Topics at the DRS Late stages stellar evolution White dwarfs

Slides:

Advertisements

Similar presentations

X-ray pulsars in wind-fed accretion systems 王伟 (NAOC) July 2009, Pulsar Summer School Beijing.

Advertisements

SN 1987A spectacular physics Bruno Leibundgut ESO.

Susan CartwrightOur Evolving Universe1 The Deaths of Stars n What happens to stars when the helium runs out? l l do they simply fade into oblivion? l l.

ASTR Fall Semester Joel E. Tohline, Alumni Professor Office: 247 Nicholson Hall [Slides from Lecture17]

Feedback: in the form of outflow. AGN driven outflow.

Stephen C.-Y. Ng McGill University. Outline Why study supernova? What is a supernova? Why does it explode? The aftermaths --- Supernova remnants Will.

At the Heart of a Supernova Your name and affiliation here.

LECTURE 20, NOVEMBER 9, 2010 ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT 1ASTR 101-3, FALL 2010.

Supernovae from Massive Stars: light curves and spectral evolution Bruno Leibundgut ESO.

X-Ray UltravioletVisibleInfraredRadio The Electromagnetic Spectrum and the Universe.

Earth Science 25.2B : Stellar Evolution

Chania, Crete, August 2004 “The environment of galaxies” Pierre-Alain Duc Recycling in the galaxy environment F. Bournaud J. Braine U. Lisenfeld P. Amram.

X Ray Astronomy Presented by:- Mohit Shashwat Ankit.

Active Galactic Nuclei Astronomy 315 Professor Lee Carkner Lecture 19.

1 Origin of Variability of X-ray and γ-ray Spectra on Daily Scale Radovan Milinčić Astrophysics 711 May 3 rd 2005.

Clicker Question: What is the ultimate origin of the elements heavier than helium that make up your body? (a)They were present when the Universe was created.

Department of Astronomy, University of Padova Department of Physics, University of Padova INAF-Astronomical Observatory of Padova Paola Mucciarelli In.

Institute for Astronomy and Astrophysics, University of Tübingen, Germany July 5, 2004Cool Stars, Stellar Systems and the Sun (Hamburg, Germany)1 Turning.

Accurate Atomic Rates for Black Hole Accretion Disks John Raymond Disk winds have been know in AGN for years and suspected in Galactic Black Hole Binaries.

Question 1 Stellar parallax is used to measure the a) sizes of stars.

The Milky Way. Structure of the Milky Way The Milky Way.

Outline  Introduction  The Life Cycles of Stars  The Creation of Elements  A History of the Milky Way  Nucleosynthesis since the Beginning of Time.

Death of Stars I Physics 113 Goderya Chapter(s): 13 Learning Outcomes:

Stellar Atmospheres: Motivation 1 Stellar Atmospheres: Literature Dimitri Mihalas –Stellar Atmospheres, W.H. Freeman, San Francisco Albrecht Unsöld –Physik.

Black holes: do they exist?

Overview of Astronomy AST 200. Astronomy Nature designs the Experiment Nature designs the Experiment Tools Tools 1) Imaging 2) Spectroscopy 3) Computational.

21 October 2004UWO Studying stars with spectroscopy John Landstreet Department of Physics and Astronomy University of Western Ontario.

200 MG 500 MG TheoryObservation Authors Institutes RE J is a hydrogen rich strongly magnetic white dwarf discovered as an EUV source by the ROSAT.

Extragalactic stellar astronomy with the brightest stars in the universe Rolf Kudritzki, Fabio Bresolin, Miguel Urbaneja.

Hunting down the subdwarf populations Peter Nemeth KU Leuven, Belgium Bamberg, Germany; Sep 13, 2013.

The Sun: Part 3 and Measuring the Stars: Part 1. Net result: 4 protons → 4 He + 2 neutrinos + energy Hydrostatic Equilibrium: pressure from fusion reactions.

1 Stellar Remnants White Dwarfs, Neutron Stars & Black Holes These objects normally emit light only due to their very high temperatures. Normally nuclear.

By Chloe O.. Nebula The nebula is an interstellar cloud of dust, hydrogen gas, helium gas and plasma. Many nebulae form from the gravitational collapse.

Unravelling the formation and evolutionary histories of the most massive galaxies Ilani Loubser (Univ. of the Western Cape)

Class Goals Familiarity with basic terms and definitions Physical insight for conditions, parameters, phenomena in stellar atmospheres Appreciation of.

Hot gas in galaxy pairs Olga Melnyk. It is known that the dark matter is concentrated in individual haloes of galaxies and is located in the volume of.

How Stars Form Shantanu Basu Physics & Astronomy University of Western Ontario Preview Western, May 3/4, 2003.

A cosmic abundance standard Fernanda Nieva from massive stars in the Solar Neighborhood Norbert Przybilla (Bamberg-Erlangen) & Keith Butler (LMU)

ASTR112 The Galaxy Lecture 7 Prof. John Hearnshaw 11. The galactic nucleus and central bulge 11.1 Infrared observations (cont.) 11.2 Radio observations.

Lecture 30: The Milky Way. topics: structure of our Galaxy structure of our Galaxy components of our Galaxy (stars and gas) components of our Galaxy (stars.

© Sierra College Astronomy Department 1 Astronomy 10 Elementary Astronomy COURSE GOALS & OBJECTIVES.

Earth & Space Science March 2015

Colin Folsom (Armagh Observatory).  Read input  Calculate line components (Zeeman splitting)  Calculate continuum opacity (per window, per atmospheric.

Warm Absorbers: Are They Disk Outflows? Daniel Proga UNLV.

Progenitor stars of supernovae Poonam Chandra Royal Military College of Canada.

Hunting down the subdwarf populations Peter Nemeth Roy Østensen and Joris Vos KU Leuven, Belgium; In collaboration with Stephane Vennes and Adela Kawka.

Radio Galaxies part 4. Apart from the radio the thin accretion disk around the AGN produces optical, UV, X-ray radiation The optical spectrum emitted.

Julie Hollek and Chris Lindner.  Background on HK II  Stellar Analysis in Reality  Methodology  Results  Future Work Overview.

Neutron Stars & Black Holes (Chapter 11) APOD. Student Learning Objective Indentify properties of Neutron Stars & Black Holes NASA.

Lecture 1 Stellar evolution, spectral features and chemical composition, luminosity, blackbody radiation, color index and Hertzsprung-Russel diagram transitions,

Star Properties and Stellar Evolution. What are stars composed of? Super-hot gases of Hydrogen and Helium. The sun is 70% Hydrogen and 30% Helium.

1 ASTR 8000 STELLAR ATMOSPHERES AND SPECTROSCOPY Introduction & Syllabus Light and Matter Sample Atmosphere.

7 - Stellar Evolution-II. Surface abundances vs. time and mass loss time What’s at the surface.

FIRST LIGHT A selection of future facilities relevant to the formation and evolution of galaxies Wavelength Sensitivity Spatial resolution.

High energy Astrophysics Mat Page Mullard Space Science Lab, UCL 1. Overview.

Competitive Science with the WHT for Nearby Unresolved Galaxies Reynier Peletier Kapteyn Astronomical Institute Groningen.

The Deaths of Stars Please press “1” to test your transmitter.

“Globular” Clusters: M15: A globular cluster containing about 1 million (old) stars. distance = 10,000 pc radius  25 pc “turn-off age”  12 billion years.

Life of Stars. Star Birth – Nebular Model Huge clouds of gas and dust occur in space – may be exploded stars Most Nebulae (gas clouds) are invisible –

1 ASTRON is part of the Netherlands Organisation for Scientific Research (NWO) Netherlands Institute for Radio Astronomy Astronomy at ASTRON George Heald.

Chapter 19 Table of Contents Section 2 The Life Cycle of Stars

Determining Abundances

Keck Observations of Two Supernovae Hours After Explosion Shock-Breakout Flash Spectroscopy as a New Window into the Evolution and Death of Massive Stars.

A Galaxy Revealed in Multiple Wavelengths

Just What is a Supernova?

Neutron Stars and Black Holes

Composition of Stars Classify stars by their color, size, and brightness. Other properties of stars are chemical composition and mass. Color and Temperature.

Chapter 16 – Chemical Analysis

Just What is a Supernova?

Presentation transcript:

Topics at the DRS Late stages stellar evolution White dwarfs Hot massive stars & extragalactic stellar astronomy Binaries with massive companions X-ray astronomy, neutron stars, black holes & AGN

Late stages of stellar evolution Chemical composition Late stages of stellar evolution Kinematics, Hypervelocity stars Heiko Hirsch pulsations SN Ia progenitors White dwarf rotation Uli Heber Alfred Tillich Stephan Geier Christian Schmitt

Hot massive stars & extragalactic stellar astronomy NLTE model atmospheres Galactic abundance gradients Chemical composition Norbert Przybilla BA Supergiants Markus Firnstein Fernanda Nieva Florian Schiller

White dwarfs Magnetic fields Diffusion Klaus Unglaub Irmela Bues

Binaries with massive components Large Magellanic cloud Light curves Horst Drechsel Stefan Nesslinger

Neutron stars, black holes & AGN Cygnus X-1 Jörn Wilms Manfred Hanke

Observations Optical spectroscopy: ESO, Calar Alto, Keck UV spectroscopy: HST & FUSE X-ray: XMM, Chandra, Suzaku, RXTE γ-ray: INTEGRAL Imaging & Astrometry Future: eRosita, SIMBOL-X

Education - Physics undergraduates (1. year) - Physics graduates Lecture courses for - Physics undergraduates (1. year) - Physics graduates - student teachers - non-physics graduates (mostly computer science) Lab course (Praktikum): 60 students/year Numerics course

Plate Archive from Bamberg: 1921 – 1960 more than 12000 plates photographic monitoring (Felderplan with Sonneberg & Potsdam) from Bamberg: 1921 – 1960 Boyden-station (South Africa): 1963-1974 more than 12000 plates plate scanning since 2003 collaboration with Tsvetkov et al. (Bulgarian Academy of Sciences)

Public Outreach and public lectures: 700-2000 people/year Public observations, guided tours, slide shows and public lectures: 700-2000 people/year

Collaborations

Komponenten der Galaxis Dark matter Very old stars Old stars Young & old stars Buser

Quantitative Spektralanalyse Komplexe Modelatome: Schwere Elemente

DETAIL SURFACE Flux  Input Model Atom Atmospheric Parameters Levels: *Excitation Potentials *Statistical Weights *Ionization States Transitions: *Oscillator Strength *Photoionization cross sections *Excitation and Ionization cross sections Atmospheric Parameters Teff, logg, [M/H] * f line components * Statistical Weights   col and  rad    Abundance Model Atmosphere DETAIL Statistical Equilibrium & Radiative Transference S= S(ni) Rij = Rij(J) SURFACE Line profiles of the atom Iteration until Si = Si-1 Voigt profile Output DETAIL Input SURFACE Occupation numbers ni for each  Flux 

Elementhäufigkeiten Heiße Sterne: Ultravioletspektroskopie: HST

Elementhäufigkeiten: - Unterhäufigkeiten leichter Elemente Überhäufigkeiten schwerer Elemente im Vergleich zur Sonne

Asteroseismologie Nichtradiale Pulsationen

Hyper-velocity star Definition: - Raumgeschwindigkeit übersteigt lokale Entweichgeschwindigkeit Stern ist nicht mehr an Galaxis gebunden - Entweichgeschwindigkeit von der Galaxis: ca. 500km/s