Energetic Phenomena in Isolated Neutron Stars, Pulsar Wind Nebulae & Supernova Remnants

Total Page:16

File Type:pdf, Size:1020Kb

Energetic Phenomena in Isolated Neutron Stars, Pulsar Wind Nebulae & Supernova Remnants The Fast and the Furious: Energetic Phenomena in Isolated Neutron Stars, Pulsar Wind Nebulae & Supernova Remnants 22−24 May 2013 European Space Astronomy Centre Villafranca del Castillo Madrid, Spain A conference organised by the European Space Agency XMM-Newton Science Operations Centre ABSTRACT BOOK Oral Communications and Posters Edited by Andy Pollock with the help of Cristina Hernandez and Jan-Uwe Ness Organising Committees Scientific Organising Committee Sandro Mereghetti (Chair) INAF, IASF-Milano, Italy Werner Becker MPE, Garching, Germany Andrei Bykov Ioffe Physical-Technical Institute, St. Petersburg, Russia Wim Hermsen SRON, Utrecht, The Netherlands Victoria Kaspi McGill University, Montreal, Canada Demosthenes Kazanas NASA/GSFC, Greenbelt MD, USA Chryssa Kouveliotou NASA/MSFC, Huntsville AL, USA Dong Lai Cornell University, Ithaca, NY, USA Kazuo Makishima University of Tokyo, Japan Sergey Popov Sternberg Astronomical Institute, Moscow, Russia Norbert Schartel (co-Chair) XMM-Newton SOC, Madrid, Spain Patrick Slane CfA, Cambridge MA, USA Luigi Stella INAF, Rome, Italy Diego Torres IEEC-CSIC, Barcelona, Spain Anna Watts University of Amsterdam, The Netherlands Martin C. Weisskopf NASA/MSFC, Huntsville AL, USA Silvia Zane MSSL-UCL, Dorking, Surrey, UK Local Organising Committee (XMM-Newton Science Operations Centre) Jan-Uwe Ness (Chair) Michelle Arpizou Matthias Ehle Carlos Gabriel Aitor Ibarra Andy Pollock Richard Saxton Martin Stuhlinger Contents 1 Invited Speakers 3 Review of the theory of PWNe Niccol`oBucciantini . 4 Multi-wavelength Observations of Known, and Searches for New, Gamma-ray Binaries Robin Corbet, Chi Cheung, Malcolm Coe, Joel Coley, Davide Donato, Philip Ed- wards, Vanessa McBride, M. Virginia McSwain, Jamie Stevens . 4 TeV emitting PWNe: abundant and diverse high energy engines of all ages Arache Djannati-Atai . 5 Magnetar Bursts at All Scales Ersin Gogus . 5 Timing Solutions for all three Anti-Magnetars Eric Gotthelf, Jules Halpern . 6 The Magnificent Seven: Nearby, Thermally Emitting, Isolated Neutron Stars Frank Haberl . 6 X-ray observations of pulsar-wind nebulae: current status and future prospects Oleg Kargaltsev, George Pavlov, Martin Durant . 7 Gamma-ray emission of Crab pulsar and the nebula Maxim Lyutikov . 7 X-ray observations of rotation-powered pulsars George Pavlov, Oleg Kargaltsev, Bettina Posselt, Martin Durant . 8 Magneto-thermal evolution of strongly magnetized neutron stars. Jose Pons . 8 Magnetars: explosive neutron stars with extreme magnetic fields Nanda Rea . 9 Gamma-ray Pulsars with the Fermi Satellite David Smith . 9 Suzaku Observations of Gamma-Ray Binaries and Prospects for ASTRO-H Takaaki Tanaka . 10 The Flaring Crab Nebula: Surprises and Challenges Marco Tavani . 10 High-energy pulsar models: Developments and new questions Christo Venter, Alice K. Harding . 11 Large Observatory for X-ray Timing (LOFT) M. van der Klis . 11 3 2 High-energy emission from rotation-powered neutron stars 13 2D Particle-in-Cell Simulation of the Pulsar Polar-cap Discharge Alexander Yuran Chen, Andrei Beloborodov . 14 Multi-component X-ray Spectral Analysis of the Double Pulsar System J0737-3039 Elise Egron, Alberto Pellizzoni, Maria Noemi Iacolina . 14 XMM-Newton revealed synchronous X-ray and radio mode changing in a pulsar: a bi- stable emission behaviour requiring global magnetospheric changes Wim Hermsen . 15 New Fermi-LAT Gamma-ray Pulsars Using Radio Ephemerides Xian Hou, David Smith . 15 Long Term X-Ray Timing of the Double Pulsar PSR J0737-3039 Maria Noemi Iacolina, Alberto Pellizzoni, Elise Egron, Paolo Esposito . 16 Particle acceleration region of old pulsars Shota Kisaka, Shuta Tanaka . 16 The soft gamma-ray pulsar population and its link to the Fermi LAT pulsar population: a full high-energy picture Lucien Kuiper, Wim Hermsen . 17 Deep X-ray Observations of the High-Magnetic-Field Radio Pulsar J1119-6127 C.-Y. Ng, V. M. Kaspi, W.C.G. Ho, P. Weltevrede, S. Bogdanov, R. Shannon, M. E. Gonzalez . 17 A unified polar cap/striped wind model for pulsed radio and gamma-ray emission in pulsars J´erˆomeP´etri . 18 Plasma-producing Gaps in the Global Structure of the Pulsar Force-free Magnetosphere Svetlana Petrova . 18 Physical links between the radio and high-energy emissions of pulsars Svetlana Petrova . 19 Probing the cooling of the Central Compact Object in the Cas A supernova remnant Bettina Posselt, George Pavlov, Valery Suleimanov . 19 X-ray observations and the search for Fermi-LAT gamma-ray pulsars Pablo Saz Parkinson, Andrea Belfiore, Patrizia Caraveo, Andrea De Luca, Martino Marelli .......................................... 20 Spectral properties and HE behaviour of few bright and young Fermi PSRs Thomas Tavernier . 20 Soft Gamma-ray Pulsars Yu Wang, Jumpei Takata, Kwong Sang Cheng . 21 3 Multiwavelength properties and unification scenarios for different classes of neu- tron stars 23 Fermi-LAT observations and a broadband study of supernova remnant CTB 109 Daniel Castro . 24 Constraining Magnetar Bursts Properties from Energy-Dependent Variability Caroline D’Angelo . 24 The first complete X-ray view of the Supernova Remnant Puppis A Gloria Dubner, Nora Loiseau, Pedro Rodr´ıguez-Pascual, Michael J.S. Smith, Elsa Giacani, Gabriela Castelletti . 25 Suzaku View of Recent Magnetar and Magnetar-related Objects Teruaki Enoto, Kazuo Makishima, Shinpei Shibata, Yujin Nakagawa, Takanori Sakamoto . 25 Modulating magnetar emission by magneto-elastic oscillations Michael Gabler, Pablo Cerd´a-Dur´an, Jos´eAntonio Font, Nikolaos Stergioulas, Ewald M¨uller........................................... 26 The Progenitor and Pulsar Birth Properties of Composite SNR Kes 75 Joseph Gelfand, Patrick Slane, Tea Temim . 26 Observationally consistent evolution scenario for neutron stars in LMXBs Mikhail Gusakov, Andrey Chugunov, Elena Kantor . 27 New instability windows for rotating neutron stars Mikhail Gusakov, Andrey Chugunov, Elena Kantor . 27 Hard X-ray emission from magnetars: fit by a physical model and resulting constraints Romain Hascoet, Andrei M. Beloborodov, Peter den Hartog . 28 Magnetic fields decay in pulsars: population synthesis and other statistical methods Andrei Igoshev . 28 Deep observations of PSR J0357+3205 with GTC Aida Kirichenko, Sergey Zharikov, Yuri Shibanov, Dima Zyuzin, Peter Shternin, Andrei Danilenko . 29 On the X-ray emission mechanisms of the persistent source and very low-fluence bursts of SGR J0501+4516 Lin Lin, Ersin Gogus . 29 New XMM-Newton observation of the thermally emitting isolated neutron star in the Carina Nebula Adriana Mancini Pires, Christian Motch . 30 Supernova Remnants with Magnetars Jonatan Mart´ın,Nanda Rea, Diego F. Torres . 30 The shape of the cutoff in the synchrotron emission of SN 1006 observed with XMM- Newton Marco Miceli, Fabrizio Bocchino, Anne Decourchelle, Jacco Vink, Sjors Broersen, Salvatore Orlando . 31 Search for correlation between giant radio pulses and hard X-ray pulses from the Crab pulsar Ryo Mikami, Toshio Terasawa, Kazuhiro Takefuji, Mamoru Sekido, Hiroshi Takeuchi, Yasuyuki Tanaka, Shota Kisaka, Katsuaki Asano, Nobuyuki Kawai, Kumiko Nagata 31 Suzaku Studies of the Supernova Remnant CTB109 and its Central Magnetar 1E 2259+586 Toshio Nakano, Kazuo Makishima . 32 Equilibrium Models for Magnetized Neutron Stars in General Relativity Antonio G. Pili, Niccolo’ Bucciantini, Del Zanna Luca . 32 Unifying neutron stars: advances, problems and initial parameters Sergey Popov, Andrei Igoshev, Roberto Turolla . 33 The Magnificent Seven see (Infra)red Bettina Posselt, Sergey Popov, George Pavlov . 33 X-ray follow-up observations of confirmed and potential TeV supernova remnants Gerd Puehlhofer, . 34 Westerlund1 Transient AXP: Long-term Phase-coherent X-ray Timing & Pulse-Phase Spectroscopy of CXOU J164710.2-4552 Guillermo-Andres Rodriguez-Castillo, GianLuca Israel . 34 Is there a magnetar wind nebula around Swift J1834.9-0846? Andrea Tiengo . 35 The maximum period of pulsars as a probe of fundamental physics Daniele Vigan`o,Jose Antonio Pons, Nanda Rea . 35 Solving the Vela pulsar infrared excess problem Dima Zyuzin, Yuri Shibanov, Andrei Danilenko, Sergey Zharikov, Ronald Mennick- ent ............................................ 36 4 Energetic phenomena in non-accreting neutron stars and their effects on the surroundings 37 Modeling statistical properties of the X-ray emission from aged Pulsar Wind Nebulae Rino Bandiera . 38 RRAT J1819-1458 and its extended X-ray emission Ascensi´onCamero Arranz, Nanda Rea . 38 Particle Acceleration and Magnetic Fields: Looking at the Northwestern Rim of RCW 86 with Chandra Daniel Castro . 39 Magnetic Field Instabilities in Neutron Stars Riccardo Ciolfi, Luciano Rezzolla . 39 The Guitar Nebula Studies at Optical Wavelengths Andrei Danilenko, Victoria Komarova, Alexei Moiseev, Yuri Shibanov . 40 A fast-moving radio-quiet pulsar with a very unusual X-ray trail Andrea De Luca . 40 The power of X-ray observations in identifying TeV emitting pulsar wind nebulae: The case of HESS J1818−154 Peter Eger, Petter Hofverberg, H.E.S.S. Collaboration . 41 ”Black widow” binary systems Jorge Ernesto Horvath, Maria Alejandra De Vito, Omar Benvenuto . 41 The stability of strong waves and its implications for pulsar wind shocks Iwona Mochol, John G. Kirk . 42 Supernova Remnant Candidates in the ROSAT All-Sky Survey Tobias Prinz, Werner Becker . 42 Intrabinary Shock Emission From Black Widows and Redbacks Mallory Roberts, Maura McLaughlin, Pete Gentile, Ester Aliu, Jason Hessels, Scott Ransom, Paul Ray . 43 Supernova Dust and Ejecta Illuminated
Recommended publications
  • Report for the Academic Year 1995
    Institute /or ADVANCED STUDY REPORT FOR THE ACADEMIC YEAR 1994 - 95 PRINCETON NEW JERSEY Institute /or ADVANCED STUDY REPORT FOR THE ACADEMIC YEAR 1 994 - 95 OLDEN LANE PRINCETON • NEW JERSEY 08540-0631 609-734-8000 609-924-8399 (Fax) Extract from the letter addressed by the Founders to the Institute's Trustees, dated June 6, 1930. Newark, New jersey. It is fundamental in our purpose, and our express desire, that in the appointments to the staff and faculty, as well as in the admission of workers and students, no account shall be taken, directly or indirectly, of race, religion, or sex. We feel strongly that the spirit characteristic of America at its noblest, above all the pursuit of higher learning, cannot admit of any conditions as to personnel other than those designed to promote the objects for which this institution is established, and particularly with no regard whatever to accidents of race, creed, or sex. TABLE OF CONTENTS 4 BACKGROUND AND PURPOSE 5 • FOUNDERS, TRUSTEES AND OFFICERS OF THE BOARD AND OF THE CORPORATION 8 • ADMINISTRATION 11 REPORT OF THE CHAIRMAN 15 REPORT OF THE DIRECTOR 23 • ACKNOWLEDGMENTS 27 • REPORT OF THE SCHOOL OF HISTORICAL STUDIES ACADEMIC ACTIVITIES MEMBERS, VISITORS AND RESEARCH STAFF 36 • REPORT OF THE SCHOOL OF MATHEMATICS ACADEMIC ACTIVITIES MEMBERS AND VISITORS 42 • REPORT OF THE SCHOOL OF NATURAL SCIENCES ACADEMIC ACTIVITIES MEMBERS AND VISITORS 50 • REPORT OF THE SCHOOL OF SOCIAL SCIENCE ACADEMIC ACTIVITIES MEMBERS, VISITORS AND RESEARCH STAFF 55 • REPORT OF THE INSTITUTE LIBRARIES 57 • RECORD OF INSTITUTE EVENTS IN THE ACADEMIC YEAR 1994-95 85 • INDEPENDENT AUDITORS' REPORT INSTITUTE FOR ADVANCED STUDY: BACKGROUND AND PURPOSE The Institute for Advanced Study is an independent, nonprofit institution devoted to the encouragement of learning and scholarship.
    [Show full text]
  • Chandra Detection of a Pulsar Wind Nebula Associated with Supernova Remnant 3C 396
    Chandra Detection of a Pulsar Wind Nebula Associated With Supernova Remnant 3C 396 C.M. Olbert',2, J.W. Keohane'l2v3, K.A. Arnaud4, K.K. Dyer5, S.P. Reynolds', S. Safi-Harb7 ABSTRACT We present a 100 ks observation of the Galactic supernova remnant 3C396 (G39.2-0.3) with the Chandra X-Ray Observatory that we compare to a 20cm map of the remnant from the Verp Large Array'. In the Chandra images, a non- thermal nebula containing an embedded pointlike source is apparent near the center of the remnant which we interpret as a synchrotron pulsar wind nebula surrounding a yet undetected pulsar. From the 2-10 keV spectrum for the nebula (NH = 5.3 f 0.9 x cm-2, r=1.5&0.3) we derive an unabsorbed X-ray flux of SZ=1.62x lo-'* ergcmV2s-l, and from this we estimate the spin-down power of the neutron star to be fi = 7.2 x ergs-'. The central nebula is morphologi- cally complex, showing bent, extended structure. The radio and X-ray shells of the remnant correlate poorly on large scales, particularly on the eastern half of the remnant, which appears very faint in X-ray images. At both radio and X-ray wavelengths the western half of the remnant is substantially brighter than the east. Subject headings: ISM: individual (3C396 / G39.2-0.3) - stars: neutron - pulsars: general - supernova remnants lNorth Carolina School of Science and Mathematics, 1219 Broad St., Durham, NC 27705 2Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599 3Current Address: SIRTF Science Center, California Institute of Technology, MS 220-6, 1200 East Cali- fornia Boulevard, Pasedena, CA 91125 *Goddard Space Flight Center, Code 662, Greenbelt, MD 20771 5National Radio Astronomy Observatory, P.O.
    [Show full text]
  • Female Fellows of the Royal Society
    Female Fellows of the Royal Society Professor Jan Anderson FRS [1996] Professor Ruth Lynden-Bell FRS [2006] Professor Judith Armitage FRS [2013] Dr Mary Lyon FRS [1973] Professor Frances Ashcroft FMedSci FRS [1999] Professor Georgina Mace CBE FRS [2002] Professor Gillian Bates FMedSci FRS [2007] Professor Trudy Mackay FRS [2006] Professor Jean Beggs CBE FRS [1998] Professor Enid MacRobbie FRS [1991] Dame Jocelyn Bell Burnell DBE FRS [2003] Dr Philippa Marrack FMedSci FRS [1997] Dame Valerie Beral DBE FMedSci FRS [2006] Professor Dusa McDuff FRS [1994] Dr Mariann Bienz FMedSci FRS [2003] Professor Angela McLean FRS [2009] Professor Elizabeth Blackburn AC FRS [1992] Professor Anne Mills FMedSci FRS [2013] Professor Andrea Brand FMedSci FRS [2010] Professor Brenda Milner CC FRS [1979] Professor Eleanor Burbidge FRS [1964] Dr Anne O'Garra FMedSci FRS [2008] Professor Eleanor Campbell FRS [2010] Dame Bridget Ogilvie AC DBE FMedSci FRS [2003] Professor Doreen Cantrell FMedSci FRS [2011] Baroness Onora O'Neill * CBE FBA FMedSci FRS [2007] Professor Lorna Casselton CBE FRS [1999] Dame Linda Partridge DBE FMedSci FRS [1996] Professor Deborah Charlesworth FRS [2005] Dr Barbara Pearse FRS [1988] Professor Jennifer Clack FRS [2009] Professor Fiona Powrie FRS [2011] Professor Nicola Clayton FRS [2010] Professor Susan Rees FRS [2002] Professor Suzanne Cory AC FRS [1992] Professor Daniela Rhodes FRS [2007] Dame Kay Davies DBE FMedSci FRS [2003] Professor Elizabeth Robertson FRS [2003] Professor Caroline Dean OBE FRS [2004] Dame Carol Robinson DBE FMedSci
    [Show full text]
  • Exploring CTA Science with Ted and Friends - Activities
    Exploring CTA Science with Ted and Friends - Activities This handbook proposes questions and exercises for educators related to the animated series “Exploring CTA Science with Ted and Friends.” The goal is to reinforce the concepts the students learn in each episode about high-energy astrophysics and the future gamma-ray observatory, the Cherenkov Telescope Array (CTA), as well as to develop their scientific thinking and logic. The questions are divided according to each episode - we recommend educators to perform these activities following each episode in order to consolidate new ideas before staring the next episode. Age range: 5-11 years Supplementary material: https://www.cta-observatory.org/outreach-education/ Questions? Contact CTAO Outreach and Education Coordinator, Alba Fernández-Barral ([email protected]) Exploring CTA Science with Ted and Friends EPISODE 1: “CTA: Searching the Skies” How many CTA telescopes will be located around the world? More than 100 (Note for educators: specifically, 118 – 19 in La Palma, Spain, and 99 near Paranal, Chile). Where are they going to be located? One group will be in Chile (South America) while the other will be in La Palma (a Spanish island in the Canary Islands, off the coast of west Africa). What do CTA telescopes search for? They search the sky for gamma rays. What are gamma rays? Gamma rays are like X-rays, which are used to see human bones in the hospitals, but much more energetic (Note for educators: gamma rays are the most energetic light -electromagnetic radiation- that exists in the Universe. Light can be classified according to its energy, which is known as the electromagnetic spectrum.
    [Show full text]
  • Recycling' a Star (W/Animations) 21 May 2009
    The cosmos is green: Researchers catch nature in the act of 'recycling' a star (w/Animations) 21 May 2009 survey has found many new pulsars, but this one is truly special -- it is a very freshly 'recycled' pulsar that is emerging straight from the recycling plant." said Archibald. The McGill researchers worked with Asst. Prof. Ingrid Stairs of UBC and Scott Ransom of NRAO as well as others from the collaboration to carry out more observations of this unusual pulsar. Pulsars are rapidly rotating, highly magnetized neutron stars, the remnants left after massive stars have exploded as supernovae. Pulsars emit lighthouse-like beams of radio waves that sweep around as the star rotates. Most rotate relatively Neutron star with accretion disk (left) drawing material slowly, ten times a second or less, and their from companion star (right). CREDIT: Bill Saxton, magnetic fields ordinarily slow them down even NRAO/AUI/NSF further over the course of millennia. Millisecond pulsars, however, rotate hundreds of times a second. (PhysOrg.com) -- For the first time, researchers "We know normal pulsars typically pulsate in the have observed a singular cosmic act of rebirth: the radio spectrum for one million to ten million years, transformation of an ordinary, slow-rotating pulsar but eventually they slow down enough to die out," into a superfast millisecond pulsar with an almost explained Kaspi. "But a few of these old pulsars get infinitely extended lifespan. 'recycled' into millisecond pulsars. They end up spinning extremely fast, and then they can pulsate The discovery was made during a large radio sky forever.
    [Show full text]
  • Observatories Combine to Crack Open the Crab Nebula 10 May 2017, by Ray Villard
    Observatories combine to crack open the Crab Nebula 10 May 2017, by Ray Villard The Crab Nebula, the result of a bright supernova explosion seen by Chinese and other astronomers in the year 1054, is 6,500 light-years from Earth. At its center is a super-dense neutron star, rotating once every 33 milliseconds, shooting out rotating lighthouse-like beams of radio waves and light—a pulsar (the bright dot at image center). The nebula's intricate shape is caused by a complex interplay of the pulsar, a fast-moving wind of particles coming from the pulsar, and material originally ejected by the supernova explosion and by the star itself before the explosion. This image combines data from five different telescopes: The VLA (radio) in red; Spitzer Space Telescope (infrared) in yellow; Hubble Space Telescope (visible) in green; XMM-Newton (ultraviolet) in blue; and Chandra X-ray Observatory (X-ray) in purple. The new VLA, Hubble, and Chandra observations An image of the Crab Nebula, a supernova remnant that all were made at nearly the same time in November was assembled by combining data from five telescopes of 2012. A team of scientists led by Gloria Dubner spanning nearly the entire breadth of the of the Institute of Astronomy and Physics (IAFE), electromagnetic spectrum: the Very Large Array, the the National Council of Scientific Research Spitzer Space Telescope, the Hubble Space Telescope, (CONICET), and the University of Buenos Aires in the XMM-Newton Observatory, and the Chandra X-ray Argentina then made a thorough analysis of the Observatory. Credit: NASA, ESA, NRAO/AUI/NSF and G.
    [Show full text]
  • GMRT Observing Application
    GMRT Observing Application CYCLE 15 DEADLINE: Monday, July 07, 2008 Proposal Code: INSTRUCTIONS: Each numbered item must have an entry or N/A or NA SEND TO: GMRT Time Allocation Committee, NCRA–TIFR, Post Bag 3, Ganeshkhind, Pune 411 007, INDIA Received: Email: [email protected] (1) Date of preparing this application: July 6, 2008 (2) Title of Proposal: The first low radio frequencies study of the intriguing SNR G347.3−0.5 (RX J1713.7−3946) (3) AUTHORS† INSTITUT ION Will come Email (needed for PI & Co-PIs) Nationality * to GMRT? FABIO ACERO CEA Saclay, France Yes [email protected] French Mamta Pandey-Pommier Univeristy of Leiden No [email protected] Indian Martin Ortega IAFE, Argentina No [email protected] Argentine Gloria Dubner IAFE, Argentina No [email protected] Argentine Gabriela Castelletti IAFE, Argentina No [email protected] Argentine Elsa Giacani IAFE, Argentina No [email protected] Argentine Alexandre Marcowith Universit´eMontpellier II No [email protected] French Yves Gallant Universit´eMontpellier II No [email protected] Canadian Armand Fiasson Universit´eMontpellier II No armand.fi[email protected] French Jean Ballet CEA Saclay, France No [email protected] French Anne Decourchelle CEA Saclay, France No [email protected] French † Please write the PI’s name in CAPITAL LETTERS. * Nationality is mandatory to obtain official clearance, only for non-Indian nationals coming for observations. (4) Related previous GMRT proposal number(s): None (5) Contact author Address: M. Pandey-Pommier, Leiden Observatory, Leiden University, Oort Gebouw, P.O.
    [Show full text]
  • Long-Term Evolution and Physical Properties of Rotating Radio Transients
    LONG-TERM EVOLUTION AND PHYSICAL PROPERTIES OF ROTATING RADIO TRANSIENTS by Ali Arda Gençali Submitted to the Graduate School of Engineering and Natural Sciences in partial fulfillment of the requirements for the degree of Master of Science Sabancı University June 2018 c Ali Arda Gençali 2018 All Rights Reserved LONG-TERM EVOLUTION AND PHYSICAL PROPERTIES OF ROTATING RADIO TRANSIENTS Ali Arda Gençali Physics, Master of Science Thesis, 2018 Thesis Supervisor: Assoc. Prof. Ünal Ertan Abstract A series of detailed work on the long-term evolutions of young neutron star pop- ulations, namely anomalous X-ray pulsars (AXPs), soft gamma repeaters (SGRs), dim isolated neutron stars (XDINs), “high-magnetic-field” radio pulsars (HBRPs), and central compact objects (CCOs) showed that the X-ray luminosities, LX, and the rotational prop- erties of these systems can be reached by the neutron stars evolving with fallback discs and conventional dipole fields. Remarkably different individual source properties of these populations are reproduced in the same model as a result of the differences in their initial conditions, magnetic moment, initial rotational period, and the disc properties. In this the- sis, we have analysed the properties of the rotating radio transients (RRATs) in the same model. We investigated the long-term evolution of J1819–1458, which is the only RRAT detected in X-rays. The period, period derivative and X-ray luminosity of J1819–1458 11 can be reproduced simultaneously with a magnetic dipole field strength B0 ∼ 5 × 10 G on the pole of the neutron star, which is much smaller than the field strength inferred from the dipole-torque formula.
    [Show full text]
  • Pos(MQW7)105 Cygni Γ Radio flaring Ce
    The compact radio counterpart of IGR J20187+4041 near the flaring source AGL 2021+4029 and 3EG J2020+4017 Zsolt Paragi PoS(MQW7)105 JIVE, Dwingeloo, Netherlands MTA Research Group for Physical Geodesy and Geodynamics, Penc, Hungary E-mail: [email protected] Alfonso Trejo Cruz CRyA-UNAM, Morelia, Mexico E-mail: [email protected] Elsa Giacani IAFE, Buenos Aires, Argentina E-mail: [email protected] Gloria Dubner IAFE, Buenos Aires, Argentina E-mail: [email protected] Andrei M. Bykov Ioffe Institute, St. Petersburg, Russia E-mail: [email protected] Huib J. van Langevelde JIVE, Dwingeloo, Netherlands Sterrewacht Leiden, Leiden University, Netherlands E-mail: [email protected] We present radio results from short e-EVN (EuropeanVLBI network) observations of the counter- part to IGR J20187+4041, a hard X-ray source projected against the γ Cygni supernova remnant (SNR). The brightest unidentified EGRET source 3EG J2020+4017 is also located in the γ Cygni region, though its relation to IGR J20187+4041 has not been well established yet. The e-EVN observations were carried out following the AGILE detection of gamma-ray flaring activity in the region. Our observations show that the radio counterpart to the IGR source has a compact structure on the ∼10 mas scales that could be related to a compact object, but no radio flaring activity has been observed. e-VLBI∗is a technique which makes it possible to image the structure of radio sources at the highest angular resolution on a very short timescale. VII Microquasar Workshop: Microquasars and Beyond September 1-5 2008 Foca, Izmir, Turkey ∗e-VLBI developments in Europe are supported by the EC DG-INFSO funded Communication Network De- c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence.
    [Show full text]
  • 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.
    [Show full text]
  • ÉMILIE PARENT Email: [email protected] Ph.D
    ÉMILIE PARENT Email: [email protected] Ph.D. Candidate, Department of Physics, McGill University, 3600 rue University, Montreal QC, H3A 2T8, Canada EDUCATION . ​ Candidate for Ph.D., Physics, McGill University 2017 - present Supervisor: Prof. Victoria Kaspi Graduation expected by summer 2021 M.Sc., Physics, McGill University 2015 - 2017 Thesis: A Search for Long-Period Pulsars with a Fast-Folding Algorithm in the PALFA Survey Supervisor: Prof. Victoria Kaspi B.Sc. (Hons.) Physics, Bishop's University 2012 - 2015 Thesis: Light-Curves Calibration of Type Ia Supernovae Supervisor: Prof. Lorne Nelson Diplôme d'étude collégial en Sciences de la nature, Cégep de Sherbrooke 2009 - 2011 RESEARCH . ​ Interests: Pulsars and Fast Radio Bursts searching, software development & searching pipelines, pulsar timing and ​ population studies, formation and evolution of millisecond pulsars and binary systems PALFA Survey 2015 - present ● Lead and coordinate timing efforts (proposal writing, observation planning, data management, analyses, publication, etc.) ● Lead of searching pipeline operation and development ● Survey and timing-data quality monitoring, and related communications with Arecibo ● Act as liaison with the CHIME/Pulsar and CHIME/FRB teams for collaborative data sharing purposes ● Sensitivity analysis of the survey to long-period pulsars ● Timing analysis of regular pulsars and millisecond pulsars, and searching for high-energy pulsations Green Bank Northern Celestial Cap Pulsar Survey 2017 - present ​ ● Maintenance of the survey public
    [Show full text]
  • (NASA/Chandra X-Ray Image) Type Ia Supernova Remnant – Thermonuclear Explosion of a White Dwarf
    Stellar Evolution Card Set Description and Links 1. Tycho’s SNR (NASA/Chandra X-ray image) Type Ia supernova remnant – thermonuclear explosion of a white dwarf http://chandra.harvard.edu/photo/2011/tycho2/ 2. Protostar formation (NASA/JPL/Caltech/Spitzer/R. Hurt illustration) A young star/protostar forming within a cloud of gas and dust http://www.spitzer.caltech.edu/images/1852-ssc2007-14d-Planet-Forming-Disk- Around-a-Baby-Star 3. The Crab Nebula (NASA/Chandra X-ray/Hubble optical/Spitzer IR composite image) A type II supernova remnant with a millisecond pulsar stellar core http://chandra.harvard.edu/photo/2009/crab/ 4. Cygnus X-1 (NASA/Chandra/M Weiss illustration) A stellar mass black hole in an X-ray binary system with a main sequence companion star http://chandra.harvard.edu/photo/2011/cygx1/ 5. White dwarf with red giant companion star (ESO/M. Kornmesser illustration/video) A white dwarf accreting material from a red giant companion could result in a Type Ia supernova http://www.eso.org/public/videos/eso0943b/ 6. Eight Burst Nebula (NASA/Hubble optical image) A planetary nebula with a white dwarf and companion star binary system in its center http://apod.nasa.gov/apod/ap150607.html 7. The Carina Nebula star-formation complex (NASA/Hubble optical image) A massive and active star formation region with newly forming protostars and stars http://www.spacetelescope.org/images/heic0707b/ 8. NGC 6826 (Chandra X-ray/Hubble optical composite image) A planetary nebula with a white dwarf stellar core in its center http://chandra.harvard.edu/photo/2012/pne/ 9.
    [Show full text]