09:50 10:30 Gail Zasowski: The Milky Way s Disks (Invited)
|
|
|
- Brook Melanie Davidson
- 5 years ago
- Views:
Transcription
1 Monday, Nov. 26, :45 09:00 Registration Session I: Observations of the Galactic Components 09:00 09:10 Welcome 09:10 09:50 Nils Ryde: The Milky Way s Bulge (Invited) 09:50 10:30 Gail Zasowski: The Milky Way s Disks (Invited) 10:30 10:50 Guillaume Guiglion: The AMBRE Project: r-process elements in the Milky Way thin and thick discs 10:50 11:20 Coffee Break 11:20 11:40 Diane Feuillet: Mapping the Age-metallicity relation with APOGEE and Gaia 11:40 12:00 Sven Buder: Chemodynamics with the GALAH survey 12:00 12:20 Avrajit Bandyopadhyay: First results from HESP-GOMPA (Galactic survey Of bright Metal Poor stars) survey 12:20 13:20 Lunch Break 13:20 14:00 Piercarlo Bonifacio: The metal-poor halo and CEMP stars (Invited) 14:00 14:20 Jonay I. González Hernández: Discovery of two new extremely ironpoor dwarf stars in the Galactic halo 14:20 14:40 Kim Venn: High Resolution Spectral Analyses of Metal-Poor Stars in the CFHT Pristine Survey 14:40 15:00 Charli Sakari: R-Process-Enhanced Metal-Poor Stars in the Milky Way Halo 15:00 15:20 John Donor: Updates from the Open Cluster Chemical Abundance and Mapping (OCCAM) survey 15:20 15:50 Coffee Break
2 15:50 16:30 David Yong: A review on globular clusters (Invited) 16:30 16:50 David M. Nataf: Clues to Chemical Evolution in Current and Former Globular Cluster Stars 17:10 17:30 Xudong Gao: Abundance trends in open clusters 17:30 17:50 Mikhail Kovalev: NLTE analysis of stellar clusters Tuesday, Nov. 27, Session II: Observations of dwarf spheroidal galaxies 09:00 09:40 Ása Skúladottír: Heavy elements in dwarf Speroidals (Invited) 09:40 10:00 Sten Hasselquist: APOGEE Chemical Abundances of the Large Magellanic Cloud 10:00 10:20 Jennifer Wojno: [Fe/H] and [α/fe] Abundance Measurements from the SPLASH Survey 10:20 10:40 Moritz Reichert: The role of neutron star merger in dwarf galaxies 11:10 11:50 Giuseppina Battaglia: Chemodynamics of dwarf Spheroidals (Invited) 11:50 12:10 Christian Hayes: The Chemical Abundance Profile of the Milky Way's Accreted Halo 12:10 12:30 Aldo Mura Guzman: Tracing the evolution of the Milky Way's stellar population(s) using fluorine Session III: Stellar Evolution 13:30 14:00 Raphael Hirschi: Stellar Evolution (Theory). (Invited) 14:00 14:30 Andreas Korn: Stellar Evolution (Observations) (Invited) 14:30 14:50 Ivan Cabrera-Ziri: Evidence for changes in He in stars with homogeneous CNO: challenging the role of the hot-cno cycle in the Hevariations in globular cluster stars 14:50 15:10 Raghubar Singh: Enhancement of Li in red giants 15:10 16:00 NON-conference, breakouts 16:00 16:30 Coffee Break Session IV: Nucleosynthesis
3 16:30 17:30 Almudena Arcones: Heavy elements formation in various formation sites (Invited) Wednesday, Nov. 28, Session V: Theory of the r-process, Neutron-Star Mergers 09:00 09:40 Stephane Goriely: Neutron star mergers and the robustness of the r- process(es) (Invited) 09:40 10:00 Shinya Wanajo: Nucleosynthesis in the ejecta of neutron star mergers and kilonovae 10:00 10:20 Oliver Just: Neutrino transport in models of neutron-star mergers and supernovae 10:20 10:40 Marius Eichler: Theoretical r-process sites and their signatures 11:10 11:30 Sho Fujibashi: Mass Ejection from Remnants of Binary Neutron Star Mergers 11:30 12:10 Thomas Janka: State-of-the-art supernova modeling (Invited) 12:10 12:30 Sabrina Gronow: Double detonations of sub-chandrasekhar mass white dwarfs 13:30 14:10 Kate Maguire: Observations of various types of Supernovae and how they affect GCE (Invited) 14:10 14:30 Anders Jerkstrand: Diagnosing the nucleosynthesis production of supernovae 14:30 15:10 Dan Maoz: Binary mergers, SNe Ia, and their role in GCE (Invited) 15:10 15:30 Gabriele Cescutti: Dwarf galaxies: a lab to investigate the neutron capture elements production 15:30 16:00 Coffee Break 16:00 16:20 Freeke van de Voort: Neutron capture elements in cosmological simulations of Milky Way-mass galaxies
4 16:20 16:40 Emanuele Spitoni: Galactic Archaeology with asteroseismic ages: the role of a delayed infall of gas in chemical evolution models 16:40 17:00 Derek Homeier: Atmospheres and Opacities of Cool Dwarf Stars 17:00 18:00 Poster Session 18:30 19:30 Conference Dinner 19:30 20:30 Falk Herwig: 3D1D hydro-nucleosynthesis simulations of convectivereactive nucleosynthesis for yields and galactic chemical evolution 20:30 21:30 ALL - Wrap-up Thursday, Nov. 29, Session VI: Galactic Chemical Evolution 09:00 09:40 Nikos Prantzos: GCE of heavy elements (Invited) 09:40 10:00 Benoit Coté: Neutron Star Mergers Might Not be the Only Source of r-process Elements in the Milky Way 10:00 10:20 Valeria Grisoni: Chemical evolution models for the Milky Way thick and thin discs 10:20 10:40 Jan Rybizki: GCE with Chempy: transforming stellar physics into abundances and vice versa 11:10 11:50 Pascale Jablonka: GCE of dwarf galaxies from a theoretical point of view (Invited) 11:50 12:10 Yutaka Hirai: Understanding the Enrichment of Heavy Elements by Galactic Chemo-Dynamical Evolution Models 12:10 13:10 Lunch Break 13:10 13:50 Karl-Friedrich Thielemann: Nucleosynthesis across the Galaxy (Invited) 13:50 14:10 Ralf Schönrich: Making the merger r-process possible in chemical evolution Session VII: Observational Surveys 14:10 14:30 R. Michael Rich: Abundance Trends in the bulge and Galactic Center: The view on the doorstep of large surveys 14:30 14:50 Michael Hanke: ATHOS - a cross survey tool for determining stellar parameters 14:50 15:10 Ditte Slumstrup: Systematic Differences in Spectroscopic Analysis
5 15:10 15:30 Bertrand Lemasle: Spectroscopic diagnostics for Cepheids as stellar tracers for Galactic chemical evolution 15:30 16:00 Coffee Break 16:00 16:20 Valeriy Vasilyev: Non-LTE oxygen line formation in 2D RHD simulations of cepheid atmospheres 16:20 16:40 Poster Talks 16:40 18:00 SOC reviews Friday, Nov. 30, :15 10:00 Maria Lugaro: The s-process and grains (Invited) 10:00 10:20 Ina Kristine Berentsen Kullmann: Nuclear impact on astronomical processes: a first experimental constraint on the s-process 191 Os(n,γ) branch-point reaction rate 10:20 10:40 Diego Vescovi: The major neutron source in Asymptotic Giant Branch stars 11:10 11:40 Richard Stancliffe: Stellar Evolution and CEMP stars (Invited) 11:40 12:10 Carlo Abate: Stellar Evolution and CEMP stars (Invited) 12:10 12:30 Jacqueline den Hartogh: S-process in rotating AGB stars 13:30 14:20 Sergio Cristallo: s-process from metal-poor AGB stars and the effect of rotation (Invited) 14:20 14:40 Carolyn Doherty: s- & i-process element production in rotating massive/super-agb stars 14:40 15:10 Coffee Break 15:10 15:40 Chiaki Kobayashi: Galactic chemical evolution of neutron capture elements 15:40 16:10 Georges Meynet: Angular momentum transport, chemical mixing and nucleosynthesis 16:10 17:00 Poster talks and final discussions
The Monash Chemical Yields Project
The Monash Chemical Yields Project Carolyn Doherty (Konkoly Observatory) George Angelou Simon W. Campbell Ross Church Thomas Constantino Sergio Cristallo Pilar Gil Pons Amanda Karakas John Lattanzio Maria
Chemo-dynamical disk modeling. Ivan Minchev Leibniz-Institut fur Astrophysik Potsdam (AIP)
Chemo-dynamical disk modeling Ivan Minchev Leibniz-Institut fur Astrophysik Potsdam (AIP) Talk outline Effect of disk asymmetries on disk dynamics. Radial migration in galactic disks. Chemo-dynamical disk
Chapter 19 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. Our Galaxy Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition Our Galaxy 19.1 The Milky Way Revealed What does our galaxy look like? How do stars orbit in our galaxy? Where are globular clusters located
Following the evolution of the Galactic disc with Open Clusters
Following the evolution of the Galactic disc with Open Clusters Laura Magrini INAF-Osservatorio Astrofisico di Arcetri With Nikos Prantzos and the GES collaboration (in particular Lorenzo Spina, Sofia
Stellar Populations in the Galaxy
Stellar Populations in the Galaxy Stars are fish in the sea of the galaxy, and like fish they often travel in schools. Star clusters are relatively small groupings, the true schools are stellar populations.
Chemical evolution of the Galactic disk using Open Clusters
Chemical evolution of the Galactic disk using Open Clusters ICC Winter Meeting Feb 2017 1. Galactic Archaeology Unravel the formation and evolution of the Milky Way (MW) Resolved stars provide a fossil
Learning Objectives: Chapter 13, Part 1: Lower Main Sequence Stars. AST 2010: Chapter 13. AST 2010 Descriptive Astronomy
Chapter 13, Part 1: Lower Main Sequence Stars Define red dwarf, and describe the internal dynamics and later evolution of these low-mass stars. Appreciate the time scale of late-stage stellar evolution
Basics of Galactic chemical evolution
Basics of Galactic chemical evolution The chemical abundances of stars provide important clues as to the evolutionary history of a galaxy. Astronomers usually refer to chemical elements other than hydrogen
Lecture 11: Ages and Metalicities from Observations A Quick Review
Lecture 11: Ages and Metalicities from Observations A Quick Review Ages from main-sequence turn-off stars Main sequence lifetime: lifetime = fuel / burning rate $ M " MS = 7 #10 9 % & M $ L " MS = 7 #10
The Pristine survey: An efficient search for extremely metal-poor stars. Kris Youakim. ING Seminar Jan 22, 2018
The Pristine survey: An efficient search for extremely metal-poor stars Kris Youakim ING Seminar Jan 22, 2018 Credit: NASA / WMAP Science Team Movie First Light Wise, Abel, Kaehler, 2009 Image: Aladin sky
Chemo-Dynamical evolution of dwarf spheroidal galaxies
11 th Russbach School on Nuclear Astrophysics Chemo-Dynamical evolution of dwarf spheroidal galaxies Yutaka Hirai! (The University of Tokyo, NAOJ)! Jun Hidaka (NAOJ), Takayuki R. Saitoh (Titech),! Michiko
The Apache Point Observatory Galactic Evolution Experiment. Ricardo Schiavon
The Apache Point Observatory Galactic Evolution Experiment Ricardo Schiavon CS20, Boston, August 1st, 2018 Overview paper: Majewski, Schiavon et al. (2017) APOGEE at a Glance Dual hemisphere spectroscopic
Uncertainties in Chemical Enrichment Models
Uncertainties in Chemical Enrichment Models CLUES Cas A M82 Benoit Côté (Christian Ritter, Falk Herwig, Brian O Shea) JINA Frontiers Meeting March 2015 Galactic Outflow M82 Abell 1689 Stripping and Disruption
Delayed Outflows from BH Accretion Tori Following Neutron Star Binary Coalescence. Brian Metzger
Delayed Outflows from BH Accretion Tori Following Neutron Star Binary Coalescence Brian Metzger (Columbia University) In Collaboration with Rodrigo Fernandez (IAS) Almudena Arcones, Gabriel Martinez-Pinedo
Lecture 11: Ages and Metalicities from Observations. A Quick Review. Multiple Ages of stars in Omega Cen. Star Formation History.
Ages from main-sequence turn-off stars Lecture 11: Main sequence lifetime: Ages and Metalicities from Observations R diagram lifetime = fuel / burning rate MV *1 M ' L ' MS = 7 10 9 ) ) M. ( L. ( A Quick
Chapter 15 The Milky Way Galaxy. The Milky Way
Chapter 15 The Milky Way Galaxy The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our
Chemical Evolution and the Mass Function of Stellar Mass Black Holes
.. and Neutron Stars Chemical Evolution and the Mass Function of Stellar Mass Black Holes Benoit Côté Postdoctoral Fellow Collaborators C. Fryer, K. Belczynski, B. O Shea, C. Ritter, F. Herwig, M. Pignatari,
Spectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg"
Spectroscopy of giants and supergiants! Maria Bergemann MPIA Heidelberg" Spectroscopy of (cool) giants and supergiants! Maria Bergemann MPIA Heidelberg" Outline! Motivation why do spectroscopy of giant
ASTR 101 Introduction to Astronomy: Stars & Galaxies
We observe star-gas-star cycle operating in Milky Way s disk using many different wavelengths of light! ASTR 101 Introduction to Astronomy: Stars & Galaxies Infrared light reveals stars whose visible light
Physics HW Set 3 Spring 2015
1) If the Sun were replaced by a one solar mass black hole 1) A) life here would be unchanged. B) we would still orbit it in a period of one year. C) all terrestrial planets would fall in immediately.
Daily agenda & scientific program
Daily agenda & scientific program Sunday June 22, 2014 Welcome reception 16h00-19h00 welcome and registration reception at the Science history museum Villa Bartholoni 128, route de Lausanne 1201 Genève
Enrichment of r-process elements in nearby dsph galaxies, the Milky way, and globular cluster(s)
Enrichment of r-process elements in nearby dsph galaxies, the Milky way, and globular cluster(s) Toshikazu Shigeyama (U. Tokyo) Based on Tsujimoto & TS 2014 Kilonova Afterglow of GRB130603B at day 9! Berger+
Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.
![Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.](/thumbs/94/121056697.jpg "Dust [12.1] Star clusters. Absorb and scatter light Effect strongest in blue, less in red, zero in radio.")
More abs. Dust [1.1] kev V Wavelength Optical Infra-red More abs. Wilms et al. 000, ApJ, 54, 914 No grains Grains from http://www.astro.princeton.edu/~draine/dust/dustmix.html See DraineH 003a, column
Asymptotic Giant Branch stars
Asymptotic Giant Branch stars Falk Herwig Los Alamos National Laboratory Theoretical Astrophysics Group LA Neutron Science Center Falk Herwig, May 8, 2006, 1 Introduction: AGB evolution NGC 6826 (Balick
AGB stars as laboratories for nuclear physics
AGB stars as laboratories for nuclear physics John Lattanzio with Amanda Karakas 1, Lisa Elliott, Simon Campbell, Maria Lugaro 2, Carolyn Doherty Centre for Stellar and Planetary Astrophysics, Monash University,Australia
ASTR 101 Introduction to Astronomy: Stars & Galaxies
ASTR 101 Introduction to Astronomy: Stars & Galaxies We observe star-gas-star cycle operating in Milky Way s disk using many different wavelengths of light Infrared light reveals stars whose visible light
Basics of chemical evolution
Basics of chemical evolution The chemical abundances of stars provide important clues as to the evolutionary history of a galaxy. H and He were present very early on in the Universe, while all metals (except
5:00pm-8:00pm Ala Moana, Carnation
210th Meeting of the AAS, joint meeting with SPD 27-31 May 2007 - Honolulu, HI Hawaii Convention Center, 1801 Kalakaua Ave., Honolulu, HI 96815 Thursday, May 24, 2007 Endpoints & Interactions: Physics
Nucleosynthesis in core-collapse supernovae. Almudena Arcones
Nucleosynthesis in core-collapse supernovae Almudena Arcones Nucleosynthesis in core-collapse supernovae Explosive nucleosynthesis: O, Mg, Si, S, Ca, Ti, Fe, p-process shock wave heats falling matter shock
Abundance Constraints on Early Chemical Evolution. Jim Truran
Abundance Constraints on Early Chemical Evolution Jim Truran Astronomy and Astrophysics Enrico Fermi Institute University of Chicago Argonne National Laboratory MLC Workshop Probing Early Structure with
THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS. B. Barbuy
THE GALACTIC BULGE AND ITS GLOBULAR CLUSTERS: MOS B. Barbuy IAG - Universidade de São Paulo Outline: Interest of studies on Galactic bulge and globulars Data available on metallicity,, kinematics in field
Galactic Projects at ESO Disk and halo. Birgitta Nordström Niels Bohr Institute Copenhagen University Denmark
Galactic Projects at ESO Disk and halo Birgitta Nordström Niels Bohr Institute Copenhagen University Denmark B. Nordstrom Prague 15 April 2014 1980: Milky Way Structure was Known - the formation and evolution
in the Milky NOW Way AND and THEN dwarf galaxies Stefania Salvadori
CARBON-ENHANCED DWARF GALAXIES: METAL-POOR STARS in the Milky NOW Way AND and THEN dwarf galaxies Stefania Salvadori University of Groningen Kapteyn Astronomical Institute Netherlands Organization for
The MonKey Project. An Update on Stellar Yields
The MonKey Project An Update on Stellar Yields Current State of the Art Yields The most boring part of stellar evolution? Or is it isochrone construction? Run lots of models and collect numbers Well its
Zoccali et al. 2003, A&A, 399, 931. Overview of (old) Galactic components. bulge, thick disk, metal-weak halo. metallicity & age distribution
Chap.3 The nature of Galactic components Overview of (old) Galactic components bulge, thick disk, metal-weak halo Globular clusters metallicity & age distribution Satellite galaxies spatial and metallicity
Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages
The Deaths of Stars 1 Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
The Deaths of Stars 1
The Deaths of Stars 1 Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
The HERMES project. Reconstructing Galaxy Formation. Ken Freeman RSAA, ANU. The metallicity distribution in the Milky Way discs Bologna May 2012
The HERMES project Reconstructing Galaxy Formation Ken Freeman RSAA, ANU The metallicity distribution in the Milky Way discs Bologna May 2012 HERMES is a new high-resolution fiber-fed multi-object spectrometer
Cat's Eye Nebula, APOD 4 Sep 02, Corradi & Goncalves. Falk Herwig:»Nuclear Astrophysics with Neutron Facilities«MSU - 14 Feb 05
Cat's Eye Nebula, APOD 4 Sep 02, Corradi & Goncalves Nuclear Astrophysics with Neutron Facilities Falk Herwig Los Alamos National Laboratory, New Mexico, USA Theoretical Astrophysics and Los Alamos Neutron
Stellar Evolution: The Deaths of Stars. Guiding Questions. Pathways of Stellar Evolution. Chapter Twenty-Two
Stellar Evolution: The Deaths of Stars Chapter Twenty-Two Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come
The Great Debate: The Size of the Universe (1920)
The Great Debate: The Size of the Universe (1920) Heber Curtis Our Galaxy is rather small, with Sun near the center. 30,000 LY diameter. Universe composed of many separate galaxies Spiral nebulae = island
STELLAR HEAVY ELEMENT ABUNDANCES AND THE NATURE OF THE R-PROCESSR. JOHN COWAN University of Oklahoma
STELLAR HEAVY ELEMENT ABUNDANCES AND THE NATURE OF THE R-PROCESSR JOHN COWAN University of Oklahoma First Stars & Evolution of the Early Universe (INT) - June 19, 2006 Top 11 Greatest Unanswered Questions
The Death of Stars. Today s Lecture: Post main-sequence (Chapter 13, pages ) How stars explode: supernovae! White dwarfs Neutron stars
The Death of Stars Today s Lecture: Post main-sequence (Chapter 13, pages 296-323) How stars explode: supernovae! White dwarfs Neutron stars White dwarfs Roughly the size of the Earth with the mass of
Star systems like our Milky Way. Galaxies
Galaxies Star systems like our Milky Way Galaxies Contain a few thousand to tens of billions of stars,as well as varying amounts of gas and dust Large variety of shapes and sizes Gas and Dust in
GALAXIES 626. The Milky Way II. Chemical evolution:
GALAXIES 626 The Milky Way II. Chemical evolution: Chemical evolution Observation of spiral and irregular galaxies show that the fraction of heavy elements varies with the fraction of the total mass which
Chemical Abundances in Globular Clusters
Australian National University E-mail: yong@mso.anu.edu.au The Milky Way globular clusters are ideal laboratories for testing the predictions of nuclear astrophysics. Driven by Hubble Space Telescope photometry
Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages
The Deaths of Stars Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
Stars and Stellar Astrophysics. Kim Venn U. Victoria
Stars and Stellar Astrophysics with ngcfht Kim Venn U. Victoria Stellar SWG: Katia Cunha (NOAO), Rolf-Peter Kudritzki (IfA), Else Starkenburg (U. Victoria) Patrick Dufour (U.Montreal) Zhanwen Han (Yunnan
Mixing, Nucleosynthesis, and Stellar Yields in Intermediate Mass AGB stars
Cat's Eye Nebula, APOD 4 Sep 02, Corradi & Goncalves Mixing, Nucleosynthesis, and Stellar Yields in Intermediate Mass AGB stars Falk Herwig Los Alamos National Laboratory, New Mexico, USA Theoretical Astrophysics
r-process enrichment traced by Pu and Ba near the sun and in the Draco
r-process enrichment traced by Pu and Ba near the sun and in the Draco Takuji Tsujimoto (Nat. Aston. Obs. Jap.) capturing electromagnetic waves earth archives stellar spectra meteorites deep-sea crusts
The chemical evolution of the Milky Way
The chemical evolution of the Milky Way Dipartimento di Fisica, Università di Trieste E-mail: matteucci@oats.inaf.it Emanuele Spitoni Dipartimento di Fisica, Università di Trieste E-mail: spitoni@oats.inaf.it
AGB Evolution and Nucleosynthesis at Low-Metallicity Constrained by the Star Formation History of Our Galaxy
AGB Evolution and Nucleosynthesis at Low-Metallicity Constrained by the Star Formation History of Our Galaxy National Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo, 181-8588, Japan E-mail: takuma.suda@nao.ac.jp
Chapter 4. Galactic Chemical Evolution. 4.1 Introduction. 4.2 Chemical Abundances
Chapter 4 Galactic Chemical Evolution 4.1 Introduction Chemical evolution is the term used for the changes in the abundances of the chemical elements in the Universe over time, since the earliest times
Stellar Evolution. Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars
Lecture 11 Stellar Evolution Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars A Spiral Galaxy (Milky Way Type) 120,000 ly A few hundred billion stars
Lithium abundances and metallicities: trends from metal-poor and AGB/RGB stars
Mem. S.A.It. Suppl. Vol. 22, 103 c SAIt 2012 Memorie della Supplementi Lithium abundances and metallicities: trends from metal-poor and AGB/RGB stars W. J. Maciel and R. D. D. Costa Astronomy Department
Metal Poor Stars: A Review for Non-Observers. Charli Sakari
Metal Poor Stars: A Review for Non-Observers Charli Sakari Outline Summary: What we know and have discussed already How should we interpret published stellar abundances? Martin Asplund et al.: NOT observed
PoS(NIC XII)193. Heavy elements in the early Galaxy. Terese Hansen University of Heidelberg, ZAH, LSW
University of Heidelberg, ZAH, LSW E-mail: thansen@lsw.uni-heidelberg.de Johannes Andersen Niels Bohr Institute, University of Copenhagen E-mail: ja@astro.ku.dk Birgitta Nordtrom Niels Bohr Institute,
Supernova Feedback in Low and High Mass Galaxies: Luke Hovey 10 December 2009
Supernova Feedback in Low and High Mass Galaxies: Luke Hovey 10 December 2009 Galactic Winds: Mathews, W. et al. 1971 Effects of Supernovae on the Early Evolution of Galaxies: Larson, R. 1974 The origin
Observations of s-process elements in stars. The Amazing Life of Stars: Celebrating ISTO A. Tornambè. Cefalú Sept 4-8, 2017
Observations of s-process elements in stars C. Abia The Amazing Life of Stars: Celebrating ISTO A. Tornambè. Cefalú Sept 4-8, 2017 Outline: 1. The s-process 2. Observational constraints from stars - intrinsic
20. Stellar Death. Interior of Old Low-Mass AGB Stars
20. Stellar Death Low-mass stars undergo three red-giant stages Dredge-ups bring material to the surface Low -mass stars die gently as planetary nebulae Low -mass stars end up as white dwarfs High-mass
Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008
Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008 Wed, July 16 MW galaxy, then review. Start with ECP3Ch14 2 through 8 Then Ch23 # 8 & Ch 19 # 27 & 28 Allowed Harlow Shapely to locate
Bridging the near and the far: constraints on first star formation from stellar archaeology. Raffaella Schneider Sapienza University of Rome
Bridging the near and the far: constraints on first star formation from stellar archaeology Raffaella Schneider Sapienza University of Rome Kyoto,First Stars IV 2012 Kyoto,First Stars IV 2012 "As we extend
Renegades in the Solar neighborhood
Title Renegades in the Solar neighborhood Ana Bonaca ITC Fellow Harvard University // Charlie Conroy // // Andrew Wetzel // Origin of the halo stars: In situ Eggen, Lynden-Bell & Sandage (1962) Accretion
Substructure in the Galaxy
Substructure in the Galaxy Amina Helmi Kapteyn Astronomical Institute Groningen, NL Is this how our Galaxy formed? Jeffrey Gardner Hierarchical paradigm Main characteristic of model: mergers Can we find
Review of the Bulge Stellar Population And Comparison to the Nuclear Bulge
Review of the Bulge Stellar Population And Comparison to the Nuclear Bulge David M. Nataf, Australian National University 22 July, 2016 IAU Symposium 322, 'The Multi- Messenger Astrophysics of the Galactic
Contents. List of Participants
Introduction List of Participants page xiii xiv 1 Mount Wilson Observatory contributions to the study of cosmic abundances of the chemical elements George W. Preston 1 References 7 2 Synthesis of the elements
15th High Energy Astrophysics Division Meeting Naples, Florida Sunday, 3 April :00 pm Registration, 3:00 pm 7:00 pm, Royal Palms Foyer Speaker
Sunday, 3 April 2016 3:00 pm Registration, 3:00 pm 7:00 pm, Royal Palms Foyer Speaker Ready, 3:00 pm 7:00 pm, Royal Palms 5 (back of room) 7:00 pm Opening Reception, 7:00 pm 8:30 pm, Vista Ballroom Monday,
Moment of beginning of space-time about 13.7 billion years ago. The time at which all the material and energy in the expanding Universe was coincident
Big Bang Moment of beginning of space-time about 13.7 billion years ago The time at which all the material and energy in the expanding Universe was coincident Only moment in the history of the Universe
Chemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia
Chemistry & Dynamics of the Milky Way From Before Hipparcos Until Gaia J. Andersen 1,2, B. Nordström 1,2 1 Dark Cosmology Centre, The Niels Bohr Institute, University of Copenhagen, Denmark 2 Stellar Astrophysics
The Origin of the Elements between Iron and the Actinides Probes for Red Giants and Supernovae
The Origin of the Elements between Iron and the Actinides Probes for Red Giants and Supernovae I Outline of scenarios for neutron capture nucleosynthesis (Red Giants, Supernovae) and implications for laboratory
Comparing a Supergiant to the Sun
The Lifetime of Stars Once a star has reached the main sequence stage of it life, it derives its energy from the fusion of hydrogen to helium Stars remain on the main sequence for a long time and most
29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A
29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A There are 20 questions (Note: There will be 32 on the real thing). Read each question and all of the choices before choosing.
Robert Izzard Université Libre de Bruxelles
Binary Star Populations: Keys to Understanding Stellar Astrophysics Robert Izzard Université Libre de Bruxelles with Onno Pols, Evert Glebbeek and Richard Stancliffe A Short Journey... Your Night Sky:
White dwarf dynamical interactions. Enrique García-Berro. Jornades de Recerca, Departament de Física
White dwarf dynamical interactions Enrique García-Berro Jornades de Recerca, Departament de Física CONTENTS 1. Introduction 2. Smoothed Particle Hydrodynamics 3. White dwarf mergers 4. White dwarf collisions
Ages of the oldest stars and the connection to the halo and accretion. Three questions about the ages of old stars
ages 2 : Taking stellar ages to the next power Daily Agenda Monday, September 18, 2017 Ages of the oldest stars and the connection to the halo and accretion 9:15 S. Cassisi, S. Degl Innocenti Three questions
The Chemical/Dynamical Evolution of the Galactic Bulge
Astro2020 Science White Paper The Chemical/Dynamical Evolution of the Galactic Bulge Thematic Areas: Stars and Stellar Evolution Resolved Stellar Populations and their Environments Galaxy Evolution Principal
STELLAR POPULATIONS. Erasmus Mundus Padova - Italy
STELLAR POPULATIONS Erasmus Mundus Padova - Italy 2010-2011 Prof. Antonio Bianchini Dipartimento di Astronomia Università di Padova antonio.bianchini@unipd.it THE HR DIAGRAM - 5b Notes about stellar evolution
Nobuya Nishimura Keele University, UK
7. Aug. 2014 @INT Studies of r-process nucleosynthesis based on recent hydrodynamical models of NS-NS mergers Nobuya Nishimura Keele University, UK The r-process: observational request - many r-rich Galactic
Short-lived 244 Pu points to compact binary mergers as sites for heavy r-process nucleosynthesis
SUPPLEMENTARY INFORMATION DOI: 10.1038/NPHYS3574 Short-lived 244 Pu points to compact binary mergers as sites for heavy r-process nucleosynthesis 1 Interpretation of the deep sea measurement Wallner et
A100 Exploring the Universe: The Milky Way as a Galaxy. Martin D. Weinberg UMass Astronomy
A100 Exploring the Universe: The Milky Way as a Galaxy Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu November 12, 2014 Read: Chap 19 11/12/14 slide 1 Exam #2 Returned and posted tomorrow
Stars and their properties: (Chapters 11 and 12)
Stars and their properties: (Chapters 11 and 12) To classify stars we determine the following properties for stars: 1. Distance : Needed to determine how much energy stars produce and radiate away by using
Astronomy Ch. 21 Stellar Explosions. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 21 Stellar Explosions MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A surface explosion on a white dwarf, caused
The power of chemical tagging for studying Galactic evolution
for studying Galactic evolution RSAA, Australian National University, Cotter Rd, Weston Creek, ACT, 2611, Australia E-mail: ewylie@mso.anu.edu.au Kenneth Freeman RSAA, Australian National University, Cotter
The King's University College Astronomy 201 Mid-Term Exam Solutions
The King's University College Astronomy 201 Mid-Term Exam Solutions Instructions: The exam consists of two sections. Part A is 20 multiple choice questions - please record answers on the sheet provided.
A100H Exploring the Universe: Discovering Galaxies. Martin D. Weinberg UMass Astronomy
A100H Exploring the Universe: Discovering Galaxies Martin D. Weinberg UMass Astronomy astron100h-mdw@courses.umass.edu April 05, 2016 Read: Chap 19 04/05/16 slide 1 Exam #2 Returned by next class meeting
Stellar Explosions (ch. 21)
Stellar Explosions (ch. 21) First, a review of low-mass stellar evolution by means of an illustration I showed in class. You should be able to talk your way through this diagram and it should take at least
Rob Izzard. February 21, University of Utrecht. Binary Star Nucleosynthesis. Nucleosynthesis. Single Star Evolution. Binary Star.
University of Utrecht February 21, 2006 Contents Mechanisms Proton capture: H He via pp-chain, CNO, NeNa, MgAl The Sun and most stars Alpha capture: He C, C O, O Ne... Fe Evolved stars C-burning: C + C
Announcement: Quiz Friday, Oct 31
Announcement: Quiz Friday, Oct 31 What is the difference between the giant, horizontal, and asymptotic-giant branches? What is the Helium flash? Why can t high-mass stars support themselves in hydrostatic
Clicker Question: Clicker Question: Clicker Question: Clicker Question: What is the remnant left over from a Type Ia (carbon detonation) supernova:
Test 3 results D C Grades posted in cabinet and Grades posted on-line B A F If you are not properly registered then come see me for your grade What is the ultimate origin of the elements heavier than helium
The electrons then interact with the surrounding medium, heat it up, and power the light curve. 56 Ni 56 Co + e (1.72 MeV) half life 6.
Supernovae The spectra of supernovae fall into many categories (see below), but beginning in about 1985, astronomers recognized that there were physically, only two basic types of supernovae: Type Ia and
Chapter 21 Stellar Explosions
Chapter 21 Stellar Explosions Units of Chapter 21 21.1 XXLife after Death for White Dwarfs (not on exam) 21.2 The End of a High-Mass Star 21.3 Supernovae Supernova 1987A The Crab Nebula in Motion 21.4
Carbon Enhanced Metal Poor (CEMP) Stars and the Halo System of the Milky Way
Carbon Enhanced Metal Poor (CEMP) Stars and the Halo System of the Milky Way Daniela Carollo Sydney Castiglione della Pescaia September 2013 Carbon Enhanced Metal Poor Stars (CEMP) CEMP = Carbon Enhanced
Nucleosynthesis of heavy elements. Almudena Arcones Helmholtz Young Investigator Group
Nucleosynthesis of heavy elements Almudena Arcones Helmholtz Young Investigator Group The nuclear chart uranium masses measured at the ESR 82 silver gold r-proce path 126 stable nuclei 50 82 will be measured
ASTR-101 4/4/2018 Stellar Evolution: Part II Lecture 19
ASTR-101 4/4/2018 Stellar Evolution: Part II Lecture 19 WHEN S THE NEXT TEST?!?!?!? If anyone is following the syllabus, you know that it says there is a test today. The test will be on April 11 th (a
Our Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye
Our Galaxy Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust Held together by gravity! The Milky Way with the Naked Eye We get a special view of our own galaxy because we are part of it!
Galaxy Formation: Overview
Galaxy Formation: Overview Houjun Mo March 30, 2004 The basic picture Formation of dark matter halos. Gas cooling in dark matter halos Star formation in cold gas Evolution of the stellar populaion Metal
金属欠乏星の r プロセス元素組成. r-process abundance of metal-poor stars
金属欠乏星の r プロセス元素組成 r-process abundance of metal-poor stars 本田敏志 Satoshi Honda Center for Astronomy, Univ. of Hyogo Nishi-Harima Astronomical Observatory 初代星 初代銀河研究会 2017@ 呉 2018.2.10-12 Stellar abundances
The physics of stars. A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure.
Lecture 4 Stars The physics of stars A star begins simply as a roughly spherical ball of (mostly) hydrogen gas, responding only to gravity and it s own pressure. X-ray ultraviolet infrared radio To understand
Late Stages of Stellar Evolution. Late Stages of Stellar Evolution
Late Stages of Stellar Evolution The star enters the Asymptotic Giant Branch with an active helium shell burning and an almost dormant hydrogen shell Again the stars size and luminosity increase, leading
Gas and dust pollution. from AGB stars.
Osservatorio Astronomico di Roma Gas and dust pollution from AGB stars. Marcella Di Criscienzo INAF-Osservatorio Astronomico di Roma Collaborators: P. Ventura, F. Dell Agli, F. D Antona, A. Karakas, A.