Constraints on the explosion mechanism and progenitors of Type Ia supernovae
|
|
|
- Jeffery Simon
- 10 years ago
- Views:
Transcription
1 Constraints on the explosion mechanism and progenitors of Type Ia supernovae Stéphane Blondin Laboratoire d Astrophysique de Marseille Luc Dessart Observatoire de la Côte d Azur John Hillier University of Pi>sburgh Alexei Khokhlov University of Chicago Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes"
2 A one- dimensional Chandrasekhar- mass delayed- detona3on model for the broad- lined Type Ia supernova 2002bo Blondin, S., Dessart, L., Hillier, D. J MNRAS, 448, 2766 Cri3cal ingredients of Type Ia supernova radia3ve- transfer modelling Dessart, L., Hillier, D. J., Blondin, S., Khokhlov, A. M MNRAS, 441, 3249 Constraints on the explosion mechanism and progenitors of type Ia supernovae Dessart, L., Blondin, S., Hillier, D. J., Khokhlov, A. M MNRAS, 441, 532 [CoIII] versus NaID in type Ia supernova spectra Dessart, L., Hillier, D. J., Blondin, S., Khokhlov, A. M MNRAS, 439, One- dimensional delayed- detona3on models of Type Ia supernovae: Confronta3on to observa3ons at bolometric maximum Blondin, S., Dessart, L., Hillier, D. J., Khokhlov, A. M MNRAS, 429, 2127 Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 2
3 Chemical evolujon Explosive nucleosynthesis main producers of iron combusbon, turbulence Cosmic- Ray AcceleraJon supernova remnants Binary stellar evolujon mass transfer, grav. waves Cosmology, Dark Energy distance measurements Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 3
4 Thermonuclear disrupbon of a C/O WD star near the Chandrasekhar mass 1.4 M M( 56 Ni) 0.5 M Blondin et al. (2015) Light- curve powered by 56 Ni decay Spectra indicate chemical strajficajon Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 4
5 Thermonuclear disrupbon of a C/O WD star near the Chandrasekhar mass 1.4 M M( 56 Ni) 0.5 M Blondin et al. (2015) Light- curve powered by 56 Ni decay Spectra indicate chemical strajficajon Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 5
6 seconds Credit: Frank Timmes Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 6
7 56 Ni M seconds IMEs M Unburnt C/O < 0.1 M Stable Fe/Ni M Credit: Frank Timmes Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 7
8 VariaRon in peak luminosity 10 Diversity at a given luminosity SN 2002bo SN 2011fe Δv 3000 km/s Evidence for mul3ple progenitor channels and explosion mechanisms? Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 8
9 No direct detecjon of SN Ia progenitors (e.g., SN 2011fe in M101, D=6.4 Mpc) Li et al. (2011) M Excluded: Red Giants M > 3.5 M # He star RNe M V 0 Indirect constraints from: potenral progenitor popularons (recurrent Novae, binary WDs, ) early post shock- breakout luminosity (R prog < 0.1 R for SN 2011fe) interacron with binary companion + CSM (Ṁ 10-9 M yr - 1 from radio/x- ray limits) surviving companion star in SN remnants SN rates vs. host stellar popularon Need constraints from numerical simula3ons! Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 9
10 1. C/O WD HydrostaRc X C X O 0.5 Magic 2. Explosion 1D hydro + burning Homologous expansion v(r) t exp < 1 min 1 st Law 3. RadiaJve Transfer 1D non- LTE (CMFGEN) Time- dependent D/Dt Non- local energy deposiron Non- thermal effects Hillier & Dessart (2012) Days since Explosion Iron Nickel Silicon Oxygen Carbon 4. Comparison to ObservaJons Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 10
11 Maximum- light spectra (Blondin et al. 2013) IniRal deflagrajon transirons to a detonajon at a fixed density, ρ tr Lower ρ tr Less 56 Ni Lower L peak but same kinerc energy! Decreasing 56 Ni mass Temperature IonizaRon Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 11
12 Good match to spectral evolujon between d past explosion Blondin et al. (2015) DDC15 vs. SN 2002bo chemical strarficaron spherical symmetry no fine- tuning! Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 12
13 Tycho SNR Iron Silicon Shocked e - Dust spherically symmetric strarfied ejecta Image Credit: MPIA/NASA/Calar Alto Observatory Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 13
14 ρ AM : DDTa-c-e ρ AM =2x10-24 Tycho SNR 56 Ni Iron Silicon Shocked e - Dust Bright Normal SN SN Ia Ia spherically symmetric strarfied ejecta uce amics. check ness. X- ray spectra matched by 1D delayed- detonaron models Dim Normal SN Ia SN Ia Badenes et al. (2006) Image Credit: MPIA/NASA/Calar Alto Observatory Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 14 sity of Pittsburgh Jan
15 Good match to spectral evolujon between d past explosion Blondin et al. (2015) DDC15 vs. SN 2002bo chemical strarficaron spherical symmetry no fine- tuning! too faint/cool at earliest Rmes Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 15
16 Good match to spectral evolujon between d past explosion Blondin et al. (2015) DDC15 vs. SN 2002bo chemical strarficaron spherical symmetry no fine- tuning! too faint/cool at earliest Rmes Ca II 8500 Å emission (Co II?) Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 16
17 11 Khokhlov, Höflich & Müller (1992) Outer envelope v > km/s 10 Outer layers sjll expanding lg R, cm 9 Inner layers v km/s 8 E bind < 0 DeflagraJon Inward shock wave DetonaJon at a fixed density, ρ tr Jme, sec Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 17
18 Standard DD PulsaJng DD PulsaRon leads to a density cliff and a hoher outer ejecta Density Temperature Impacts early- Jme spectra: unburnt C/O at large velocity narrower lines bluer oprcal colors independent of 56 Ni mass! Expect similar interacbon in double WD mergers Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 18
19 Standard DD PulsaJng DD Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 19
20 t exp = 2 d C II 6580 Å Standard DD PulsaJng DD t exp = 15 d Diversity bluer spectra unburnt C narrow lines Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 20
21 Be>er match to the nearby SN 2011fe Standard DD Δt B = 14 d PulsaJng DD Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 21
22 Pure detonaron of sub- M Ch WD Density Model M tot [M ] M( 56 Ni) [M ] E kin [10 51 erg] DDC SCH1p Standard M Ch Sub- M Ch 56 Ni extends to outermost ejecta Impacts light- curve evolujon: 56 Ni faster rise to maximum faster post- maximum decline Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 22
23 Standard M Ch Sub- M Ch SN 1999by (Blondin et al., in preparabon) Be>er match to subluminous events Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 23
24 Standard Chandrasekhar- mass model matches most normal SN Ia No evidence for strong departures from spherical symmetry PulsaRon/interacRon produces diversity at a given luminosity Sub- luminous events appear to require less massive progenitors Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 24
25 Standard Chandrasekhar- mass model matches most normal SN Ia No evidence for strong departures from spherical symmetry PulsaRon/interacRon produces diversity at a given luminosity Sub- luminous events appear to require less massive progenitors More realisrc WD progenitors from stellar evolujon models Compare 1D to angle- averaged mulj- D explosion models hsps://www- n.oca.eu/supernova/home.html Stéphane Blondin (LAM) Journées de la SF2A Atelier PNPS/PNHE "Stades UlJmes" 25
Evolution of Close Binary Systems
Evolution of Close Binary Systems Before going on to the evolution of massive stars and supernovae II, we ll think about the evolution of close binary systems. There are many multiple star systems in the
165 points. Name Date Period. Column B a. Cepheid variables b. luminosity c. RR Lyrae variables d. Sagittarius e. variable stars
Name Date Period 30 GALAXIES AND THE UNIVERSE SECTION 30.1 The Milky Way Galaxy In your textbook, read about discovering the Milky Way. (20 points) For each item in Column A, write the letter of the matching
Stéphane Blondin Curriculum Vitæ 1. Stéphane Blondin
Stéphane Blondin Curriculum Vitæ 1 Stéphane Blondin Laboratoire d Astrophysique de Marseille (LAM) 38, rue Frédéric Joliot-Curie 13388 Marseille Cedex 13, France Phone: +33 (0)4 91 05 69 41 Email: [email protected]
Nuclear fusion in stars. Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars
Nuclear fusion in stars Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars The origin of structure in the Universe Until the time of formation of protogalaxies,
Ay 20 - Lecture 9 Post-Main Sequence Stellar Evolution. This file has many figures missing, in order to keep it a reasonable size.
Ay 20 - Lecture 9 Post-Main Sequence Stellar Evolution This file has many figures missing, in order to keep it a reasonable size. Main Sequence and the Range of Stellar Masses MS is defined as the locus
Astro 102 Test 5 Review Spring 2016. See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14
Astro 102 Test 5 Review Spring 2016 See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14 Sec 14.5 Expanding Universe Know: Doppler shift, redshift, Hubble s Law, cosmic distance ladder, standard candles,
Stellar Evolution: a Journey through the H-R Diagram
Stellar Evolution: a Journey through the H-R Diagram Mike Montgomery 21 Apr, 2001 0-0 The Herztsprung-Russell Diagram (HRD) was independently invented by Herztsprung (1911) and Russell (1913) They plotted
Class 2 Solar System Characteristics Formation Exosolar Planets
Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System
Stellar Evolution. The Basic Scheme
Stellar Evolution The Basic Scheme Stars live for a very long time compared to human lifetimes. Even though stellar life-spans are enormous, we know how stars are born, live, and die. All stars follow
The Orbital Period Distribution of Wide Binary Millisecond Pulsars
Binary Radio Pulsars ASP Conference Series, Vol. 328, 2005 F. A. Rasio and I. H. Stairs The Orbital Period Distribution of Wide Binary Millisecond Pulsars B. Willems Northwestern University, Department
Be Stars. By Carla Morton
Be Stars By Carla Morton Index 1. Stars 2. Spectral types 3. B Stars 4. Be stars 5. Bibliography How stars are formed Stars are composed of gas Hydrogen is the main component of stars. Stars are formed
Origins of the Cosmos Summer 2016. Pre-course assessment
Origins of the Cosmos Summer 2016 Pre-course assessment In order to grant two graduate credits for the workshop, we do require you to spend some hours before arriving at Penn State. We encourage all of
The Universe Inside of You: Where do the atoms in your body come from?
The Universe Inside of You: Where do the atoms in your body come from? Matthew Mumpower University of Notre Dame Thursday June 27th 2013 Nucleosynthesis nu cle o syn the sis The formation of new atomic
thermal history of the universe and big bang nucleosynthesis
thermal history of the universe and big bang nucleosynthesis Kosmologie für Nichtphysiker Markus Pössel (vertreten durch Björn Malte Schäfer) Fakultät für Physik und Astronomie, Universität Heidelberg
WHERE DID ALL THE ELEMENTS COME FROM??
WHERE DID ALL THE ELEMENTS COME FROM?? In the very beginning, both space and time were created in the Big Bang. It happened 13.7 billion years ago. Afterwards, the universe was a very hot, expanding soup
The Chemical Composition of a Molecular Cloud at the Outer Edge of the Galaxy
Carnegie Observatories Astrophysics Series, Vol. 4: Origin and Evolution of the Elements, 2003 ed. A. McWilliam and M. Rauch (Pasadena: Carnegie Observatories, http://www.ociw.edu/ociw/symposia/series/symposium4/proceedings.html)
The Universe. The Solar system, Stars and Galaxies
The Universe The Universe is everything. All us, the room, the U.S. the earth, the solar system, all the other stars in the Milky way galaxy, all the other galaxies... everything. How big and how old is
Einstein Rings: Nature s Gravitational Lenses
National Aeronautics and Space Administration Einstein Rings: Nature s Gravitational Lenses Leonidas Moustakas and Adam Bolton Taken from: Hubble 2006 Science Year in Review The full contents of this book
Homework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh
Homework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh Chapter 5: #50 Hotter Sun: Suppose the surface temperature of the Sun were about 12,000K, rather than 6000K. a. How
Ernst Zinner Washington University St. Louis
QuickTime and a decompressor are needed to see this picture. QuickTime and a decompressor are needed to see this picture. QuickTime and a decompressor are needed to see this picture. Constraints on SN
18.1 Close Binary Star Systems
M. Pettini: Structure and Evolution of Stars Lecture 18 BINARY STARS and TYPE Ia SUPERNOVAE 18.1 Close Binary Star Systems It is thought that about half of the stars in the sky are in multiple systems,
Top 10 Discoveries by ESO Telescopes
Top 10 Discoveries by ESO Telescopes European Southern Observatory reaching new heights in astronomy Exploring the Universe from the Atacama Desert, in Chile since 1964 ESO is the most productive astronomical
Heating & Cooling in Molecular Clouds
Lecture 8: Cloud Stability Heating & Cooling in Molecular Clouds Balance of heating and cooling processes helps to set the temperature in the gas. This then sets the minimum internal pressure in a core
Astronomy & Physics Resources for Middle & High School Teachers
Astronomy & Physics Resources for Middle & High School Teachers Gillian Wilson http://www.faculty.ucr.edu/~gillianw/k12 A cosmologist is.... an astronomer who studies the formation and evolution of the
How Do Galeries Form?
8-5-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c9-1 8-5-2015see http://www.strw.leidenuniv.nl/ franx/college/ mf-sts-2015-c9-2 Galaxy Formation Leading questions for today How do
Lecture 14. Introduction to the Sun
Lecture 14 Introduction to the Sun ALMA discovers planets forming in a protoplanetary disc. Open Q: what physics do we learn about the Sun? 1. Energy - nuclear energy - magnetic energy 2. Radiation - continuum
IV. Molecular Clouds. 1. Molecular Cloud Spectra
IV. Molecular Clouds Dark structures in the ISM emit molecular lines. Dense gas cools, Metals combine to form molecules, Molecular clouds form. 1. Molecular Cloud Spectra 1 Molecular Lines emerge in absorption:
8 Radiative Cooling and Heating
8 Radiative Cooling and Heating Reading: Katz et al. 1996, ApJ Supp, 105, 19, section 3 Thoul & Weinberg, 1995, ApJ, 442, 480 Optional reading: Thoul & Weinberg, 1996, ApJ, 465, 608 Weinberg et al., 1997,
Stellar Astrophysics: Stellar Evolution 1. Stellar Evolution
Stellar Astrophysics: Stellar Evolution 1 Stellar Evolution Update date: October 29, 2014 With the understanding of the basic physical processes in stars, we now proceed to study their evolution. In particular,
7. In which part of the electromagnetic spectrum are molecules most easily detected? A. visible light B. radio waves C. X rays D.
1. Most interstellar matter is too cold to be observed optically. Its radiation can be detected in which part of the electromagnetic spectrum? A. gamma ray B. ultraviolet C. infrared D. X ray 2. The space
Using Photometric Data to Derive an HR Diagram for a Star Cluster
Using Photometric Data to Derive an HR Diagram for a Star Cluster In In this Activity, we will investigate: 1. How to use photometric data for an open cluster to derive an H-R Diagram for the stars and
WELCOME to Aurorae In the Solar System. J.E. Klemaszewski
WELCOME to Aurorae In the Solar System Aurorae in the Solar System Sponsoring Projects Galileo Europa Mission Jupiter System Data Analysis Program ACRIMSAT Supporting Projects Ulysses Project Outer Planets
OUTLINE The Hubble parameter After these lectures, you should be able to: Define the Hubble parameter H Sketch a(t) for k>0, k=0, k<0 assuming Λ=0 Def
Observational cosmology: The Friedman equations 2 Filipe B. Abdalla Kathleen Lonsdale Building G.22 http://zuserver2.star.ucl.ac.uk/~hiranya/phas3136/phas3136 OUTLINE The Hubble parameter After these lectures,
Introduction and Origin of the Earth
Page 1 of 5 EENS 1110 Tulane University Physical Geology Prof. Stephen A. Nelson Introduction and Origin of the Earth This page last updated on 30-Jul-2015 Geology, What is it? Geology is the study of
Classroom Exercise ASTR 390 Selected Topics in Astronomy: Astrobiology A Hertzsprung-Russell Potpourri
Classroom Exercise ASTR 390 Selected Topics in Astronomy: Astrobiology A Hertzsprung-Russell Potpourri Purpose: 1) To understand the H-R Diagram; 2) To understand how the H-R Diagram can be used to follow
Chapter 15.3 Galaxy Evolution
Chapter 15.3 Galaxy Evolution Elliptical Galaxies Spiral Galaxies Irregular Galaxies Are there any connections between the three types of galaxies? How do galaxies form? How do galaxies evolve? P.S. You
Magellanic Cloud planetary nebulae as probes of stellar evolution and populations. Letizia Stanghellini
Magellanic Cloud planetary nebulae as probes of stellar evolution and populations Letizia Stanghellini Planetary nebulae beyond the Milky Way - May 19-21, 2004 1 Magellanic Cloud PNe The known distances,
1 Introduction. Name: 1.1 Spectral Classification of Stars. PHYS-1050 Hertzsprung-Russell Diagram Solutions Spring 2013
Name: 1 Introduction Read through this information before proceeding on with the lab. 1.1 Spectral Classification of Stars 1.1.1 Types of Spectra Astronomers are very interested in spectra graphs of intensity
on Recent Developments on Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories
Thirteenth Marcel Grossman Meeting on Recent Developments on Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories ON GENERAL RELATIVISTIC UNIFORMLY ROTATING WHITE
Ellipticals. Elliptical galaxies: Elliptical galaxies: Some ellipticals are not so simple M89 E0
Elliptical galaxies: Ellipticals Old view (ellipticals are boring, simple systems)! Ellipticals contain no gas & dust! Ellipticals are composed of old stars! Ellipticals formed in a monolithic collapse,
= = GM. v 1 = Ωa 1 sin i.
1 Binary Stars Consider a binary composed of two stars of masses M 1 and We define M = M 1 + and µ = M 1 /M If a 1 and a 2 are the mean distances of the stars from the center of mass, then M 1 a 1 = a
World of Particles Big Bang Thomas Gajdosik. Big Bang (model)
Big Bang (model) What can be seen / measured? basically only light (and a few particles: e ±, p, p, ν x ) in different wave lengths: microwave to γ-rays in different intensities (measured in magnitudes)
Test 2 --- Natural Sciences 102, Professors Rieke --- VERSION B March 3, 2010
Enter your answers on the form provided. Be sure to write your name and student ID number on the first blank at the bottom of the form. Please mark the version (B) in the Key ID space at the top of the
MODERN ATOMIC THEORY AND THE PERIODIC TABLE
CHAPTER 10 MODERN ATOMIC THEORY AND THE PERIODIC TABLE SOLUTIONS TO REVIEW QUESTIONS 1. Wavelength is defined as the distance between consecutive peaks in a wave. It is generally symbolized by the Greek
8.1 Radio Emission from Solar System objects
8.1 Radio Emission from Solar System objects 8.1.1 Moon and Terrestrial planets At visible wavelengths all the emission seen from these objects is due to light reflected from the sun. However at radio
8. The evolution of stars a more detailed picture
8. The evolution of stars a more detailed picture 8.1Pre Main-Sequence Evolution Evolution onto the main sequence begins with a cloud of cold gas which contracts under self-gravity. Potential Energy is
Observing the Universe
Observing the Universe Stars & Galaxies Telescopes Any questions for next Monday? Light Doppler effect Doppler shift Doppler shift Spectra Doppler effect Spectra Stars Star and planet formation Sun Low-mass
The Hidden Lives of Galaxies. Jim Lochner, USRA & NASA/GSFC
The Hidden Lives of Galaxies Jim Lochner, USRA & NASA/GSFC What is a Galaxy? Solar System Distance from Earth to Sun = 93,000,000 miles = 8 light-minutes Size of Solar System = 5.5 light-hours What is
5. The Nature of Light. Does Light Travel Infinitely Fast? EMR Travels At Finite Speed. EMR: Electric & Magnetic Waves
5. The Nature of Light Light travels in vacuum at 3.0. 10 8 m/s Light is one form of electromagnetic radiation Continuous radiation: Based on temperature Wien s Law & the Stefan-Boltzmann Law Light has
The Sino-French Gamma-Ray Burst Mission SVOM (Space-based multi-band astronomical Variable Objects Monitor)
The Sino-French Gamma-Ray Burst Mission SVOM (Space-based multi-band astronomical Variable Objects Monitor) Didier BARRET on behalf of the SVOM collaboration [email protected] Outline SVOM background
Data Provided: A formula sheet and table of physical constants is attached to this paper. DARK MATTER AND THE UNIVERSE
Data Provided: A formula sheet and table of physical constants is attached to this paper. DEPARTMENT OF PHYSICS AND ASTRONOMY Autumn Semester (2014-2015) DARK MATTER AND THE UNIVERSE 2 HOURS Answer question
Cosmic Journey: Teacher Packet
Cosmic Journey: Teacher Packet Compiled by: Morehead State University Star Theatre with help from Bethany DeMoss Table of Contents Table of Contents 1 Corresponding Standards 2 Vocabulary 4 Sizing up the
On a Flat Expanding Universe
Adv. Studies Theor. Phys., Vol. 7, 2013, no. 4, 191-197 HIKARI Ltd, www.m-hikari.com On a Flat Expanding Universe Bo Lehnert Alfvén Laboratory Royal Institute of Technology, SE-10044 Stockholm, Sweden
Cosmic Dust in an Expanding Universe?
Planck energy - E - ev Cosmic Dust in an Expanding Universe? QED Radiations, Discovery Bay, Hong Kong, China [email protected] Copyright 2016 Horizon Research Publishing All rights reserved. Abstract Dust
Malcolm S. Longair. Galaxy Formation. With 141 Figures and 12 Tables. Springer
Malcolm S. Longair Galaxy Formation With 141 Figures and 12 Tables Springer Contents Part I Preliminaries 1. Introduction, History and Outline 3 1.1 Prehistory 3 1.2 The Theory of the Expanding Universe
The Messier Objects As A Tool in Teaching Astronomy
The Messier Objects As A Tool in Teaching Astronomy Dr. Jesus Rodrigo F. Torres President, Rizal Technological University Individual Member, International Astronomical Union Chairman, Department of Astronomy,
The Solar Journey: Modeling Features of the Local Bubble and Galactic Environment of the Sun
The Solar Journey: Modeling Features of the Local Bubble and Galactic Environment of the Sun P.C. Frisch and A.J. Hanson Department of Astronomy and Astrophysics University of Chicago and Computer Science
The Physics of Stellar Collapse (and GR Hydrodynamics)
The Physics of Stellar Collapse (and GR Hydrodynamics) Christian David Ott California Institute of Technology C. D. Ott - The Physics of Stellar Collapse Outline Outline Part 1 (a not so big picture overview)
and the VO-Science Francisco Jiménez Esteban Suffolk University
The Spanish-VO and the VO-Science Francisco Jiménez Esteban CAB / SVO (INTA-CSIC) Suffolk University The Spanish-VO (SVO) IVOA was created in June 2002 with the mission to facilitate the international
Study Guide: Solar System
Study Guide: Solar System 1. How many planets are there in the solar system? 2. What is the correct order of all the planets in the solar system? 3. Where can a comet be located in the solar system? 4.
Probes of Star Formation in the Early Universe
Gamma Ray Bursts Probes of Star Formation in the Early Universe Edward P.J.van den Heuvel Universiteit van Amsterdam &KITP-UCSB KITP, March 17, 2007 Age of the Universe: 13.7 billion years Age of our Milky
Spectral Classification of Stars
Department of Physics and Geology Astronomy 1402 Spectral Classification of Stars The purpose of this laboratory activity is to introduce you to stellar spectral classification. You will have an opportunity
Faber-Jackson relation: Fundamental Plane: Faber-Jackson Relation
Faber-Jackson relation: Faber-Jackson Relation In 1976, Faber & Jackson found that: Roughly, L! " 4 More luminous galaxies have deeper potentials Can show that this follows from the Virial Theorem Why
Department of Physics University of Wisconsin-Milwaukee Phone: (414) 229-2590 E-mail: [email protected] Milwaukee, WI 53201
Philip Chang Contact Information Education Department of Physics University of Wisconsin-Milwaukee Phone: (414) 229-2590 PO Box 413 E-mail: [email protected] Milwaukee, WI 53201 University of California
The Expanding Universe
Stars, Galaxies, Guided Reading and Study This section explains how astronomers think the universe and the solar system formed. Use Target Reading Skills As you read about the evidence that supports the
Elliptical Galaxies. Houjun Mo. April 19, 2004. Basic properties of elliptical galaxies. Formation of elliptical galaxies
Elliptical Galaxies Houjun Mo April 19, 2004 Basic properties of elliptical galaxies Formation of elliptical galaxies Photometric Properties Isophotes of elliptical galaxies are usually fitted by ellipses:
Class #14/15 14/16 October 2008
Class #14/15 14/16 October 2008 Thursday, Oct 23 in class You ll be given equations and constants Bring a calculator, paper Closed book/notes Topics Stellar evolution/hr-diagram/manipulate the IMF ISM
1W High Power Purple LED Technical Data Sheet. Part No.: LL-HP60MUVA
1W High Power Purple LED Technical Data Sheet Part No.: LL-HP60MUVA Spec No.: HP60M Rev No.: V.2 Date: Aug./18/2009 Page: 1 OF 8 Features: Luckylight High power LED type. Lead frame type package (Heat
Light. What is light?
Light What is light? 1. How does light behave? 2. What produces light? 3. What type of light is emitted? 4. What information do you get from that light? Methods in Astronomy Photometry Measure total amount
Lecture 3 Properties and Evolution of Molecular Clouds. Spitzer space telescope image of Snake molecular cloud (IRDC G11.11-0.11
Lecture 3 Properties and Evolution of Molecular Clouds Spitzer space telescope image of Snake molecular cloud (IRDC G11.11-0.11 From slide from Annie Hughes Review CO t in clouds HI: Atomic Hydrogen http://www.atnf.csiro.au/research/lvmeeting/magsys_pres/
From lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation?
From lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation? From lowest energy to highest energy, which of the following correctly
Solar Ast ro p h y s ics
Peter V. Foukal Solar Ast ro p h y s ics Second, Revised Edition WI LEY- VCH WILEY-VCH Verlag Co. KCaA Contents Preface 1 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2 2.1 2.1.1 2.1.2 2.2 2.2.1 2.2.2 2.2.3 2.3
SKINAKAS OBSERVATORY. Astronomy Projects for University Students PROJECT THE HERTZSPRUNG RUSSELL DIAGRAM
PROJECT 4 THE HERTZSPRUNG RUSSELL DIGRM Objective: The aim is to measure accurately the B and V magnitudes of several stars in the cluster, and plot them on a Colour Magnitude Diagram. The students will
Neutron Stars. How were neutron stars discovered? The first neutron star was discovered by 24-year-old graduate student Jocelyn Bell in 1967.
Neutron Stars How were neutron stars discovered? The first neutron star was discovered by 24-year-old graduate student Jocelyn Bell in 1967. Using a radio telescope she noticed regular pulses of radio
HL-A-3528H308W-S1-13. Description. Applications. Recommended Soldering. Package Dimensions
RoHS Specification Client Name: Client P/N: Factory P/N: HL-A-3528H308W-S1-13 OF-SMD3528WN Sending Date: Client approval Hong li approval Approval Audit Confirmation Approval Audit Confirmation 殷 小 平 王
Elliptical Galaxies. Galaxies and Their Properties, Part II: Fine Structure in E-Galaxies: A Signature of Recent Merging
Elliptical Galaxies Ay 21 - Lecture 12 Galaxies and Their Properties, Part II: Old view: ellipticals are boring, simple systems Ellipticals contain no gas & dust Ellipticals are composed of old stars Ellipticals
Lesson Plan G2 The Stars
Lesson Plan G2 The Stars Introduction We see the stars as tiny points of light in the sky. They may all look the same but they are not. They range in size, color, temperature, power, and life spans. In
Modeling Galaxy Formation
Galaxy Evolution is the study of how galaxies form and how they change over time. As was the case with we can not observe an individual galaxy evolve but we can observe different galaxies at various stages
Name: João Fernando Alves da Silva Class: 7-4 Number: 10
Name: João Fernando Alves da Silva Class: 7-4 Number: 10 What is the constitution of the Solar System? The Solar System is constituted not only by planets, which have satellites, but also by thousands
The Milky Way Galaxy is Heading for a Major Cosmic Collision
The Milky Way Galaxy is Heading for a Major Cosmic Collision Roeland van der Marel (STScI) [based on work with a team of collaborators reported in the Astrophysical Journal July 2012] Hubble Science Briefing