Shell Supernova Remnants As Cosmic Accelerators: I Stephen Reynolds, North Carolina State University
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Pos(BASH 2013)009 † ∗ [email protected] Speaker
The Progenitor Systems and Explosion Mechanisms of Supernovae PoS(BASH 2013)009 Dan Milisavljevic∗ † Harvard University E-mail: [email protected] Supernovae are among the most powerful explosions in the universe. They affect the energy balance, global structure, and chemical make-up of galaxies, they produce neutron stars, black holes, and some gamma-ray bursts, and they have been used as cosmological yardsticks to detect the accelerating expansion of the universe. Fundamental properties of these cosmic engines, however, remain uncertain. In this review we discuss the progress made over the last two decades in understanding supernova progenitor systems and explosion mechanisms. We also comment on anticipated future directions of research and highlight alternative methods of investigation using young supernova remnants. Frank N. Bash Symposium 2013: New Horizons in Astronomy October 6-8, 2013 Austin, Texas ∗Speaker. †Many thanks to R. Fesen, A. Soderberg, R. Margutti, J. Parrent, and L. Mason for helpful discussions and support during the preparation of this manuscript. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. http://pos.sissa.it/ Supernova Progenitor Systems and Explosion Mechanisms Dan Milisavljevic PoS(BASH 2013)009 Figure 1: Left: Hubble Space Telescope image of the Crab Nebula as observed in the optical. This is the remnant of the original explosion of SN 1054. Credit: NASA/ESA/J.Hester/A.Loll. Right: Multi- wavelength composite image of Tycho’s supernova remnant. This is associated with the explosion of SN 1572. Credit NASA/CXC/SAO (X-ray); NASA/JPL-Caltech (Infrared); MPIA/Calar Alto/Krause et al. -
Thursday, September 17, 2009 First Exam, Week from Today Pic of The
Thursday, September 17, 2009 First exam, week from today Astronomy in the news - end of Ramadan with new Moon. Pic of the Day - Andromeda in the Ultraviolet What happens when two white dwarfs spiral together? Larger mass WD has smaller radius Smaller mass, Which WD has the smaller Roche lobe? Larger The smaller mass radius Larger mass, Which fills its Roche Lobe first? Smaller radius Must be the smaller mass As small mass WD loses mass, its radius gets larger, but its Roche Lobe gets smaller! Runaway mass transfer. Small mass WD transfers essentially all its mass to larger mass WD Could end up with one larger mass WD If larger mass hits Mch → could get explosion => Supernova First WD < 1.4 solar masses First WD gets to 1.4 solar masses Classical Nova Recurrent Nova Two WD EXPLOSION! Gravitational Radiation, in-spiral WDs coalesce < 1.4 solar masses > 1.4 solar masses One Big WD EXPLOSION! End of Material for Test 1 Reading for First Exam Chapter 1: 1.2.3, 1.2.4, 1.3.2 Chapter 2: 2.3 Chapter 3: 3.1, 3.2, 3.3, 3.4, 3.8, 3.9, 3.10 Chapter 4: 4.1, 4.2, 4.3, 4.4, 4.5 Chapter 5: ALL Sky Watch Extra Credit Due Thursday, in Class Must be typed on regular 8-1/2x11 paper See web site for more details, or ask! See web site for star charts to help guide you where and when to look. Part of the exercise is to learn how to orient yourself and recognize objects and patterns in the sky. -
Pulsars and Supernova Remnants
1604–2004: SUPERNOVAE AS COSMOLOGICAL LIGHTHOUSES ASP Conference Series, Vol. 342, 2005 M. Turatto, S. Benetti, L. Zampieri, and W. Shea Pulsars and Supernova Remnants Roger A. Chevalier Dept. of Astronomy, University of Virginia, P.O. Box 3818, Charlottesville, VA 22903, USA Abstract. Massive star supernovae can be divided into four categories de- pending on the amount of mass loss from the progenitor star and the star’s ra- dius. Various aspects of the immediate aftermath of the supernova are expected to develop in different ways depending on the supernova category: mixing in the supernova, fallback on the central compact object, expansion of any pul- sar wind nebula, interaction with circumstellar matter, and photoionization by shock breakout radiation. Models for observed young pulsar wind nebulae ex- panding into supernova ejecta indicate initial pulsar periods of 10 − 100 ms and approximate equipartition between particle and magnetic energies. Considering both pulsar nebulae and circumstellar interaction, the observed properties of young supernova remnants allow many of them to be placed in one of the super- nova categories; the major categories are represented. The pulsar properties do not appear to be related to the supernova category. 1. Introduction The association of SN 1054 with the Crab Nebula and its central pulsar can be understood in the context of the formation of the neutron star in the core collapse and the production of a bubble of relativistic particles and magnetic fields at the center of an expanding supernova. Although the finding of more young pulsars and their wind nebulae initially proceeded slowly, there has recently been a rapid set of discoveries of more such pulsars and nebulae (Camilo 2004). -
Blasts from the Past Historic Supernovas
BLASTS from the PAST: Historic Supernovas 185 386 393 1006 1054 1181 1572 1604 1680 RCW 86 G11.2-0.3 G347.3-0.5 SN 1006 Crab Nebula 3C58 Tycho’s SNR Kepler’s SNR Cassiopeia A Historical Observers: Chinese Historical Observers: Chinese Historical Observers: Chinese Historical Observers: Chinese, Japanese, Historical Observers: Chinese, Japanese, Historical Observers: Chinese, Japanese Historical Observers: European, Chinese, Korean Historical Observers: European, Chinese, Korean Historical Observers: European? Arabic, European Arabic, Native American? Likelihood of Identification: Possible Likelihood of Identification: Probable Likelihood of Identification: Possible Likelihood of Identification: Possible Likelihood of Identification: Definite Likelihood of Identification: Definite Likelihood of Identification: Possible Likelihood of Identification: Definite Likelihood of Identification: Definite Distance Estimate: 8,200 light years Distance Estimate: 16,000 light years Distance Estimate: 3,000 light years Distance Estimate: 10,000 light years Distance Estimate: 7,500 light years Distance Estimate: 13,000 light years Distance Estimate: 10,000 light years Distance Estimate: 7,000 light years Distance Estimate: 6,000 light years Type: Core collapse of massive star Type: Core collapse of massive star Type: Core collapse of massive star? Type: Core collapse of massive star Type: Thermonuclear explosion of white dwarf Type: Thermonuclear explosion of white dwarf? Type: Core collapse of massive star Type: Thermonuclear explosion of white dwarf Type: Core collapse of massive star NASA’s ChANdrA X-rAy ObServAtOry historic supernovas chandra x-ray observatory Every 50 years or so, a star in our Since supernovas are relatively rare events in the Milky historic supernovas that occurred in our galaxy. Eight of the trine of the incorruptibility of the stars, and set the stage for observed around 1671 AD. -
G7. 7-3.7: a Young Supernova Remnant Probably Associated with the Guest
Draft version September 12, 2018 Typeset using LATEX twocolumn style in AASTeX62 G7.7-3.7: a young supernova remnant probably associated with the guest star in 386 CE (SN 386) Ping Zhou (hs),1, 2 Jacco Vink,1, 3, 4 Geng Li (Î耕),5, 6 and Vladim´ır Domcekˇ 1, 3 1Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands 2School of Astronomy and Space Science, Nanjing University, 163 Xianlin Avenue, Nanjing, 210023, China 3GRAPPA, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands 4SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands 5National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100101, China 6School of Astronomy and Space Science, University of Chinese Academy of Sciences, No.19A Yuquan Road, Shijingshan District, Beijing 100049, China Submitted to ApJL ABSTRACT Although the Galactic supernova rate is about 2 per century, only few supernova remnants are associated with historical records. There are a few ancient Chinese records of \guest stars" that are probably sightings of supernovae for which the associated supernova remnant is not established. Here we present an X-ray study of the supernova remnant G7.7−3:7, as observed by XMM-Newton, and discuss its probable association with the guest star of 386 CE. This guest star occurred in the ancient Chinese asterism Nan-Dou, which is part of Sagittarius. The X-ray morphology of G7.7−3:7 shows an arc-like feature in the SNR south, which is characterized by an under-ionized plasma with sub-solar abundances, a temperature of 0:4{0.8 keV, and a density of ∼ 0:5(d=4 kpc)−0:5 cm−3. -
Supernovae 6 Supernovae Stellar Catastrophes 1. Observations
Supernovae 6 Supernovae Stellar Catastrophes 1. Observations Which stars explode? Which collapse? Which outwit the villain gravity and settle down to a quiet old age as a white dwarf? Astrophysicists are beginning to block out answers to these questions. We know that a quiet death eludes some stars. Astronomers observe some stars exploding as supernovae, a sudden brightening by which a single star becomes as bright as an entire galaxy. Estimates of the energy involved in such a process reveal that a major portion of the star, if not the entire star, must be blown to smithereens. Historical records, particularly the careful data recorded by the Chinese, show that seven or eight supernovae have exploded over the last 2000 years in our portion of the Galaxy. The supernova of 1006 was the brightest ever recorded. One could read by this supernova at night. Astronomers throughout the Middle and Far East observed this event. The supernova of 1054 is by far the most famous, although this event is clearly not the only so-called “Chinese guest star.” This explosion produced the rapidly expanding shell of gas that modern astronomers identify as the Crab nebula. The supernova of 1054 was apparently recorded first by the Japanese and was also clearly mentioned by the Koreans, although the Chinese have the most careful records. There is a strong suspicion that Native Americans recorded the event in rock paintings and perhaps on pottery. An entertaining mystery surrounds the question of why there is no mention of the event in European history. One line of thought is that the church had such a grip on people in the Middle Ages that no one having seen the supernova would have dared voice a difference with the dogma of the immutability of the heavens. -
Cosmic Catastrophes Wheeler 309N Spring 2008 February 25, 2008 (49490) Review for Test #2 SUPERNOVAE
Cosmic Catastrophes Wheeler 309N Spring 2008 February 25, 2008 (49490) Review for Test #2 SUPERNOVAE Historical Supernovae in the Milky Way - several seen and recorded with naked eye in last 2000 years. SN 386 earliest on record, SN 1006 brightest, SN 1054, now the Crab Nebula, contains a rapidly rotating pulsar and suggestions of a jet. Tycho 1572, Kepler 1604. Cas A, not clearly seen about 1680, shows evidence for jets, and a dim compact object in the center. The events that show compact objects also seem to show evidence of “elongated” explosions or “jets.” SN1006, SN 1572 and SN 1604 were probably Type 1a. SN 1987A in a very nearby galaxy shows elongated ejecta, produced neutrinos so we know it was powered by core collapse. Extragalactic Supernovae - many, but dimmer, more difficult to study. Common elements produced in supernovae - carbon, oxygen, magnesium, silicon, sulfur, calcium - are built up by adding “building blocks” of helium nuclei consisting of four particles, 2 protons and 2 neutrons. Type I supernovae - no evidence for hydrogen in spectrum. Type II supernovae - definite evidence for hydrogen in spectrum. Type Ia supernovae - brightest, no hydrogen or helium, avoid spiral arms, occur in elliptical galaxies, origin in lower mass stars. Observe silicon early on, iron later. Unregulated burning, explosion in quantum pressure supported carbon/oxygen white dwarf of Chandrasekhar mass. Expected to occur in a binary system so white dwarf can grow. Star is completely disrupted, no neutron star or black hole. Light curve shows peak lasting about a week. Type II Supernovae - explode in spiral arms, never occur in elliptical galaxies, normal hydrogen, massive stars, recently born, short lived. -
Science Highlights
>>> SCIENCENOAO/NSO HIGHLIGHTS Echoes of Galactic Supernovae Armin Rest (Harvard University) & Chris Smith (NOAO) for the Echoes of Historical Supernovae (EHS) Team ight echoes from ancient supernova offer a unique and powerful oppor- tunity to study supernovae and their Lrelationships to supernova remnants (SNRs), as well as interstellar dust and Galactic structure. The use of this relatively simple phenomenon of light echoes in such studies is just now developing into an exciting new field of study. This is one of the very rare occasions in astronomy that the cause and effect of the same astronomical event can be observed, in that we can study the physics of the SNR as it appears now and also the physics of the explosion that produced it hundreds of years ago. We define a light echo as reflected light from a light source, not reprocessed light. Similar to the muffled echo of sound when someone shouts something toward a wall, the light echo still contains the initial signature of the original light, even if the precise signa- ture is somewhat modified by details of the reflecting surface. Since the reflected light traverses a longer path than the light that takes the direct path to the observer, it will be Figure 1 observed some time after the initial explosion is observed. to the SNR may be tens of times larger than if the Galactic plane than the supernovae in the the same SN and reflecting dust were located expectation that dust would be more highly Our group pioneered the optical discovery in the LMC. Thus the search annuli for light concentrated there. -
Supernovae and Neutron Stars
Outline of today’s lecture Lecture 17: •Finish up lecture 16 (nucleosynthesis) •Supernovae •2 main classes: Type II and Type I Supernovae and •Their energetics and observable properties Neutron Stars •Supernova remnants (pretty pictures!) •Neutron Stars •Review of formation http://apod.nasa.gov/apod/ •Pulsars REVIEWS OF MODERN PHYSICS, VOLUME 74, OCTOBER 2002 The evolution and explosion of massive stars S. E. Woosley* and A. Heger† Department of Astronomy and Astrophysics, University of California, Santa Cruz, California 95064 T. A. Weaver Lawrence Livermore National Laboratory, Livermore, California 94551 (Published 7 November 2002) Like all true stars, massive stars are gravitationally confined thermonuclear reactors whose composition evolves as energy is lost to radiation and neutrinos. Unlike lower-mass stars (M Շ8M᭪), however, no point is ever reached at which a massive star can be fully supported by electron degeneracy. Instead, the center evolves to ever higher temperatures, fusing ever heavier elements until a core of iron is produced. The collapse of this iron core to a neutron star releases an enormous amount of energy, a tiny fraction of which is sufficient to explode the star as a supernova. The authors examine our current understanding of the lives and deaths of massive stars, with special attention to the relevant nuclear and stellar physics. Emphasis is placed upon their post-helium-burning evolution. Current views regarding the supernova explosion mechanism are reviewed, and the hydrodynamics of supernova shock propagation and ‘‘fallback’’ is discussed. The calculated neutron star masses, supernova light curves, and spectra from these model stars are shown to be consistent with observations. -
Nature's Biggest Explosions: Past, Present, and Future
Nature’s Biggest Explosions: Past, Present, and Future Edo Berger Harvard University Why Study Cosmic Explosions? Why Study Cosmic Explosions? Why Study Cosmic Explosions? Why Study Cosmic Explosions? Why Study Cosmic Explosions? The Past About 10 “guest stars” have been mentioned in historical records, spanning from 185 to 1604 AD. All were observed with the naked eye (first telescope was built in 1608 AD). “Throughout all past time, according to the records handed down from generation to generation, nothing is observed to have changed either in the whole of the outermost heaven or in any of its proper parts.” Aristotle, De caelo (On the Heavens), 350 BC SN 185 In 185 AD Chinese records mark the appearance of a “guest star” which remained visible for 8 months and did not move like a planet or a comet. This is the oldest record of a supernova. “In the 2nd year of the epoch Zhongping, the 10th month, on the day Kwei Hae, a strange star appeared in the middle of Nan Mun … In the 6th month of the succeeding year it disappeared.” SN 1006 On April 1006 records from Europe, the Middle East, and Asia mark the appearance of the brightest “guest star” ever seen: bright as a quarter moon and visible during the day. It remained visible for almost 2 years. “…spectacle was a large circular body, 2½ to 3 times as large as Venus. The sky was shining because of its light. The intensity of its light was a little more than the light of the Moon when one-quarter illuminated" SN 1054 On July 4, 1054 AD records from the Middle East and Asia (and potentially North America) mark the appearance of a bright “guest star”; as bright as a 1/16 moon and remained visible for 2 years. -
A Brief History of Astronomical Brightness Determination Methods at Optical Wavelengths
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server A Brief History of Astronomical Brightness Determination Methods at Optical Wavelengths Kevin Krisciunas Abstract In this brief article I review the history of astronomical photometry, touching on observations made by the ancient Chinese, Hipparchus and Ptolemy, the development of the concept (and definition) of magnitude, the endeavors of Argelander and Z¨ollner, work at Harvard at the end of the 19th century, and the development of photography, photomultipliers, and CCD’s and their application to astronomy. ...this brave o'erhanging firmament, this majestical roof fretted with golden fire.... Hamlet, II, ii, 308-310 The following introduction to photometry served as Chapter 1 to my recent University of Washington Dissertation; see Krisciunas (2001) for a summary. Chapter 2 (Krisciunas, Margon, & Szkody 1998) dealt with the identification of objects of interest, in particular RR Lyrae stars, carbon stars, asteroids, and cataclysmic variables, using the photometric system being used for the Sloan Digital Sky Survey. Chapter 3 involved the confirmation of RR Lyrae candidates from SDSS as bona fide RR Lyrae stars; light curves of six of these can be found in Ivezic et al. (2000). Chapters 4 and 5 (Krisciunas et al. 2000, 2001) dealt 1 with Type Ia supernovae and the use of optical and infrared photometry to determine the extinction of these objects attributable to dust along the line of sight. The first systematic observations of the heavens which can be considered “scientific” in any sense were carried out by the Chinese as early as the 14th century BC (Needham & Ling 1959, p. -
Wheeler February 1, 2016 Cosmic Catastrophes 309N Spring 2016
Cosmic Catastrophes Wheeler 309N Spring 2016 February 1, 2016 (46890) Review for Test #1 BACKGROUND AND INTRODUCTION TO SUPERNOVAE The Universe is a strange place. For stars, red is cool, white is hot, giant means bright and dwarf means dim. Main Sequence — stars fuse hydrogen into helium and thus supply energy. In evolution after the Main Sequence, “core” refers to the inner part of the star that is composed of elements heavier than hydrogen and “envelope” means the outer regions still composed of hydrogen. Red Giant — when hydrogen burns out in the center, excess heat flowing from the contracting core causes the outer layers to gain energy. They then expand and cool. The envelope becomes larger, cooler, redder, and more luminous. Planetary nebulae —Most stars less than 8 M ( is the symbol for the Sun, so 8 times the mass of the Sun) eject their outer envelopes of unburned hydrogen as planetary nebulae. Core of C and O cools to become white dwarf. White Dwarfs. Size of Earth, mass of Sun. Cooling time longer than the age of the Universe. Almost every white dwarf ever born in the Milky Way is still here. Sirius has a white dwarf companion orbiting around it. Two explosion mechanisms – collapse of core of massive star or exploding white dwarf. Historical Supernovae in the Milky Way - several seen and recorded with naked eye in last 2000 years. SN 386 earliest on record, SN 1006 brightest, SN 1054, now the Crab Nebula, contains a rapidly rotating pulsar and suggestions of a jet. Tycho 1572, Kepler 1604.