18. Stellar Explosions
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The Birth of Stars and Planets
Unit 6: The Birth of Stars and Planets This material was developed by the Friends of the Dominion Astrophysical Observatory with the assistance of a Natural Science and Engineering Research Council PromoScience grant and the NRC. It is a part of a larger project to present grade-appropriate material that matches 2020 curriculum requirements to help students understand planets, with a focus on exoplanets. This material is aimed at BC Grade 6 students. French versions are available. Instructions for teachers ● For questions and to give feedback contact: Calvin Schmidt [email protected], ● All units build towards the Big Idea in the curriculum showing our solar system in the context of the Milky Way and the Universe, and provide background for understanding exoplanets. ● Look for Ideas for extending this section, Resources, and Review and discussion questions at the end of each topic in this Unit. These should give more background on each subject and spark further classroom ideas. We would be happy to help you expand on each topic and develop your own ideas for your students. Contact us at the [email protected]. Instructions for students ● If there are parts of this unit that you find confusing, please contact us at [email protected] for help. ● We recommend you do a few sections at a time. We have provided links to learn more about each topic. ● You don’t have to do the sections in order, but we recommend that. Do sections you find interesting first and come back and do more at another time. ● It is helpful to try the activities rather than just read them. -
Stellar Explosions
Chapter 11: Stellar Explosions Prof. Douglas Laurence AST 1002 What are Stellar Explosions? Stellar remnant, probably a neutron star. • When stars above a certain mass die (run out of fuel at their core), they will literally explode in novae, supernovae, or hypernovae • The explosions “blows away” some of the star, leaving a stellar remnant, which can be: • A white dwarf • A neutron star • Or a black hole Stellar and Remnants Masses • Stars with a (main sequence) mass < 8#⊙ will eventually become white dwarfs. • White dwarfs have a remnant mass < 1.4#⊙, known as the Chandrasekhar limit. • Stars with a mass < 25#⊙will eventually become neutron stars. • Neutron stars have a remnant mass < 3#⊙, known as the Tolman-Oppenheimer- Volkoff (TOV) limit. • Stars with mass > 25#⊙, or remnant mass > 3#⊙, become black holes. • What a star becomes is determined by the remnant mass; remnant masses trend with main sequence masses, but they’re the decider. • A star with a very large mass can have a dramatically lower remnant mass after a stellar explosion, if the explosion blows away much of the star’s mass. Novae and White Dwarfs • Very little mass is ejected by a nova, so it will not affect the type of stellar remnant left behind (which will invariably be a white dwarf.) • Novae can increase brightness by 10,000 times. • Some novae repeat themselves, becoming what are called recurrent novae. Mechanism of Nova Production • Novae occur in binary systems between a red giant and a white dwarf. • White dwarf is formed by planetary nebula. • Novae don’t produce white dwarfs. -
Metadata of the Chapter That Will Be Visualized Online
Metadata of the chapter that will be visualized online Chapter Title Binary Systems and Their Nuclear Explosions Copyright Year 2018 Copyright Holder The Author(s) Author Family Name Isern Particle Given Name Jordi Suffix Organization Institute of Space Sciences (ICE, CSIC) Address Barcelona, Spain Organization Institut d’Estudis Espacials de Catalunya (IEEC) Address Barcelona, Spain Email [email protected] Corresponding Author Family Name Hernanz Particle Given Name Margarita Suffix Organization Institute of Space Sciences (ICE, CSIC) Address Barcelona, Spain Organization Institut d’Estudis Espacials de Catalunya (IEEC) Address Barcelona, Spain Email [email protected] Author Family Name José Particle Given Name Jordi Suffix Organization Universitat Politècnica de Catalunya (UPC) Address Barcelona, Spain Organization Institut d’Estudis Espacials de Catalunya (IEEC) Address Barcelona, Spain Email [email protected] Abstract The nuclear energy supply of a typical star like the Sun would be ∼ 1052 erg if all the hydrogen could be incinerated into iron peak elements. Chapter 5 1 Binary Systems and Their Nuclear 2 Explosions 3 Jordi Isern, Margarita Hernanz, and Jordi José 4 5.1 Accretion onto Compact Objects and Thermonuclear 5 Runaways 6 The nuclear energy supply of a typical star like the Sun would be ∼1052 erg if all 7 the hydrogen could be incinerated into iron peak elements. Since the gravitational 8 binding energy is ∼1049 erg, it is evident that the nuclear energy content is more 9 than enough to blow up the Sun. However, stars are stable thanks to the fact that their 10 matter obeys the equation of state of a classical ideal gas that acts as a thermostat: if 11 some energy is released as a consequence of a thermal fluctuation, the gas expands, 12 the temperature drops and the instability is quenched. -
Fundamentals of Stellar Evolution Theory: Understanding the HRD
Fundamentals of Stellar Evolution Theory: Understanding the HRD By C E S A R E C H I O S I Department of Astronomy, University of Padua, Vicolo Osservatorio 5, 35122 Padua, Italy Published in: "Stellar Astrophysics for the Local Group: a First Step to the Universe" VIII Canary Islands Winter School Cambridge University Press 25 March, 1997 Abstract. We summarize the results of stellar evolution theory for single stars that have been obtained over the last two decades, and compare these results with the observations. We discuss in particular the effect of mass loss by stellar winds during the various evolutionary stages of stars that are affected by this phenomenon. In addition, we focus on the problem of mixing in stellar interiors calling attention on weak aspects of current formulations and presenting plausible alternatives. Finally, we survey some applications of stellar models to several areas of modern astrophysics. 1. Introduction The major goal of stellar evolution theory is the interpretation and reproduction of the Hertzsprung-Russell Diagram (HRD) of stars in different astrophysical environments: solar vicinity, star clusters of the Milky Way and nearby galaxies, fields in external galaxies. The HRD of star clusters, in virtue of the small spread in age and composition of the component stars, is the classical template to which stellar models are compared. If the sample of stars is properly chosen from the point of view of completeness, even the shortest lived evolutionary phases can be tested. The HRD of field stars, those in external galaxies in particular, contains much information on the past star formation history. -
How Supernovae Became the Basis of Observational Cosmology
Journal of Astronomical History and Heritage, 19(2), 203–215 (2016). HOW SUPERNOVAE BECAME THE BASIS OF OBSERVATIONAL COSMOLOGY Maria Victorovna Pruzhinskaya Laboratoire de Physique Corpusculaire, Université Clermont Auvergne, Université Blaise Pascal, CNRS/IN2P3, Clermont-Ferrand, France; and Sternberg Astronomical Institute of Lomonosov Moscow State University, 119991, Moscow, Universitetsky prospect 13, Russia. Email: [email protected] and Sergey Mikhailovich Lisakov Laboratoire Lagrange, UMR7293, Université Nice Sophia-Antipolis, Observatoire de la Côte d’Azur, Boulevard de l'Observatoire, CS 34229, Nice, France. Email: [email protected] Abstract: This paper is dedicated to the discovery of one of the most important relationships in supernova cosmology—the relation between the peak luminosity of Type Ia supernovae and their luminosity decline rate after maximum light. The history of this relationship is quite long and interesting. The relationship was independently discovered by the American statistician and astronomer Bert Woodard Rust and the Soviet astronomer Yury Pavlovich Pskovskii in the 1970s. Using a limited sample of Type I supernovae they were able to show that the brighter the supernova is, the slower its luminosity declines after maximum. Only with the appearance of CCD cameras could Mark Phillips re-inspect this relationship on a new level of accuracy using a better sample of supernovae. His investigations confirmed the idea proposed earlier by Rust and Pskovskii. Keywords: supernovae, Pskovskii, Rust 1 INTRODUCTION However, from the moment that Albert Einstein (1879–1955; Whittaker, 1955) introduced into the In 1998–1999 astronomers discovered the accel- equations of the General Theory of Relativity a erating expansion of the Universe through the cosmological constant until the discovery of the observations of very far standard candles (for accelerating expansion of the Universe, nearly a review see Lipunov and Chernin, 2012). -
Cosmic Times Teachers' Guide Table of Contents
Cosmic Times Teachers’ Guide Table of Contents Cosmic Times Teachers’ Guide ....................................................................................... 1 1919 Cosmic Times ........................................................................................................... 3 Summary of the 1919 Articles...................................................................................................4 Sun’s Gravity Bends Starlight .................................................................................................4 Sidebar: Why a Total Eclipse?.................................................................................................4 Mount Wilson Astronomer Estimates Milky Way Ten Times Bigger Than Thought ............4 Expanding or Contracting? ......................................................................................................4 In Their Own Words................................................................................................................4 Notes on the 1919 Articles .........................................................................................................5 Sun's Gravity Bends Starlight..................................................................................................5 Sidebar: Why a Total Eclipse?.................................................................................................7 Mount Wilson Astronomer Estimates Milky Way Ten Times Bigger Than Thought ............7 Expanding or Contracting? ......................................................................................................8 -
N-Body Techniques for Astrophysics: Lecture 4 – STARLAB
Michela Mapelli N-body techniques for astrophysics: Lecture 4 – STARLAB PhD School in Astrophysics, University of Padova November 19-30, 2018 Michela Mapelli N-body techniques for astrophysics: Lecture 4 – STARLAB MOST IMPORTANT INGREDIENT: stay calm, breath, don't panic, don't kill yourself, don't kill your office mates PhD School in Astrophysics, University of Padova November 19-30, 2018 OUTLINE: 1* definition and structure of starlab http://www.sns.ias.edu/~starlab/overview/ http://www.sns.ias.edu/~starlab/structure/ 2* the dynamics: KIRA http://www.sns.ias.edu/~starlab/kira/ 3* the stellar evolution: SEBA 4* the outputs http://www.sns.ias.edu/~starlab/internals/ 5* compilation and installation 6* writing initial conditions http://www.sns.ias.edu/~starlab/examples/ 7* running kira 8* visualize outputs 1) definition and structure of starlab http://www.sns.ias.edu/~starlab/ * Software environment: multiple codes to generate, evolve and analyze a collisional system (such as a star cluster) They can be combined * Tools to Monte Carlo generate initial conditions (e.g. makeplummer) Evolve stars and binaries via population synthesis (e.g. SeBa) Evolve collisional dynamics (e.g. kira) Analyze outputs (e.g. xstarplot) * Collisional dynamics is evolved through HERMITE SCHEME with block time steps: example of code adopting tools described in lecture 3 1) definition and structure of starlab http://www.sns.ias.edu/~starlab/structure/ - CLASS: description of structure+ its functions - an OBJECT belongs to a class if it is DEFINED as member of the class → star a; EACH PARTICLE + root belongs to the node class (include/node.h) class node { static node* root; // Global address of the root node. -
Ch 06-Phys--Star Death & H-R Di
Ch. 6--Stars and H-R Diagrams Chapter 6 THE LIFE AND DEATH OF A STAR, and THE H-R DIAGRAM A.) Hertzsprung-Russell Diagrams: 1.) The Hertzsprung-Russell diagram plots luminosity versus temperature. Aside from its primary use (i.e., if you can determine a star's surface temperature, the H-R diagram will give you its luminosity), it is a useful educational tool in the sense that it highlights in the universe order out of what would otherwise appear to be disorder. Hertzsprung-Russell diagram 2.) The basics of the H-R diagram and things you Luminosity (solar units) blue giants need to understand about and supergiants the system follow. 10,000 red giants and supergiants a.) Temperature 100 on the H-R diagram 100 R ranges from 30,000 main sun sequence degrees Kelvin to 1 sun 3000 degrees Kelvin 10 Rsun (those temperatures are plotted backward- .01 R -odd, but that's the sun red dwarfs way some white dwarfs astronomers are--a .0001 .1 Rsun little bit of physicist humor). It plots from 30,000 10,000 6000 3000 O type to M type stars (we talked about spec- Surface Temperature (degrees K) tral classification earlier). OAGMBFK Spectral Class 171 b.) The luminosity scale is expressed in terms of luminosity of the sun. That is, on a H-R diagram, L = 1 is found in the middle of the plot and denotes the sun's position on the diagram. c.) Luminosity on the H-R diagram ranges from 10-4 to 104. Again, 1 denotes the luminosity of the sun. -
NEUTRON STARS, GAMMA RAY BURSTS, and BLACK HOLES (Chap
NEUTRON STARS, GAMMA RAY BURSTS, and BLACK HOLES (chap. 22 in textbook) We will review the classes of remnants that can be left behind a star at the end of its life. We have already discussed the remnants of low-mass stars: white dwarfs. The following diagram may clarify, and is a useful review of stellar evolution. So we will discuss “neturon stars” and “black holes,” but in between we discuss the still mysterious “gamma-ray bursts.” Neutron Stars For carbon detonation SN ⇒ probably no remnant. The entire white dwarf explodes and disperses. A large fraction of it is turned into iron, and in fact this is believed to be the main supply of iron everywhere in the universe. (Recall that the light curves could be interpreted as the radioactive decay of two elements: nickel and cobalt. These will become iron.) For core-collapse SN ⇒ remnant is a neutron-degenerate core ⇒ neutron star Densities ~ 1014 to 1015 g/cm3 ~ billion times denser than water Cubic centimeter contains ~ 100 million tons! Like a single enormous nucleus, all neutrons nearly touching. So they are very tiny for stars! (See graphic figure 22.1 in textbook.) Gravity at surface is huge. e.g. a human would weigh ~ million tons Rotation period ~ fraction of a second when first formed (conservation of angular momentum) Magnetic field is huge, amplified by the collapse (~1012 x Earth’s field strength). Most extreme of these are called “magnetars”—100s now known. Observed as pulsars (discovered 1967). This was one of the most important astronomical discoveries of all time, by graduate student Jocelyn Bell, although her advisor was given the Nobel Prize for the totally accidental or serendipitous discovery. -
Stellar Evolution
Stellar Evolution The Lives and Deaths of Stars Protostars. These objects radiate energy away in the form of light. That energy comes from gravity – released by contraction. On the Main Sequence, the contraction stops because gravity and internal pressure exactly balance each other. Nuclear reactions occur at exactly the right rate to blbalance grav ity. AstarsA stars’ mass determines its luminosity Nuclear reactions slowly convert H to He in the core. Newlyyypy formed stars are typically: ~91% Hydrogen (H) ~9% Helium (He) In the Sun’s core, the conversion of H to He w ill take ~10 billion years (its Main Sequence lifetime). Composition of a Sun-Sun-likelike star What happens when the core Hydrogen is used up? Nuclear reactions stop. Core pressure decreases. Core contracts and gets hotter - htiheating overl liaying l ayers. 4H → 1He burning moves to a hot “shell.” Post-Main Sequence evolution •4H → 1He reactions occur faster than before. •The star gets brighter (more luminous)! •The hot shell causes the outer layers to expand and cool! •The star moves o ff t he Ma in Sequence, …up the “Red Giant” branch. AiAscension up thditthe red giant branch takes ~100 million years What happens in the core as it continues to contract and getht ho tter? Remember why Hydrogen burning requires 107 K? (Protons repel each other.) Helium nuclei ((p2 protons) rep el each other even more… Helium begins to fuse into Carbon at >108 K. This reaction is called “triple alpha ”= 3He → C. The Helium Flash: Post-Main Sequence evolution 8 After the core reaches 10 K, Helium “ignites” to make Carbon. -
Chapter 22 Neutron Stars and Black Holes Units of Chapter 22 22.1 Neutron Stars 22.2 Pulsars 22.3 Xxneutron-Star Binaries: X-Ray Bursters
Chapter 22 Neutron Stars and Black Holes Units of Chapter 22 22.1 Neutron Stars 22.2 Pulsars 22.3 XXNeutron-Star Binaries: X-ray bursters [Look at the slides and the pictures in your book, but I won’t test you on this in detail, and we may skip altogether in class.] 22.4 Gamma-Ray Bursts 22.5 Black Holes 22.6 XXEinstein’s Theories of Relativity Special Relativity 22.7 Space Travel Near Black Holes 22.8 Observational Evidence for Black Holes Tests of General Relativity Gravity Waves: A New Window on the Universe Neutron Stars and Pulsars (sec. 22.1, 2 in textbook) 22.1 Neutron Stars According to models for stellar explosions: After a carbon detonation supernova (white dwarf in binary), little or nothing remains of the original star. After a core collapse supernova, part of the core may survive. It is very dense—as dense as an atomic nucleus—and is called a neutron star. [Recall that during core collapse the iron core (ashes of previous fusion reactions) is disintegrated into protons and neutrons, the protons combine with the surrounding electrons to make more neutrons, so the core becomes pure neutron matter. Because of this, core collapse can be halted if the core’s mass is between 1.4 (the Chandrasekhar limit) and about 3-4 solar masses, by neutron degeneracy.] What do you get if the core mass is less than 1.4 solar masses? Greater than 3-4 solar masses? 22.1 Neutron Stars Neutron stars, although they have 1–3 solar masses, are so dense that they are very small. -
Review for Test #3 Nov 8
Review for Test #3 Nov 8 Topics: • Stars (including our Sun) • The Interstellar medium • Stellar Evolution and Stellar Death • Neutron stars, pulsars and magnetars • Black Holes and General Relativity Methods • Conceptual Review and Practice Problems Chapters 11, 12, 13, 14 • Review lectures (on-line) and know answers to clicker questions • Try practice quizzes on-line • Bring: • Two Number 2 pencils and your UNM ID • Simple calculator (no electronic notes) Reminder: There are NO make-up tests for this class Test #3 Review How to take a multiple choice test 1) Before the Test: • Study hard (~2 hours/day Friday through Monday) • Get plenty of rest the night before 2) During the Test: • Draw simple sketches to help visualize problems • Solve numerical problems in the margin • Come up with your answer first, then look for it in the choices • If you can’t find the answer, try process of elimination • If you don’t know the answer, Go on to the next problem and come back to this one later • TAKE YOUR TIME, don’t hurry • If you don’t understand something, ask me. Test #3 Useful Equations parallactic distance d = 1/p where p is parallax in arcsec and d is in parsecs Schwarschild Radius: 2 GM R = c2 Lifetimes of stars (on the main sequence): L = 1010/M2 years where M is the Mass in solar masses and L is the Lifetime Equivalence of Matter and Energy: E = mc2 We can observe emission from molecules. Most abundant is H2 (don't confuse with H II), but its emission is extremely weak, so other "trace" molecules observed: CO (carbon monoxide) H2O (water vapor) HCN (hydrogen cyanide) NH3 (ammonia) etc.