Nature's Biggest Explosions: Past, Present, and Future
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FY08 Technical Papers by GSMTPO Staff
AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................ -
Species Which Remained Immutable and Unchanged Thereafter
THE ORIGIN OF THE ELEMENTS BY WILLIAM A. FOWLER CALIFORNIA INSTITUTE OF TECHNOLOGY, PASADENA They [atoms] move in the void and catching each other up jostle together, and some recoil in any direction that may chance, and others become entangled with one another in various degrees according to the symmetry of their shapes and sizes and positions and order, and they remain together and thus the coming into being of composite things is effected. -SIMPLICIUS (6th Century A.D.) It is my privilege to begin our consideration of the history of the universe during this first scientific session of the Academy Centennial with a discussion of the origin of the elements of which the matter of the universe is constituted. The question of the origin of the elements and their numerous isotopes is the modern expression of one of the most ancient problems in science. The early Greeks thought that all matter consisted of the four simple substances-air, earth, fire, and water-and they, too, sought to know the ultimate origin of what for them were the elementary forms of matter. They also speculated that matter consists of very small, indivisible, indestructible, and uncreatable atoms. They were wrong in detail but their concepts of atoms and elements and their quest for origins persist in our science today. When our Academy was founded one century ago, the chemist had shown that the elements were immutable under all chemical and physical transformations known at the time. The alchemist was self-deluded or was an out-and-out charla- tan. Matter was atomic, and absolute immutability characterized each atomic species. -
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. -
Neutron Stars: Introduction
Neutron Stars: Introduction Stephen Eikenberry 16 Jan 2018 Original Ideas - I • May 1932: James Chadwick discovers the neutron • People knew that n u clei w ere not protons only (nuclear mass >> mass of protons) • Rutherford coined the name “neutron” to describe them (thought to be p+ e- pairs) • Chadwick identifies discrete particle and shows mass is greater than p+ (by 0.1%) • Heisenberg shows that neutrons are not p+ e- pairs Original Ideas - II • Lev Landau supposedly suggested the existence of neutron stars the night he heard of neutrons • Yakovlev et al (2012) show that he in fact discussed dense stars siiltimilar to a gi ant nucl eus BEFORE neutron discovery; this was immediately adapted to “t“neutron s t”tars” Original Ideas - III • 1934: Walter Baade and Fritz Zwicky suggest that supernova eventtttts may create neutron stars • Why? • Suppg(ernovae have huge (but measured) energies • If NS form from normal stars, then the gravitational binding energy gets released • ESN ~ star … Original Ideas - IV • Late 1930s: Oppenheimer & Volkoff develop first theoretical models and calculations of neutron star structure • WldhWould have con tidbttinued, but WWII intervened (and Oppenheimer was busy with other things ) • And that is how things stood for about 30 years … Little Green Men - I • Cambridge experiment with dipole antennae to map cosmic radio sources • PI: Anthony Hewish; grad students included Jocelyn Bell Little Green Men - II • August 1967: CP 1919 discovered in the radio survey • Nov ember 1967: Bell notices pulsations at P =1.337s -
Beeps, Flashes, Bangs and Bursts
Beeps, Flashes, Big stars work much faster: Bangs and Bursts. 1,000,000 100,000 100,000 100,000 and Chirps. Forever Peter Watson 3 hours! Live fast, Die Young! Peter Watson, Dept. of Physics Change colour, size, brightness •Vast majority of stars are boring: “main- sequence” (aka middle- class) changing very slowly. •Some oscillate: e.g Cepheids •Large bright stars change by factor 3 in brightness Peter Watson Peter Watson If Stars are large.... • we get supernovae • 6 visible in Milky Way over last 1000 years •well understood: work by blocking mechanism • SN 1006: Brightest •very important since period is proportional to Supernova. intrinsic brightness: • Can see remnants of the expanding •i.e. measure the apparent brightness, the period tells shockwave you the actual brightness, so you know how far away Frank Winkler (Middlebury College) et it is al., AURA, NOAO, NSF Peter Watson Peter Watson Remnant of a very Tycho’s old SN Supernova • Part of the veil nebula in X-rays in Cygnus (1572) Sara Wager NASA / CXC / F.J. Lu (Chinese Academy of Sciences) et al. Peter Watson Peter Watson The Crab (M1) •Recorded by Chinese astronomers "I humbly observe that a guest star has appeared; above the star there is a feeble yellow glimmer. If one examines the divination regarding the Emperor, the interpretation [of the presence of this guest star] is the following: The fact that the star has not overrun Bi and that its brightness must represent a person of great value. I demand that the Office of Historiography is informed of this." PW Peter Watson 1054: Crab •Recorded by Chinese astronomers as “guest star” •May have been recorded by Chaco Indians in New • X-rays (in blue) Mexico • + Optical 4 a.m. -
The Korean 1592--1593 Record of a Guest Star: Animpostor'of The
Journal of the Korean Astronomical Society 49: 00 ∼ 00, 2016 December c 2016. The Korean Astronomical Society. All rights reserved. http://jkas.kas.org THE KOREAN 1592–1593 RECORD OF A GUEST STAR: AN ‘IMPOSTOR’ OF THE CASSIOPEIA ASUPERNOVA? Changbom Park1, Sung-Chul Yoon2, and Bon-Chul Koo2,3 1Korea Institute for Advanced Study, 85 Hoegi-ro, Dongdaemun-gu, Seoul 02455, Korea; [email protected] 2Department of Physics and Astronomy, Seoul National University, Gwanak-gu, Seoul 08826, Korea [email protected], [email protected] 3Visiting Professor, Korea Institute for Advanced Study, Dongdaemun-gu, Seoul 02455, Korea Received |; accepted | Abstract: The missing historical record of the Cassiopeia A (Cas A) supernova (SN) event implies a large extinction to the SN, possibly greater than the interstellar extinction to the current SN remnant. Here we investigate the possibility that the guest star that appeared near Cas A in 1592{1593 in Korean history books could have been an `impostor' of the Cas A SN, i.e., a luminous transient that appeared to be a SN but did not destroy the progenitor star, with strong mass loss to have provided extra circumstellar extinction. We first review the Korean records and show that a spatial coincidence between the guest star and Cas A cannot be ruled out, as opposed to previous studies. Based on modern astrophysical findings on core-collapse SN, we argue that Cas A could have had an impostor and derive its anticipated properties. It turned out that the Cas A SN impostor must have been bright (MV = −14:7 ± 2:2 mag) and an amount of dust with visual extinction of ≥ 2:8 ± 2:2 mag should have formed in the ejected envelope and/or in a strong wind afterwards. -
EVOLUTION of the CRAB NEBULA in a LOW ENERGY SUPERNOVA Haifeng Yang and Roger A
Draft version August 23, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 EVOLUTION OF THE CRAB NEBULA IN A LOW ENERGY SUPERNOVA Haifeng Yang and Roger A. Chevalier Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904; [email protected], [email protected] Draft version August 23, 2018 ABSTRACT The nature of the supernova leading to the Crab Nebula has long been controversial because of the low energy that is present in the observed nebula. One possibility is that there is significant energy in extended fast material around the Crab but searches for such material have not led to detections. An electron capture supernova model can plausibly account for the low energy and the observed abundances in the Crab. Here, we examine the evolution of the Crab pulsar wind nebula inside a freely expanding supernova and find that the observed properties are most consistent with a low energy event. Both the velocity and radius of the shell material, and the amount of gas swept up by the pulsar wind point to a low explosion energy ( 1050 ergs). We do not favor a model in which circumstellar interaction powers the supernova luminosity∼ near maximum light because the required mass would limit the freely expanding ejecta. Subject headings: ISM: individual objects (Crab Nebula) | supernovae: general | supernovae: indi- vidual (SN 1054) 1. INTRODUCTION energy of 1050 ergs (Chugai & Utrobin 2000). However, SN 1997D had a peak absolute magnitude of 14, con- The identification of the supernova type of SN 1054, − the event leading to the Crab Nebula, has been an en- siderably fainter than SN 1054 at maximum. -
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). -
Nd AAS Meeting Abstracts
nd AAS Meeting Abstracts 101 – Kavli Foundation Lectureship: The Outreach Kepler Mission: Exoplanets and Astrophysics Search for Habitable Worlds 200 – SPD Harvey Prize Lecture: Modeling 301 – Bridging Laboratory and Astrophysics: 102 – Bridging Laboratory and Astrophysics: Solar Eruptions: Where Do We Stand? Planetary Atoms 201 – Astronomy Education & Public 302 – Extrasolar Planets & Tools 103 – Cosmology and Associated Topics Outreach 303 – Outer Limits of the Milky Way III: 104 – University of Arizona Astronomy Club 202 – Bridging Laboratory and Astrophysics: Mapping Galactic Structure in Stars and Dust 105 – WIYN Observatory - Building on the Dust and Ices 304 – Stars, Cool Dwarfs, and Brown Dwarfs Past, Looking to the Future: Groundbreaking 203 – Outer Limits of the Milky Way I: 305 – Recent Advances in Our Understanding Science and Education Overview and Theories of Galactic Structure of Star Formation 106 – SPD Hale Prize Lecture: Twisting and 204 – WIYN Observatory - Building on the 308 – Bridging Laboratory and Astrophysics: Writhing with George Ellery Hale Past, Looking to the Future: Partnerships Nuclear 108 – Astronomy Education: Where Are We 205 – The Atacama Large 309 – Galaxies and AGN II Now and Where Are We Going? Millimeter/submillimeter Array: A New 310 – Young Stellar Objects, Star Formation 109 – Bridging Laboratory and Astrophysics: Window on the Universe and Star Clusters Molecules 208 – Galaxies and AGN I 311 – Curiosity on Mars: The Latest Results 110 – Interstellar Medium, Dust, Etc. 209 – Supernovae and Neutron -
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.