversityZhuhai 519082China CSST Science Center for the Guangdong-Hong Kong-Macao Greater Bay Area Zhuhai 519082China departamento de astronomía Universidad de ConcepcionConcepcionChile Instituto de Investigación Multidisciplinario en Ciencia y Tecnología Universidad de La SerenaLa SerenaChile departamento de astronomía Facultad de CienciasUniversidad de La SerenaChile department of astronomy University of MichiganAnn Arbor 48109USA David A.Dunlap department of astronomy&Astrophysics University of TorontoToronto ON M5S 3H4Canada Dunlap Institute for astronomy&Astrophysics University of TorontoToronto ON M5S 3H4Canada School of Mathematics and Physics The University of QueenslandSt.Lucia QLD 4072Australia Instituto de Alta Investigación Universidad de TarapacáAricaChile CAS Key Laboratory of Optical astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China Instituto de Astrofísica Departamento de Ciencias FísicasFacultad de Ciencias ExactasUniversidad Andres BelloSantiagoChile Instituto de astronomía Universidad Católica del NorteAntofagastaChile

Star clusters were historically considered simple stellar populations,with all stars sharing the same age and initial chemical ***,the presence of chemical anomalies in globular clusters(GCs),called multiple stellar populations(MPs),has challenged star formation theories in dense *** studies show that mass,metallicity,and age are likely controlling parameters for the manifestation of *** the limit between clusters with/without MPs in physical parameter space is crucial to reveal the driving mechanism behind their *** this study,we look for MP signals in Whiting 1,which is traditionally considered a young *** the Magellan telescope,we obtained low-resolution spectra withinλλ=3850-5500?for eight giants of Whiting *** measured the C and N abundances from the CN and CH spectral indices.C and N abundances have variations comparable with their measurement errors(~0.1 dex),suggesting that MPs are absent from Whiting *** these findings with literature studies,we propose a limit in the metallicity *** compactness index parameter space,which relatively clearly separates star clusters with/without MPs(GCs/open clusters).This limit is physically *** a larger scale,the galactic environment determines cluster compactness and metallicity,leading to metal-rich,diffuse,old clusters formed ex *** proposed limit also impacts our understanding of the formation of the Sagittarius dwarf galaxy:star clusters formed after the first starburst(age≤8-10 Gyr).These clusters are simple stellar populations because the enriched galactic environment is no longer suitable for MP formation.

关键词： stellar galactic galaxy

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Can near-to-mid Infrared Spectral Energy Distribution Quantitatively Trace Protoplanetary Disk Evolution?

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Research in astronomy and Astrophysics 2024年第7期24卷 34-46页

作者： Mingchao Liu Jinhua He Zhen Guo Jixing Ge Yuping Tang Yunnan Observatories Chinese Academy of SciencesKunming 650216China Chinese Academy of Sciences South America Center for astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China University of Chinese Academy of Sciences Beijing 100049China departamento de astronomía Universidad de ChileLas Condes7591245 SantiagoChile Instituto de Física y astronomía Universidad de Valparaísoave.Gran Bretaña1111Casilla 5030ValparaísoChile Centre for Astrophysics Research University of HertfordshireHatfield AL109ABUK Millennium Institute of Astrophysics Nuncio Monseñor Sotero Sanz 100Of.104ProvidenciaSantiagoChile Xinjiang astronomical Observatory Chinese Academy of SciencesUrumqi 830011China Xinjiang Key Laboratory of Radio Astrophysics Urumqi 830011China Shanghai Key Lab for Astrophysics Shanghai Normal UniversityShanghai 200234China

Infrared(IR)spectral energy distribution(SED)is the major tracer of protoplanetary *** was recently proposed to use the near-to-mid IR(or K-24)SED slopeαdefined between 2 and 24μm as a potential quantitative tracer of disk *** critically examine the viability of this idea and confront it with additional statistics of IR luminosities and SED *** point out that,because the statistical properties of most of the complicated physical factors involved in disk evolution are still poorly understood in a quantitative sense,the only viable way is to assume them to be random so that an idealized“average disk”can be defined,which allows theαhistogram to trace its *** confirm that the statistics of the zeroth order(luminosity),first order(slopeα),and second order characteristics(concavity)of the observed K-24 SEDs indeed carry useful information upon the evolutionary processes of the“average disk”.We also stress that intrinsic diversities in K-24 SED shapes and luminosities are always large at the level of individual stars so that the application of the evolutionary path of the“average disk”to individual stars must be done with *** data of most curves in plots are provided on GitHub(Disk-age package https://***/starage/disk-age/).

关键词： stars formation-stars pre-main sequence-stars protostars-infrared stars-protoplanetary disks

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Palaeogeographic reconstruction of Minchin palaeolake system,South America: The influence of astronomical forcing

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Geoscience Frontiers 2014年第2期5卷 249-259页

作者： Andrea Sánchez-Saldías Richard A.Faria Universidad de la República Facultad de Ciencias Departamento de Astronomía Universidad de la República Facultad de Ciencias Laboratorio de Paleobiología

Current palaeoclimatic reconstructions for the R＆#237;o de la Plata region during the latest Pleistocene （30,000 e10,000 yr BP） propose dry conditions, with rainfall at the Last Glacial Maximum amounting to one-third of today＇s precipitation. despite the consequential low primary productivity inferred, an impressive megafauna existed in the area at that time. Here we explore the influence of the flooding from a huge extinct system of water bodies in the Andean Altiplano as a likely source for wet regimes that might have increased the primary productivity and, hence, the vast number of megaherbivores. The system was reconstructed using specifically combined software resources, including Insola, Global Mapper v13, Surfer and Matlab. Changes in water volume and area covered were related to climatic change, assessed through a model of astronomical forcing that describes the changes in insolation at the top of the at-mosphere in the last 50,000 yr BP. The model was validated by comparing its results with several proxies （CH4, CO2, D, 18O） from dated cores taken from the ice covering Antarctic lakes Vostok and EPICA Dome C. It is concluded that the Altiplano Lake system drained towards the southeast in the rainy seasons and that it must have been a major source of water for the Paran＆#225;-Plata Basin, consequently enhancing primary productivity within it.

关键词： Planetary science Climate science Quaternary Palaeoecology Megafauna Parana Basin

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The ALMA-QUARKS Survey.Ⅰ.Survey description and Data Reduction

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Research in astronomy and Astrophysics 2024年第2期24卷 104-124页

作者：刘训川 Tie Liu Lei Zhu Guido Garay Hong-Li Liu Paul Goldsmith Neal Evans Kee-Tae Kim Sheng-Yuan Liu Fengwei Xu Xing Lu Anandmayee Tej Xiaofeng Mai Leonardo Bronfman Shanghuo Li Diego Mardones Amelia Stutz Ken'ichi Tatematsu Ke Wang Qizhou Zhang Sheng-Li Qin Jianwen Zhou Qiuyi Luo Siju Zhang Yu Cheng Jinhua He Qilao Gu Ziyang Li Zhenying Zhang Suinan Zhang Anindya Saha Lokesh dewangan Patricio Sanhueza Zhiqiang Shen Shanghai astronomical Observatory Chinese Academy of SciencesShanghai 200030China Chinese Academy of Sciences South America Center for astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China departamento de astronomía Universidad de ChileLas Condes7591245 SantiagoChile School of Physics and astronomy Yunnan UniversityKunming 650091China Jet Propulsion Laboratory California Institute of Technology4800 Oak Grove DrivePasadena CA 91109USA department of astronomy The University of Texas at AustinTX 78712-1205USA Korea astronomy and Space Science Institute 776 Daedeokdae-roYuseong-guDaejeon 34055Republic of Korea Institute of astronomy and Astrophysics Academia SinicaRoosevelt RoadTaipei 10617China Kavli Institute for astronomy and Astrophysics Peking UniversityBeijing 100871China department of astronomy School of PhysicsPeking UniversityBeijing 100871China Indian Institute of Space Science and Technology Thiruvananthapuram 695547KeralaIndia Max Planck Institute for astronomy Königstuhl 17D-69117 HeidelbergGermany departamento de astronomía Universidad de ConcepciónCasilla 160-CConcepciónChile Nobeyama Radio Observatory National Astronomical Observatory of JapanNational Institutes of Natural Sciences462-2 NobeyamaMinamimakiMinamisakuNagano 384-1305Japan Center for Astrophysics∣Harvard&Smithsonian 60 Garden StreetCambridgeMA 02138USA Max-Planck-Institut für Radioastronomie Auf dem Hügel 69D-53125 BonnGermany School of astronomy and Space Sciences University of Chinese Academy of SciencesBeijing 100049China National astronomical Observatory of Japan 2-21-1 OsawaMitakaTokyo181-8588Japan Yunnan Observatories Chinese Academy of SciencesKunming 650216China Physical Research Laboratory NavrangpuraAhmedabad-380009India astronomical Science Program The Graduate University for Advanced StudiesSOKENDAI2-21-1 OsawaMitakaTokyo 181-8588Japan University of Science and Technology Korea(UST)217 Gajeong-roYuseong-guDaejeon 34113Republic o

This paper presents an overview of the QUARKS survey,which stands for Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures."The QUARKS survey is observing139 massive clumps covered by 156 pointings at Atacama Large Millimeter/submillimeter Array(ALMA)Band 6(λ~1.3 mm).In conjunction with data obtained from the ALMA-ATOMS survey at Band 3(λ~3 mm),QUARKS aims to carry out an unbiased statistical investigation of massive star formation process within protoclusters down to a scale of 1000 *** overview paper describes the observations and data reduction of the QUARKS survey,and gives a first look at an exemplar source,the mini-starburst Sgr B2(M).The wide-b and width(7.5 GHz)and high-angular-resolution(~0."3)observations of the QUARKS survey allow for the resolution of much more compact cores than those could be done by the ATOMS survey,and to detect previously unrevealed fainter filamentary *** spectral windows cover transitions of species including CO,SO,N_(2)D^(+),SiO,H_(30)α,H_(2)CO,CH_(3)CN,and many other complex organic molecules,tracing gas components with different temperatures and spatial *** aims to deepen our understanding of several scientific topics of massive star formation,such as the mass transport within protoclusters by(hub-)filamentary structures,the existence of massive starless cores,the physical and chemical properties of dense cores within protoclusters,and the feedback from already formed high-mass young protostars.

关键词： stars formation-stars kinematics and dynamics-ISM clouds-ISM molecules

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Scaling Symmetry and Integrable Spherical Hydrostatics

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Journal of Modern Physics 2013年第4期4卷 486-494页

作者： Sidney Bludman Dallas C. Kennedy departamento de astronomía Universidad de Chile Santiago Chile Natick USA

Any symmetry reduces a second-order differential equation to a first integral: variational symmetries of the action (exemplified by central field dynamics) lead to conservation laws, but symmetries of only the equations of motion (exemplified by scale-invariant hydrostatics) yield first-order non-conservation laws between invariants. We obtain these non- conservation laws by extending Noether’s Theorem to non-variational symmetries and present an innovative variational formulation of spherical adiabatic hydrostatics. For the scale-invariant case, this novel synthesis of group theory, hydrostatics, and astrophysics allows us to recover all the known properties of polytropes and define a core radius, inside which polytropes of index n share a common core mass density structure, and outside of which their envelopes differ. The Emden solutions (regular solutions of the Lane-Emden equation) are obtained, along with useful approximations. An appendix discusses the n = 3 polytrope in order to emphasize how the same mechanical structure allows different thermal structures in relativistic degenerate white dwarfs and zero age main sequence stars.

关键词： Lagrangian Mechanics Symmetry Hydrodynamics Astrophysics Stellar Structure

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The ALMA-QUARKS Survey.Ⅱ.The ACA 1.3 mm Continuum Source Catalog and the Assembly of dense Gas in Massive Star-Forming Clumps

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Research in astronomy and Astrophysics 2024年第6期24卷 119-139页

作者：许峰玮 Ke Wang Tie Liu Lei Zhu Guido Garay Xunchuan Liu Paul Goldsmith Qizhou Zhang Patricio Sanhueza Shengli Qin Jinhua He Mika Juvela Anandmayee Tej Hongli Liu Shanghuo Li Kaho Morii Siju Zhang Jianwen Zhou Amelia Stutz Neal JEvans Kee-Tae Kim Shengyuan Liu Diego Mardones Guangxing Li Leonardo Bronfman Ken’ichi Tatematsu Chang Won Lee Xing Lu Xiaofeng Mai Sihan Jiao James O.Chibueze Keyun Su Viktor L.Tóth Kavli Institute for astronomy and Astrophysics Peking UniversityBeijing 100871China department of astronomy School of PhysicsPeking UniversityBeijing 100871China Shanghai astronomical Observatory Chinese Academy of SciencesShanghai 200030China Chinese Academy of Sciences South America Center for astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China departamento de astronomía Universidad de ChileLas Condes7591245 SantiagoChile Jet Propulsion Laboratory California Institute of Technology4800 Oak Grove DrivePasadena CA 91109USA Center for Astrophysics|Harvard&Smithsonian 60 Garden StreetCambridgeMA 02138USA National astronomical Observatory of Japan National Institutes of Natural Sciences2-21-1 OsawaMitakaTokyo 181-8588Japan astronomical Science Program The Graduate University for Advanced StudiesSOKENDAI2-21-1 OsawaMitakaTokyo 181-8588Japan School of Physics and astronomy Yunnan UniversityKunming 650091China Yunnan Observatories Chinese Academy of SciencesKunming 650216China department of Physics University of HelsinkiPO Box 64FI-00014 HelsinkiFinland Indian Institute of Space Science and Technology Thiruvananthapuram 695547KeralaIndia Max Planck Institute for astronomy Königstuhl 17D-69117 HeidelbergGermany department of astronomy Graduate School of ScienceThe University of Tokyo7-3-1 HongoBunkyo-kuTokyo 113-0033Japan Max-Planck-Institut für Radioastronomie Auf dem Hügel 6953121 BonnGermany departamento de astronomâıa Universidad de ConcepcionCasilla 160-CConcepci onChile department of astronomy The University of Texas at AustinTexas 78712-1205USA Korea astronomy and Space Science Institute 776 Daedeokdae-roYuseong-guDaejeon 34055Republic of Korea Institute of astronomy and Astrophysics Academia SinicaRoosevelt RoadTaipei 10617TaiwanChina South-Western Institute for astronomy Research Yunnan UniversityKunming 650091China Korea astronomy and Space Science Institute 776 Daedeok-daeroYuseong-guDaejeon 34055Republic of

Leveraging the high resolution,sensitivity,and wide frequency coverage of the Atacama Large Millimeter/submillimeter Array(ALMA),the QUARKS survey,standing for“Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures”,is observing 139 massive starforming clumps at ALMA Band 6(λ~1.3 mm).This paper introduces the Atacama Compact Array(ACA)7 m data of the QUARKS survey,describing the ACA observations and data *** multiwavelength data,we provide the first edition of QUARKS atlas,offering insights into the multiscale and multiphase interstellar medium in high-mass star *** ACA 1.3 mm catalog includes 207 continuum sources that are called ACA *** gas kinetic temperatures are estimated using three formaldehyde transitions with a non-LTE radiation transfer model,and the mass and density are derived from a dust emission *** ACA sources are massive(16–84 percentile values of 6–160 M_(⊙)),gravity-dominated(M∝R^(1.1))fragments within massive clumps,with supersonic turbulence(M>1)and embedded star-forming *** find a linear correlation between the masses of the fragments and the massive clumps,with a ratio of 6%between the *** considering fragments as representative of dense gas,the ratio indicates a dense gas fraction(DGF)of 6%,although with a wide scatter ranging from 1%to 10%.If we consider the QUARKS massive clumps to be what is observed at various scales,then the size-independent DGF indicates a self-similar fragmentation or collapsing mode in protocluster *** the ACA data over four orders of magnitude of luminosity-to-mass ratio(L/M),we find that the DGF increases significantly with L/M,which indicates clump evolutionary *** observed a limited fragmentation at the subclump scale,which can be explained by a dynamic global collapse process.

关键词： stars:formation ISM:kinematics and dynamics ISM:clouds stars:protostars

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Hadronic spectra from deformed AdS backgrounds

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Chinese Physics C 2020年第6期44卷 109-122页

作者： Eduardo Folco Capossoli Miguel Angel Martín Contreras Danning Li Alfredo Vega Henrique Boschi-Filho Instituto de Física Universidade Federal do Rio de Janeiro21.941-972-Rio de Janeiro-RJ-Brazil departamento de Física/Mestrado Profissional em Práticas da Educação Básica(MPPEB) Colégio Pedro II20.921-903-Rio de Janeiro-RJ-Brazil Instituto de Física y astronomía Universidad de ValparaísoA.Gran Bretaña 1111ValparaísoChile department of Physics and Siyuan Laboratory Jinan UniversityGuangzhou 510632China

Because of the presence of modified warp factors in metric tensors,we use deformed AdS5 spaces to apply the AdS/CFT correspondence to calculate the spectra for even and odd glueballs,scalar and vector mesons,and baryons with different *** the glueball cases,we derive their Regge trajectories and compare them with those related to the pomeron and the *** the scalar and vector mesons,as well as baryons,the determined masses are compatible with the *** particular,for these hadrons we found Regge trajectories compatible with another holographic approach as well as with the hadronic spectroscopy,which present an universal Regge slope of approximately 1.1 GeV^2.

关键词： hadronic spectra AdS/QCD model Regge trajectories

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The Universe as a Graviton Condensate: The “Dark-Bright Conjecture”

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Journal of High Energy Physics, Gravitation and Cosmology 2017年第2期3卷 277-284页

作者： A. Sigal Facultad de Matemática Astronomía Física y Computación Universidad Nacional de Córdoba Ciudad Universitaria Córdoba Argentina departamento de Química Teórica y Computacional Facultad de Ciencias Químicas Universidad Nacional de Córdoba Ciudad Universitaria Córdoba Argentina

The idea of a homogeneous, isotropic and spatially flat universe brings with it some unresolved issues, such as the nature of dark matter and the “coincidence problem”, i.e. the same order of magnitude between matter and vacuum density at the present time. In order to better understand these problems, it has been recently presented a physical interpretation based on quantum corrections within the second order Friedmann equation, which assumes a quantum condensate composed of gravitons filling the universe. In this article we show that the above supposition is consistent with the picture of a holographic universe created from vacuum fluctuations. From five postulates based on principles of modern quantum cosmology, we propose a very simple conjecture that, while shedding light on the properties of dark matter and dark energy, is able to predict values for the cosmological parameters which are in great agreement with the most accurate data gathered in recent astronomical observations.

关键词： Gravitons Dark Energy Quantum Cosmology Holographic Principle

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delamination of southern Puna lithosphere revealed by body wave attenuation tomography

Delamination of southern Puna lithosphere revealed by body w...

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中国科学院地质与地球物理研究所2014年度（第14届）学术年会

作者： Xiaofeng Liang Eric Sandvol Suzanne Kay Benjamin Heit Xiaohui Yuan Patrick Mulcahy Chen Chen Larry Brown Diana Comte Patricia Alvarado Institute of Geology and Geophysics Chinese Academy of Sciences department of Geological Sciences University of Missouri department of Earth and Atmospheric Science Cornell University deutsches Geo Forschungs Zentrum AMTC-departamento de Geo fisica FCFMUniversidad de Chile departamento de Geo fisicay astronomía CONICETUniversidad Nacional de San Juan

The southern Puna Plateau has been proposed to result from a major Pliocene delamination event that has previously been inferred from geochemical, geological, and some preliminary geophysical *** seismic stations were deployed across the southern Puna Plateau in 2007–2009 by scientists from the U.S., Germany, Chile, and Argentina to test the delamination model for the region. The Puna passive seismic stations were located between 25 and 28°S. Using the seismic waveform data collected from the PUNA experiment, we employ attenuation tomography methods to resolve both compressional and shear quality factors(Qp and Qs, respectively) in the crust and uppermost mantle. The images clearly show a highQ Nazca slab subducting eastward beneath the Puna plateau and another highQ block with a westward dip beneath the Eastern Cordillera. We suggest that the latter is a piece of delaminated South American lithosphere. A signi ficant lowQ zone lies between the Nazca slab and the South American lithosphere and extends southward from the northern margin of the seismic array at 25°S before vanishing around 27.5°S. This lowQ zone extends farther west in the crust and uppermost mantle at the southern end of the seismic array. The lowQ zone reaches 00 km depth beneath the northern part of the array but only 0 km depth in the south. Lateral variations of the lowQzone re flect the possible mechanism conversion between mantle upwelling related to delamination and dehydration. The depth of the Nazca slab as de fined by Q images decreases from north to south beneath the plateau, which is consistent with the steepflat transition of the angle of the subducting slab as de fined by previous earthquake studies.

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development of a Low Cost Pulsed Laser deposition System for Thin Films Growth

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Modern Instrumentation 2012年第4期1卷 41-48页

作者： Marcos Iván Oliva Carlos Iván Zandalazini Juan Carlos Ferrero Hector Raúl Bertorello Centro Láser de Ciencias Moleculare Departamento de Fisicoquímica Facultad de Ciencias Químicas Universidad Nacional de Córdoba Ciudad Universitaria Córdoba Argentina Grupo de Ciencia de Materiales Facultad de Matemática Astronomía y Física Universidad Nacional de Córdoba Ciudad Universitaria Córdoba Argentina Instituto de Física Enrique Gaviola Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET) Córdoba Argentina

.Pulsed Laser deposition (PLD) is a powerful technique to grow thin films. Oxides, Magnetics and superconducting materials have been obtained by PLD and theirs properties are strongly dependent of deposition parameters. The construction of a simple and cheap PLD system that is suitable for growing various thin films, including magnetic materials, controlling some deposition parameters is presented. The design characteristics and construction are presented for each one of the devices that compose this PLD system. The equipment has the possibility of carrying out films deposition using up to five targets under controlled atmosphere and substrate temperature. The system also allows controlling the cool off sample time after growing up films at high temperatures. A wide range of relative speeds between target and substrate axial rotation can be externally controlled. With the configuration and the dimensions adopted in their construction, a PLD system of great experimental flexibility is achieved, at a very low cost regarding the commercial systems. To evaluate their performance and effectiveness, the deposition characteristics of a BaFe12O19 film on (0001) sapphire substrate is presented.

关键词： Pulsed Laser deposition Thin Film Multilayer

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