The Physics of Stellar Collapse (and GR Hydrodynamics)
|
|
|
- Delilah Owen
- 8 years ago
- Views:
Transcription
1 The Physics of Stellar Collapse (and GR Hydrodynamics) Christian David Ott California Institute of Technology C. D. Ott - The Physics of Stellar Collapse
2 Outline Outline Part 1 (a not so big picture overview) Core- Collapse Supernova Basics The Supernova Problem & Supernova Mechanisms Part 2 GR hydrodynamics GRHydro, the Einstein Toolkit 3D hydro code. GR1D C. D. Ott - The Physics of Stellar Collapse 2
3 For more details... H. Bethe, Supernova mechanisms, Rev. Mod. Phys. 62:4, 1990 H.- T. Janka, Conditions for shock revival by neutrino heating in core- collapse supernovae, A & A, 368:527, 2001 H.- T. Janka et al., Theory of core- collapse supernovae, Physics Reports 442, 38 C. D. Ott - The Physics of Stellar Collapse 3
4 Betelgeuse as seen by the HST, D 200 pc Rigel, D 240 pc
5 Supernova Explosion Betelgeuse as seen by the HST, D 200 pc Rigel, D 240 pc SN1987A, LMC, D 51.4 kpc Progenitor: BSG Sanduleak a, 18 M SUN
6 Core- Collapse Supernova Rates Local group of galaxies: V 30 Mpc 3 Milky Way, Andromeda (M31), Triangulum (M33) + 30 small galaxies/satellite galaxies (incl. SMC & LMC). Compiled from long list of references, e.g. Cappellaro et al., den Bergh & Tammann. Local group: worst case 1 SN in 90 years, best case 1 SN in 20 years. Most local group events with 100 kpc from Earth. Next jump in rate around M82 at 3.5 Mpc. C. D. Ott - The Physics of Stellar Collapse 6
7 Core- Collapse Supernova Ratees Ando et al C. D. Ott - The Physics of Stellar Collapse 7
8 Massive Stars and Their Evolution Mass: 7 M SUN 130 M SUN. Nuclear Burning: H - > He - > C/O - > O/Ne/Mg - > Si - > Fe M < 7 M SUN Envelope ejection C- O White Dwarf 7 M SUN < M < 10 M SUN M > 10 M SUN O- Ne White Dwarf Key parameters controlling stellar evolution: Mass Metallicity Binary Interactions Rotation (Red Super- giant ) C. D. Ott - The Physics of Stellar Collapse 8
9 The End of Nuclear Fusion exoergic endoergic C. D. Ott - The Physics of Stellar Collapse 9
10 Hydrostatics of the Iron Core and the Onset of Collapse Ions: Assume pure Fe 56 (not quite right, of course) Radiation pressure: c 10 g/cm 3 MeV Y e (in reality: T lower and Ye slightly lower) Electrons: degenerate and relativistic C. D. Ott - The Physics of Stellar Collapse 10
11 Chandrasekhar Mass Maximum mass for a relativistically degenerate object: + GR, thermal, and other corrections. (at Y e = > M Ch 1.45 M Sun ) M Ch - > radial instability - > collapse Two ways to get there: c 10 g/cm 3 MeV Y e (in reality: T lower and Ye slightly lower) (1) Silicon shell burning adding mass to the core. (2) Reduction of Y e. - > electron capture C. D. Ott - The Physics of Stellar Collapse 11
12 Electron Capture Simplest case: Capture on free protons, neutrinos escape capture if At zero T, non- degenerate nucleons: In core collapse: Capture typically at e >10 MeV - > excess energy given to. Capture rates: (see, e.g., Bethe et al. 1979, Bethe 1990, Burrows, Reddy & Thompson 2006) Complications: Capture on nuclei more complicated; can be blocked due to neutron shells filling up. Pauli blocking of low- energy states, since neutrinos C. D. Ott - The Physics of Stellar Collapse 12
13 Collapse C. D. Ott - The Physics of Stellar Collapse 13
14 More Collapse Physics In collapse, pressure support is reduced by Photodissociation of heavy nuclei: 125 MeV/reaction Electron Capture Neutrinos stream off almost freely at densities below g/cm 3. - deleptonizes Net entropy change is small, - > collapse proceeds practically adiabatically. C. D. Ott - The Physics of Stellar Collapse 14
15 More Collapse Physics: Deleptonization Liebendörfer 2005 Y e C. D. Ott - The Physics of Stellar Collapse 15
16 Stellar Collapse: Neutrino Trapping Neutrino Trapping Collapse phase: Neutrino opacity dominated by coherent neutrino- nucleus scattering: Neutrino mean- free path: For 3 x g/cm 3, diffusion time diff >> time between collisions coll - > neutrinos become trapped in the collapsing core. Consequences: Deleptonization stopped Beta Equilibrium Detailed simulations: C. D. Ott - The Physics of Stellar Collapse 16
17 Collapse still collapsing... C. D. Ott - The Physics of Stellar Collapse 17
18 Stellar Collapse: Self Similarity Self- Similarity in Stellar Collapse Schematic View of Spherical Collapse Analytic similarity solutions: Goldreich & Weber 1980 Yahil & Lattimer 1982 Yahil 1983 Separation into homologously (v r) collapsing inner core and supersonically collapsing outer core. C. D. Ott - The Physics of Stellar Collapse 18
19 Collapse Still collapsing... is there an end? C. D. Ott - The Physics of Stellar Collapse 19
20 Nuclear EOS The Nuclear Equation of State (EOS) Nuclear Statistical Equilibrium ( > 10 7 g/cm 3, T > 0.5 MeV) - > P = P(,T,Y e ) C. D. Ott - The Physics of Stellar Collapse 20
21 Nuclear EOS The Nuclear Equation of State (EOS) Nuclear Statistical Equilibrium ( > 10 7 g/cm 3, T > 0.5 MeV) - > P = P(,T,Y e ) C. D. Ott - The Physics of Stellar Collapse 21
22 Nuclear EOS The Nuclear Equation of State (EOS) Nuclear Statistical Equilibrium ( > 10 7 g/cm 3, T > 0.5 MeV) - > P = P(,T,Y e ) Something happens near g/cm 3! C. D. Ott - The Physics of Stellar Collapse 22
23 Nuclear EOS The Nuclear Equation of State (EOS) Nuclear Physics: Nuclear Density: recall: of the EOS C. D. Ott - The Physics of Stellar Collapse 23
24 Nuclear EOS Nuclear EOS: What happens near nuc? Nuclear Physics: Nuclear Density: pure nucleons nucleons, alphas, nuclei recall: of the EOS nuc n,p are so close in and leads to the stiffening of the EOS Phase transition from inhomogeneous to homogeneous nuclear matter C. D. Ott - The Physics of Stellar Collapse 24
25 Core Bounce nuclear density. 2.2 M SUN M = M CH,0 + corrections (thermal, GR, etc.) C. D. Ott - The Physics of Stellar Collapse 25
26 Stellar Collapse: Nuclear EOS Collapse and Bounce Inner Core reaches nuc into still infalling outer core. C. D. Ott - The Physics of Stellar Collapse 26
27 Core Bounce and Shock Formation C. D. Ott - The Physics of Stellar Collapse 27
28 Stellar Collapse: Bounce Shock Formation Credit: E. Müller Saas- Fee Lectures 1998 Inner Core Stiffening of EOS leads to sound wave that propagates through the inner core and steepens to a shock at the sonic point. C. D. Ott - The Physics of Stellar Collapse 28
29 Stellar Collapse: Universality of Collapse Universality of Core Collapse M ic Credit: E. Müller Saas- Fee Lectures 1998 Inner Core M ic (Y lep ) 2 + GR correction (- ) + thermal correction (+) + rotation (+) The Mass M ic of the inner core at bounce is determined by nuclear physics and weak interactions, is 0.5 M SUN, and is practically independent of progenitor star mass and structure. C. D. Ott - The Physics of Stellar Collapse 29
30 Stellar Collapse: Inner Core Mass Why worry about M ic? Bethe 1990!!! M ic is the amount of matter dynamically relevant in bounce. M ic sets kinetic energy imparted to the shock. M ic (and IC radius) sets the angular momentum that can be dynamically relevant. Sets mass cut for material that the shock needs to go through. M ic M ic 0.5 M SUN can easily stabilized by nuclear EOS. M ic sets the mass that must be accreted (before explosion?) to make a canonical 1.4 M SUN neutron star. C. D. Ott - The Physics of Stellar Collapse 30
31 Stellar Collapse: Getting into trouble The Supernova Problem Movie by Radius (km) C. D. Ott - The Physics of Stellar Collapse 31
32 Stellar Collapse: Getting into trouble. Why Does the Shock Stall Shock loses energy to: Dissociation of infalling heavy nuclei: 8.8 MeV/baryon Neutrinos that stream away from behind the shock. Inner core - > Core of the proto- neutron star (PNS) Janka et al C. D. Ott - The Physics of Stellar Collapse 32
33 Stellar Collapse: Neutrinos Neutrino Burst Optical depth Neutrinosphere: Depends on ( ) 2 Postbounce neutrino burst: Release of neutrinos created by e - capture on free protons in shocked region when e neutrinospheres. Trapping Thompson et al C. D. Ott - The Physics of Stellar Collapse 33
34 Stellar Collapse: Neutrinos, Neutrinos, Neutrinos Postbounce Neutrino Emission Thompson et al Neutrinos and Anti- neutrinos of ALL species: - current Emission: Pair processes: hot & dense environment needed Accretion luminosity and diffusive luminosity. C. D. Ott - The Physics of Stellar Collapse 34
35 Stellar Collapse: The Quantitative Picture Rough Supernova Energetics Supernova problem: What revives the shock? Precollapse iron core gravitational energy: Binding energy of a cold 1.5 M SUN NS, R=12.5 km - > Energy Reservoir Initial shock energy: Dissociation: (Shock formation at 0.55 M SUN, v 0.05 c ) M SUN. Neutrinos: initially up to Binding energy of the mantle (12- M SUN star): - > need multiple Bethes to blow up the star! C. D. Ott - The Physics of Stellar Collapse 35
36 The General Picture C. D. Ott - The Physics of Stellar Collapse 36
37 The General Picture C. D. Ott - The Physics of Stellar Collapse 37
38 The General Picture C. D. Ott - The Physics of Stellar Collapse 38
39 The General Picture The Supernova Problem What is the Mechanism of shock revival? C. D. Ott - The Physics of Stellar Collapse 39
40 Stellar Collapse: Supernova Mechanims The Essence of any Supernova Mechanism Collapse to neutron star: 3 x erg = 300 Bethe [B] gravitational energy erg = 1 B kinetic and internal energy of the ejecta. (Extreme cases: hypernova 99% of the energy is radiated as neutrinos over hundreds of seconds as the protoneutron star (PNS) cools. Explosion mechanism must tap the gravitational energy reservoir and convert the necessary fraction into energy of the explosion. C. D. Ott - The Physics of Stellar Collapse 40
41 Understanding Core- Collapse Supernovae Fully coupled! Core- Collapse Supernova Models Magneto- Hydrodynamics / Plasma Physics General Relativity Nuclear and Neutrino Physics Transport Theory C. D. Ott - The Physics of Stellar Collapse 41 C. D. Hanse 2011, 2011/07/20 Dynamics of the stellar fluid. Gravity Nuclear EOS, nuclear reactions & interactions. Neutrino transport. Additional Complication: The Multi- D Nature of the Beast Rotation, fluid instabilities (convection, turbulence, advective- acoustic, rotational), MHD dynamos, precollapse multi- D perturbations. - > Need multi- D (ideally 3D) treatment. Route of Attack: Computational Modeling Colgate & White, Arnett, Wilson Best current simulations still 1D. Good 2D Models (with various approximations [Gravity/Transport]). First 3D Models.
42 Stellar Collapse: Supernova Mechansims Supernova Mechanism: First Simulations Stirling Colgate Dave Arnett Hans Bethe Jim Wilson Colgate & White 1966 Arnett 1966 Bethe & Wilson 1985 No supercomputers yet (Cray- I only in 1976!): Limited to spherical symmetry, low resolution, poor neutrino transport. Nevertheless: Very important discovery - > Energy deposition by neutrinos may revive/drive the shock. C. D. Ott - The Physics of Stellar Collapse 42
43 Stellar Collapse: Supernova Mechansims Neutrino cooling: Neutrino heating: The Neutrino Mechanism Neutrino- driven mechanism: Based on subtle imbalance between neutrino heating and cooling in postshock region. Gain Radius [Ott et al. 2008] C. D. Ott - The Physics of Stellar Collapse 43
44 Stellar Collapse: Neutrino Mechanism A few Words on Neutrino Transport 6D problem: 3D space, 3D (,, ) momentum space. Limiting cases easy to handle: (1) Diffusion (isotropic radiation field) (2) Free streaming - 30 km 60 km 120 km 240 km C. D. Ott - The Physics of Stellar Collapse 44
45 Stellar Collapse: Neutrino Mechanism Neutrino Transport in Core- Collapse SNe Main complication: Need to track radiation field from complete isotropy to full free streaming over many orders of magnitude of. Neutrino heating depends on details of the radiation field: Inverse Flux factor: C. D. Ott - The Physics of Stellar Collapse 45
46 Stellar Collapse: Neutrino Mechanism Yes! BUT: Only for lowest- mass massive stars. (Kitaura et al. 2006, Burrows 1988, Burrows, Livne, Dessart 2007) FAILS in spherical symmetry (1D) for garden- variety massive stars ( 15 M SUN ) in simulations with best neutrino physics and neutrino transport Does it work? 8.8 M SUN progenitor Kitaura et al C. D. Ott - The Physics of Stellar Collapse 46
47 Stellar Collapse: Neutrino Mechanism Failure of the Neutrino Mechanism in 1D Marek & Janka 2009 C. D. Ott - The Physics of Stellar Collapse 47
48 Stellar Collapse: Neutrino Mechanism Anyway... What next? Why does the neutrino mechanism fail in 1D? Is dimensionality an issue? What is 1D missing? Rotation and magnetohydrodynamics (MHD) Convection/Turbulence Other multi- D processes; e.g., pulsations First multi- D radiation- hydrodynamics simulations: early to mid 1990s: Herant et al. 1994, Burrows et al. 1995, Janka & Müller C. D. Ott - The Physics of Stellar Collapse 48
49 A Look at the Beast: [Ott et al. 2008, Ott 2009 b] [Ott et al. 2008] C. D. NAOJ Mitaka, Tokyo 2009/05/24 49
50 Convection Convection Ledoux criterion for instability: Entropy Gradient C L > 0 - > convective instability. Postbounce supernova cores: < 0 < 0 Negative entropy gradient in postshock region - > convection Negative entropy region inside the neutrinosphere in the PNS - > convection Important effect of convection: Lepton Gradient region is increased - > leads to more favorable ratio advect / heat. (alternative interpretation: Pejcha C. D. Ott - The Physics of Stellar Collapse 50
51 SASI Standing Accretion Shock Instability [Blondin Foglizzo Advective- acoustic cycle drives shock instability. Seen in simulations by all groups! C. D. Ott - The Physics of Stellar Collapse 51
52 1D - > 2D 1D - > 2D Simple analytic/ode model of Burrows & Goshy Luminosity required to explode at given accretion rate. C. D. Ott - The Physics of Stellar Collapse 52
53 Status of the Neutrino Mechanism Status of the Neutrino Mechanism Best simulations are still in 2D. Things look better in 2D, some models explode under special circumstances. No robust explosions. Crucial conditions (?): General relativity Soft nuclear EOS Robust explosions in 3D? Marek & Janka 2009 C. D. Ott - The Physics of Stellar Collapse 53
54 First 3D Simulations Nordhaus, Burrows, Almgren, Bell D/2D/3D simulations with the CASTRO code. H. Shen EOS, Simple neutrino cooling/heating treatment, 1D gravity. C. D. Ott - The Physics of Stellar Collapse 54
55 First 3D Simulations Nordhaus, Burrows, Almgren, Bell D/2D/3D simulations with the CASTRO code. H. Shen EOS, Simple neutrino cooling/heating treatment, 1D gravity. C. D. Ott - The Physics of Stellar Collapse 55
56 First 3D Simulations Nordhaus, Burrows, Almgren, Bell D/2D/3D simulations with the CASTRO code. H. Shen EOS, Simple neutrino cooling/heating treatment, 1D gravity. C. D. Ott - The Physics of Stellar Collapse 56
57 First 3D Simulations Hanke, Janka, Müller et al. in prep. Repeated Nordhaus et al. study Results inconsistent. Why? C. D. Ott - The Physics of Stellar Collapse 57
58 Alternatives Alternatives to the Neutrino Mechanism Magnetorotational Mechanism [LeBlanc & Wilson 1970, Bisnovatyi- Kogan et al. 1976, Meier et al. 1976, Symbalisty 1984] Acoustic Mechanism [proposed by Burrows et al. 2006, 2007; not (yet?) confirmed by other groups/codes] C. D. Ott - The Physics of Stellar Collapse 58
59 Alternatives Alternatives to the Neutrino Mechanism Magnetorotational Mechanism [LeBlanc & Wilson 1970, Bisnovatyi- Kogan et al. 1976, Meier et al. 1976, Symbalisty 1984] Acoustic Mechanism [proposed by Burrows et al. 2006, 2007; not (yet?) confirmed by other groups/codes] C. D. Ott - The Physics of Stellar Collapse 59
60 MHD- driven Explosions [e.g., Burrows et al. 2007, Dessart et al. 2008, Kotake et al. 2004, Yamada & Sawai 2004, Sawai et al. 2008, Takiwaki et al. 2009] Rapid rotation: P 0 < 4-6 s - > millisecond PNS PNS rotational energy: 10 B Amplification of B fields up to equipartition: compression dynamos magneto- rotational instability (MRI) Jet- driven outflows. MHD- driven explosion may be GRB precursor. VULCAN 2D R- MHD code, Livne et al. 2007, Burrows et al
61 MHD jet/explosion launched when P mag / P gas 1 61
62 Alternatives Features/Limitations of the Magnetorotational Mechanism [Burrows et al. 2007] Jet powers up to 10 B/s (10 52 erg/s). Simultaneous explosion and accretion. Hypernova energies (> 10 B) attainable. MHD mechanism inefficient for cores with precollapse P 0 > 4 s, but stellar evolution + NS birth spin estimates: P 0 > 30 s in most cores. MHD explosion a GRB precursor? [Heger et al. 2005, Ott et al. 2006] Limitations: Resolution does not allow to capture Magnetorotational Instability; Simulations 2D and Newtonian. C. D. Ott - The Physics of Stellar Collapse 62
63 Alternatives Alternatives to the Neutrino Mechanism Magnetorotational Mechanism [LeBlanc & Wilson 1970, Bisnovatyi- Kogan et al. 1976, Meier et al. 1976, Symbalisty 1984] Acoustic Mechanism [proposed by Burrows et al. 2006, 2007; not (yet?) confirmed by other groups/codes] C. D. Ott - The Physics of Stellar Collapse 63
64 Alternatives: The Acoustic Mechanism SASI- modulated supersonic accretion streams and SASI generated turbulence excite lowest- order (l=1) g- mode in the PNS. f 300 Hz. g- modes reach large amplitudes 500 ms 1 s after bounce. Damping by strong sound waves that steepen into shocks; deposit energy in the stalled shock. 1 B explosions at late times. (1) hard to simulate; unconfirmed, (2) possible parametric instability, limiting mode amplitudes (Weinberg & Quataert C. D. Ott - The Physics of Stellar Collapse 64
65 Summary Summary and Take- Home Messages (Part I) Core- Collapse Supernovae are Gravity Bombs. CCSNe are the most energetic explosive events in the universe. CCSNe are rare events in the local group of galaxies. The Core- Collapse Supernova Problem: The shock always stalls and must be revived. There are multiple possible supernova mechanisms: Neutrino, magnetorotational, and acoustic mechanism. What I did not talk about: CCSN postbounce dynamics can be observed directly in neutrinos and gravitational waves! - > next galactic CCSN will provide answers. C. D. Ott - The Physics of Stellar Collapse 65
66 I like things that explode nukes, supernovae, and orgasms attributed to Stirling Colgate C. D. Ott - The Physics of Stellar Collapse
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,
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
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
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
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
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
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
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
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
Solar Energy Production
Solar Energy Production We re now ready to address the very important question: What makes the Sun shine? Why is this such an important topic in astronomy? As humans, we see in the visible part of the
White Dwarf Properties and the Degenerate Electron Gas
White Dwarf Properties and the Degenerate Electron Gas Nicholas Rowell April 10, 2008 Contents 1 Introduction 2 1.1 Discovery....................................... 2 1.2 Survey Techniques..................................
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
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
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
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,
Low- and high-energy neutrinos from gamma-ray bursts
Low- and high-energy neutrinos from gamma-ray bursts Hylke B.J. Koers Low- and high-energy neutrinos from gamma-ray bursts Hylke B.J. Koers HK and Ralph Wijers, MNRAS 364 (2005), 934 (astro-ph/0505533)
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
Constraints on the explosion mechanism and progenitors of Type Ia supernovae
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
The Layout of the Solar System
The Layout of the Solar System Planets fall into two main categories Terrestrial (i.e. Earth-like) Jovian (i.e. Jupiter-like or gaseous) [~5000 kg/m 3 ] [~1300 kg/m 3 ] What is density? Average density
Nuclear Physics. Nuclear Physics comprises the study of:
Nuclear Physics Nuclear Physics comprises the study of: The general properties of nuclei The particles contained in the nucleus The interaction between these particles Radioactivity and nuclear reactions
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
Main sequence stars. Haris Ðapo. Antalya Lecture 3. 1 Akdeniz University, Antalya
Main sequence stars Haris Ðapo 1 Akdeniz University, Antalya Antalya Lecture 3. Haris Ðapo (Akdeniz University) Main sequence stars Main sequence stars 1 / 22 Outline 1 Introduction 2 Hydrogen burning
The Sun and Solar Energy
I The Sun and Solar Energy One of the most important forces behind global change on Earth is over 90 million miles distant from the planet. The Sun is the ultimate, original source of the energy that drives
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
Hydrodynamics of stellar explosions
Some basic hydrodynamics The art of CFD Hydrodynamic challenges in stellar explosions Hydrodynamics of stellar explosions General: Literature L.D.Landau & E.M.Lifshitz, Fluid Mechanics, Pergamon (1959)
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
Basic Nuclear Concepts
Section 7: In this section, we present a basic description of atomic nuclei, the stored energy contained within them, their occurrence and stability Basic Nuclear Concepts EARLY DISCOVERIES [see also Section
Supernova. Author: Alex Nervosa. Essay Supervisor: Brad Gibson, HET611 Swinburne Astronomy Online
Supernova Author: Alex Nervosa Essay Supervisor: Brad Gibson, HET611 Swinburne Astronomy Online Introduction A supernova (SNa) is a stellar cataclysmic explosion which occurs at the end of a star s life.
The Physics of Neutron Stars
The Physics of Neutron Stars Alfred Whitehead Physics 518, Fall 009 The Problem Describe how a white dwarf evolves into a neutron star. Compute the neutron degeneracy pressure and balance the gravitational
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
Lecture 7 Formation of the Solar System. Nebular Theory. Origin of the Solar System. Origin of the Solar System. The Solar Nebula
Origin of the Solar System Lecture 7 Formation of the Solar System Reading: Chapter 9 Quiz#2 Today: Lecture 60 minutes, then quiz 20 minutes. Homework#1 will be returned on Thursday. Our theory must explain
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
JINA AT UNIVERSITY OF CHICAGO
Jim Truran Astronomy and Astrophysics Enrico Fermi Institute ASC Center for Astrophysical Thermonuclear Flashes University of Chicago JINA Advisory Committee Meeting University of Notre Dame April 30,
Name Class Date. true
Exercises 131 The Falling Apple (page 233) 1 Describe the legend of Newton s discovery that gravity extends throughout the universe According to legend, Newton saw an apple fall from a tree and realized
L3: The formation of the Solar System
credit: NASA L3: The formation of the Solar System UCL Certificate of astronomy Dr. Ingo Waldmann A stable home The presence of life forms elsewhere in the Universe requires a stable environment where
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/
Sound. References: L.D. Landau & E.M. Lifshitz: Fluid Mechanics, Chapter VIII F. Shu: The Physics of Astrophysics, Vol. 2, Gas Dynamics, Chapter 8
References: Sound L.D. Landau & E.M. Lifshitz: Fluid Mechanics, Chapter VIII F. Shu: The Physics of Astrophysics, Vol., Gas Dynamics, Chapter 8 1 Speed of sound The phenomenon of sound waves is one that
The Birth of the Universe Newcomer Academy High School Visualization One
The Birth of the Universe Newcomer Academy High School Visualization One Chapter Topic Key Points of Discussion Notes & Vocabulary 1 Birth of The Big Bang Theory Activity 4A the How and when did the universe
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
The Evolution of GMCs in Global Galaxy Simulations
The Evolution of GMCs in Global Galaxy Simulations image from Britton Smith Elizabeth Tasker (CITA NF @ McMaster) Jonathan Tan (U. Florida) Simulation properties We use the AMR code, Enzo, to model a 3D
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
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
Lesson 3: Isothermal Hydrostatic Spheres. B68: a self-gravitating stable cloud. Hydrostatic self-gravitating spheres. P = "kt 2.
Lesson 3: Isothermal Hydrostatic Spheres B68: a self-gravitating stable cloud Bok Globule Relatively isolated, hence not many external disturbances Though not main mode of star formation, their isolation
Carol and Charles see their pencils fall exactly straight down.
Section 24-1 1. Carol is in a railroad car on a train moving west along a straight stretch of track at a constant speed of 120 km/h, and Charles is in a railroad car on a train at rest on a siding along
Pablo Laguna Center for Relativistic Astrophysics School of Physics Georgia Tech, Atlanta, USA
Pablo Laguna Center for Relativistic Astrophysics School of Physics Georgia Tech, Atlanta, USA The Transient Sky SN, GRBs, AGN or TDEs? Arcavi et al. 2014, ApJ, 793, 38 van Velzen et al. 2011, ApJ, 741,
Specific Intensity. I ν =
Specific Intensity Initial question: A number of active galactic nuclei display jets, that is, long, nearly linear, structures that can extend for hundreds of kiloparsecs. Many have two oppositely-directed
Build Your Own Universe
Build Your Own Universe You will need: At least 10,000,000,000,000,00 0,000,000,000,000,000,000,00 0,000,000,000,000,000,000,00 0,000,000,000,000,000,000,00 0,000 x Down quarks At least 10,000,000,000,000,000,
Science Standard 4 Earth in Space Grade Level Expectations
Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal
Nuclear Physics and Radioactivity
Nuclear Physics and Radioactivity 1. The number of electrons in an atom of atomic number Z and mass number A is 1) A 2) Z 3) A+Z 4) A-Z 2. The repulsive force between the positively charged protons does
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
Solar System Fundamentals. What is a Planet? Planetary orbits Planetary temperatures Planetary Atmospheres Origin of the Solar System
Solar System Fundamentals What is a Planet? Planetary orbits Planetary temperatures Planetary Atmospheres Origin of the Solar System Properties of Planets What is a planet? Defined finally in August 2006!
MASTER OF SCIENCE IN PHYSICS MASTER OF SCIENCES IN PHYSICS (MS PHYS) (LIST OF COURSES BY SEMESTER, THESIS OPTION)
MASTER OF SCIENCE IN PHYSICS Admission Requirements 1. Possession of a BS degree from a reputable institution or, for non-physics majors, a GPA of 2.5 or better in at least 15 units in the following advanced
Ay 122 - Fall 2004. The Sun. And The Birth of Neutrino Astronomy. This printout: Many pictures missing, in order to keep the file size reasonable
Ay 122 - Fall 2004 The Sun And The Birth of Neutrino Astronomy This printout: Many pictures missing, in order to keep the file size reasonable Why Study the Sun? The nearest star - can study it in a greater
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
Fridolin Weber San Diego State University San Diego, California USA
Fridolin Weber San Diego State University San Diego, California USA IAU Symposium 291 Neutron Stars and Pulsars: Challenges and OpportuniEes afer 80 years IAU General Assembly XXVIII 20-31 August 2012,
Chapter 9 Summary and outlook
Chapter 9 Summary and outlook This thesis aimed to address two problems of plasma astrophysics: how are cosmic plasmas isotropized (A 1), and why does the equipartition of the magnetic field energy density
Institut für Kern- und Teilchenphysik Neutrinos & Cosmology
Neutrinos & Cosmology 1 Cosmology: WHY??? From laboratory experiment limits can be set ONLY in neutrino mass difference No information if neutrino masses are degenerated From kinematic experiment limits
The Main Point. Lecture #34: Solar System Origin II. Chemical Condensation ( Lewis ) Model. How did the solar system form? Reading: Chapter 8.
Lecture #34: Solar System Origin II How did the solar system form? Chemical Condensation ("Lewis") Model. Formation of the Terrestrial Planets. Formation of the Giant Planets. Planetary Evolution. Reading:
Wave-particle and wave-wave interactions in the Solar Wind: simulations and observations
Wave-particle and wave-wave interactions in the Solar Wind: simulations and observations Lorenzo Matteini University of Florence, Italy In collaboration with Petr Hellinger, Simone Landi, and Marco Velli
Topic 3. Evidence for the Big Bang
Topic 3 Primordial nucleosynthesis Evidence for the Big Bang! Back in the 1920s it was generally thought that the Universe was infinite! However a number of experimental observations started to question
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
Solar Wind: Theory. Parker s solar wind theory
Solar Wind: Theory The supersonic outflow of electrically charged particles, mainly electrons and protons from the solar CORONA, is called the SOLAR WIND. The solar wind was described theoretically by
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
Coronal expansion and solar wind
Coronal expansion and solar wind The solar corona over the solar cycle Coronal and interplanetary temperatures Coronal expansion and solar wind acceleration Origin of solar wind in magnetic network Multi-fluid
Masses in Atomic Units
Nuclear Composition - the forces binding protons and neutrons in the nucleus are much stronger (binding energy of MeV) than the forces binding electrons to the atom (binding energy of ev) - the constituents
= = 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
Why Does the Sun Shine?
Why Does the Sun Shine? Is the Sun on Fire? Fire (oxidation) produces light and heat, just like the Sun. Source: chemical potential energy Suppose the Sun were made of carbon and oxygen. The Sun could
Steady Heat Conduction
Steady Heat Conduction In thermodynamics, we considered the amount of heat transfer as a system undergoes a process from one equilibrium state to another. hermodynamics gives no indication of how long
In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees.
In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees. A panoramic painting of the Milky Way as seen from Earth, done by Knut Lundmark in the 1940 s. The
Gravitational instabilities in protostellar discs and the formation of planetesimals
Gravitational instabilities in protostellar discs and the formation of planetesimals Giuseppe Lodato - Università degli Studi di Milano 17 February 2011 - Bologna Gravitational instabilities in protostellar
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,
The Birth and Assembly of Galaxies: the Relationship Between Science Capabilities and Telescope Aperture
The Birth and Assembly of Galaxies: the Relationship Between Science Capabilities and Telescope Aperture Betsy Barton Center for Cosmology University of California, Irvine Grateful acknowledgements to:
Comparison of approximations to the transition rate in the DDHMS preequilibrium model
EPJ Web of Conferences 69, 0 00 24 (204) DOI: 0.05/ epjconf/ 2046900024 C Owned by the authors, published by EDP Sciences, 204 Comparison of approximations to the transition rate in the DDHMS preequilibrium
Mass transfer dynamics in white dwarf binary systems
Mass transfer dynamics in white dwarf binary systems In collaboration with: Stephan Rosswog & Marcus Brüggen EUROWD10, Tübingen, 2010 Numbers on Galactic WDs total number of WDs: 10 10 Napiwotzki (2009)
Elliptical Galaxies. Old view: ellipticals are boring, simple systems
Eliptical Galaxies Elliptical Galaxies Old view: ellipticals are boring, simple systems Ellipticals contain no gas & dust Ellipticals are composed of old stars Ellipticals formed in a monolithic collapse,
Summary: Four Major Features of our Solar System
Summary: Four Major Features of our Solar System How did the solar system form? According to the nebular theory, our solar system formed from the gravitational collapse of a giant cloud of interstellar
Indiana's Academic Standards 2010 ICP Indiana's Academic Standards 2016 ICP. map) that describe the relationship acceleration, velocity and distance.
.1.1 Measure the motion of objects to understand.1.1 Develop graphical, the relationships among distance, velocity and mathematical, and pictorial acceleration. Develop deeper understanding through representations
Chapter NP-5. Nuclear Physics. Nuclear Reactions TABLE OF CONTENTS INTRODUCTION OBJECTIVES 1.0 NUCLEAR REACTIONS 2.0 NEUTRON INTERACTIONS
Chapter NP-5 Nuclear Physics Nuclear Reactions TABLE OF CONTENTS INTRODUCTION OBJECTIVES 1.0 2.0 NEUTRON INTERACTIONS 2.1 ELASTIC SCATTERING 2.2 INELASTIC SCATTERING 2.3 RADIATIVE CAPTURE 2.4 PARTICLE
This paper is also taken for the relevant Examination for the Associateship. For Second Year Physics Students Wednesday, 4th June 2008: 14:00 to 16:00
Imperial College London BSc/MSci EXAMINATION June 2008 This paper is also taken for the relevant Examination for the Associateship SUN, STARS, PLANETS For Second Year Physics Students Wednesday, 4th June
Basic Concepts in Nuclear Physics
Basic Concepts in Nuclear Physics Paolo Finelli Corso di Teoria delle Forze Nucleari 2011 Literature/Bibliography Some useful texts are available at the Library: Wong, Nuclear Physics Krane, Introductory
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
Lecture 10 Formation of the Solar System January 6c, 2014
1 Lecture 10 Formation of the Solar System January 6c, 2014 2 Orbits of the Planets 3 Clues for the Formation of the SS All planets orbit in roughly the same plane about the Sun. All planets orbit in the
A i A i. µ(ion) = Z i X i
Lecture 2 Review: calculation of mean atomic weight of an ionized gas (µ) Given a mass fraction X i (or abundance) for an ionic (or atomic) species with atomic weight A i, we can can calculate µ by: For
Coronal Heating Problem
Mani Chandra Arnab Dhabal Raziman T V PHY690C Course Project Indian Institute of Technology Kanpur Outline 1 2 3 Source of the energy Mechanism of energy dissipation Proposed mechanisms Regions of the
X-ray Emission from Elliptical Galaxies
The Nature of Elliptical Galaxies, Proceedings of the Second Stromlo Symposium, Eds. M. Arnaboldi, G.S. Da Costa & P. Saha X-ray Emission from Elliptical Galaxies Craig L. Sarazin Department of Astronomy,
YSO Orion Molecular Cloud Aims Of Stahler & Bakk.N.R.T.P.R.T.T.
Protobinaries von Cornelia Weber, Bakk.rer.nat. Overview Motivation Molecular Clouds Young Stellar Objects Multiplicity of YSO Orion Molecular Cloud Aims of my thesis Motivation Binary and Multiple system
Part 1 Composition of Earth Composition of solar system Origin of the elements Part 2 Geochronometry: Age of Earth Formation of Earth and Moon.
Part 1 Composition of Earth Composition of solar system Origin of the elements Part 2 Geochronometry: Age of Earth Formation of Earth and Moon. Differentiation of core and mantle. Isotope tracing: sequence
Chapter 8 Formation of the Solar System. What theory best explains the features of our solar system? Close Encounter Hypothesis
Chapter 8 Formation of the Solar System What properties of our solar system must a formation theory explain? 1. Patterns of motion of the large bodies Orbit in same direction and plane 2. Existence of
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:
UNIT V. Earth and Space. Earth and the Solar System
UNIT V Earth and Space Chapter 9 Earth and the Solar System EARTH AND OTHER PLANETS A solar system contains planets, moons, and other objects that orbit around a star or the star system. The solar system
Gravitational wave group
ICRR Review @Kashiwa 19-20, October 2006 Gravitational wave group Kazuaki Kuroda LCGT/CLIO/TAMA Collaboration Gravitational wave (GW) is the propagation of spacetime distortion predicted by Einstein s
Department of Physics University of Wisconsin-Milwaukee Phone: (414) 229-2590 E-mail: chang65@uwm.edu Milwaukee, WI 53201
Philip Chang Contact Information Education Department of Physics University of Wisconsin-Milwaukee Phone: (414) 229-2590 PO Box 413 E-mail: chang65@uwm.edu Milwaukee, WI 53201 University of California
Objectives 404 CHAPTER 9 RADIATION
Objectives Explain the difference between isotopes of the same element. Describe the force that holds nucleons together. Explain the relationship between mass and energy according to Einstein s theory
FXA 2008. UNIT G485 Module 5 5.5.1 Structure of the Universe. Δλ = v λ c CONTENTS OF THE UNIVERSE. Candidates should be able to :
1 Candidates should be able to : CONTENTS OF THE UNIVERSE Describe the principal contents of the universe, including stars, galaxies and radiation. Describe the solar system in terms of the Sun, planets,
Atomic Structure: Chapter Problems
Atomic Structure: Chapter Problems Bohr Model Class Work 1. Describe the nuclear model of the atom. 2. Explain the problems with the nuclear model of the atom. 3. According to Niels Bohr, what does n stand
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,
Chapter 8 Formation of the Solar System Agenda
Chapter 8 Formation of the Solar System Agenda Announce: Mercury Transit Part 2 of Projects due next Thursday Ch. 8 Formation of the Solar System Philip on The Physics of Star Trek Radiometric Dating Lab
1 A Solar System Is Born
CHAPTER 3 1 A Solar System Is Born SECTION Formation of the Solar System BEFORE YOU READ After you read this section, you should be able to answer these questions: What is a nebula? How did our solar system
Dinamica del Gas nelle Galassie II. Star formation
Dinamica del Gas nelle Galassie II. Star formation Overview on ISM Molecular clouds: composition and properties. Plasmas Charge neutrality, infinite conductivity; Field freezing; Euler equation with magnetic
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