Broadband Emission of Magnetar Wind Nebulae
|
|
- Alaina Patrick
- 5 years ago
- Views:
Transcription
1 Broadband Emission of Magnetar Wind Nebulae Shuta Tanaka ICRR, The Univ. of Tokyo 29, Oct., 2015, TeVPA Kashiwa 1
2 Contents 1. Introduction 2. Spectral Evolution of young PWNe 3. A Spectral Model of MWNe 2
3 Pulsars in PWNe Crab (Chandra) l Pulse lumi. ~ a few % x L spin Most of L spin releases as pulsar wind! l ~ 50 of 2000 pulsars have observable PWNe. (L spin > erg/s). P - P diagram erg/s 3C58 (Chandra + VLA) L spin = IΩ Ω l Bow-shock PWNe are around MSP of L spin < erg/s How about other classes of pulsar? 3
4 Magnetar Wind Nebulae? PWNe are found around High-B radio pulsar. One of young TeV PWN around high-b radio pulsar Observed extended emission may be dust-scattering halo for 1E (e.g., Olausen+11) 4
5 Magnetar Wind l Magnetars have large surface B-field ( > 3x10 14 G) and some have L x > L spin B-powered emission?. l Magnetars have P Wind loss Ṁ wind R LC L wind c = L spin for RPP L X [erg/s] Angular momentum loss!! L x = L spin Photon loss Ṁ ph (R NS + ) L ph B c NS [G] L spin [erg/s] Even L x > L spin, wind angular momentum loss would dominate for magnetars from this simple estimate. 5
6 What We Learn from MWN l PWN spectrum tells us spin evolution of pulsar => How about MWN? l Does a millisecond magnetar exist? l Difference of wind properties from rotation powered pulsar (RPP). l magnetization: σ? pair multiplicity: κ? l Testing fall-back disk model of magnetar. l Disk model does not produce MWN because no wind flows out from magnetosphere. 6
7 Contents 1. Introduction 2. Spectral Evolution of young PWNe 3. A Spectral Model of MWNe 7
8 Spectral Evolution Model l PWN as uniform sphere l Constant rate of Expansion applicable to young (<<10kyr) PWN R PWN = V PWN x t e, B l Introduce a parameter η satisfies (no hadron) L spin = L e± + L B = (1-η) L spin + ηl spin l B-field evolution as energy conservation t 0 L B (t ')dt ' Total magnetic energy injected = 4π 3 R 3 B 2 (t) PWN 8π Magnetic energy inside PWN 8
9 Spectral Evolution Model l Injection of non-thermal e ± plasma (broken power-law) (1-η)L spin = L e± = Q inj γmc 2 dγ logn γ -p1 γ L -p2 e γ min γ b γ max logγ l Evolution of energy distribution of e ± t Radiative & adiabatic cooling N( γ, t) +! γ ( γ, t) N( γ, t) = Qinj( γ, t) γ Injection from pulsar Calculate Syn. & IC spectral evolution 9
10 Crab Most observed & studied object (one parameterη) Spectral Evolution of the Crab Nebula l Observed flux@1kyr η~ 5 x 10-3 (85μG) synchrotron Inverse Compton l SSC dominates in γ-rays. S.T.& radio[%/yr] Opt.[%/yr] Model Obs l Flux evolution is consistent. Model can reproduce observations 10
11 G G Young PWNe Chandra Park+07 G G Applicable to other young69 PWNe < 10kyr G Chandra G νfν[ergs/cm2/sec] G G (Model 2) 3C Kaspi B SYN IC/CMB IC/IR IC/OPT SSC Total Porquet ν[hz] 1025 S.T.&Takahara11 Park+10 S.T.&Takahara 13 Figure 5.10: Model spectrum of G at tage = 1.0kyr for model 2, where we ignore the One-zone model is enough to get distribution (right panel) G with the use of the same parameters as in Figure 5.8. l ofmean B-field inside PWN. While the synchrotron flux decreases with time, the inverse Compton flux increases. This l spin-evolution of central pulsars feature is due to the decrease of the magnetic field strength with time and to the increase of the particle number as seen in the right panel. Because the energy injection from the pulsar will l predictions to γ-ray flux continue till the time t τ = 3.9kyr, the particles in the PWN increase (see the discussion in -3 for lin the η~10 allof theexcept Section in details). left panel, we can see the evolution synchrotron cooling for Kes 75 infrared observation (Gallant & Tuffs, 1998) in the spectral fitting. Used and obtained parameters Kes 75 3C58 are tabulated in Table C58 (Chandra + VLA) Kumar & Safi-Harb08 0 break frequency νc (t) (from Hz at 300 yr to 1017 Hz at 10 kyr) as is predicted by 11
12 Contents 1. Introduction 2. Spectral Evolution of young PWNe 3. A Spectral Model of MWNe 12
13 Simplified One-zone Model l Spin-down evolution l Expansion of MWN l B-field inside MWN l e ± injection logq γ -p1 L e γ -p2 γ min γ b γ max logγ t c = n 1 (t age + 0 ) 2 L spin (t) L spin,now t t age R(t) =R now B(t) =B now L e ±(t) n(,t)+ t t t age R L spin (t) e ± energy distribution e, B n(,t) =Q(,t) adiabatic + synchrotron + inverse Compton coolings t t age n < α R < -1.0, -5 < α B < -3 from past studies B 2 t age n+1 n 1 13
14 Kes 75 Young RPP with magnetar-like activity L spin = 8x10 36 erg/s, B NS = 4.8x10 13 G, τ c = 0.7kyr model 1 model 2 d 6kpc 10.6kpc τ 0 0.2kyr 3yr E rot 1.5x10 48 erg 2.1x10 50 erg B PWN 20μG 24μG η 5x10-5 6x
15 νf ν [ergs/cm 2 /sec] AXP 1E Assuming (u IR, u opt ) = (1.0, 2.0) [ev/cc] L spin = 1x10 35 erg, B NS = 2.2x10 14 G, τ c = 1.4kyr AXP 1E (Model 1) (B 1, γ b, p 2 ) = (3µG, 10 6, -2.6) SYN IC/CMB IC/IR IC/OPT TOTAL XMM-Newton ν[hz] CTA l Results are insensitive to α B & α R. l X-ray upper limit gives constraints B now < 25μG. l CTA would detect MWN around 1E when B now < 3 μg & u IR > 1.0eV/cc l η<<10-3 is consistent with Kes 75. l P 0 < 100msec is presumed. νf ν [ergs/cm 2 /sec] AXP 1E (Model 2) (B 1, γ b, p 2 ) = (25µG, 10 4, -2.6) SYN IC/CMB IC/IR IC/OPT TOTAL XMM-Newton ν[hz] CTA 15
16 Summary l Pulsar & Pulsar Wind Nebula l Most of L spin lost by pulsar wind l σ- & κ- problem about physics of pulsar magnetosphere l One-zone model of PWNe tells us spin-evolution of central pulsars l A Spectral model of MWNe l Angular momentum loss of magnetar => magnetar wind? l Deep obs. of 1E by CTA can examine the hypothesis. l η<<10-3 is consistent with High-B radio pulsars. l Constraint on P 0 is not strong < 100msec l Detections of MWN in multi-wavelength are required to constrain magnetar evolution properties. 16
Spatial Profile of the Emission from Pulsar Wind Nebulae with steady-state 1D Modeling
Spatial Profile of the Emission from Pulsar Wind Nebulae with steady-state 1D Modeling Wataru Ishizaki ( Department of Physics, Graduate School of Science, The University of Tokyo ) Abstract The pulsar
More informationPulsar Wind Nebulae: A Multiwavelength Perspective
Pulsar Wind Nebulae: Collaborators: J. D. Gelfand T. Temim D. Castro S. M. LaMassa B. M. Gaensler J. P. Hughes S. Park D. J. Helfand O. C. de Jager A. Lemiere S. P. Reynolds S. Funk Y. Uchiyama A Multiwavelength
More informationParticle acceleration and pulsars
Meudon, nov. 2013 p. 1/17 Particle acceleration and pulsars Fabrice Mottez LUTH - Obs. Paris-Meudon - CNRS - Univ. Paris Diderot Meudon, nov. 2013 p. 2/17 Pulsars (PSR) and pulsar wind nebulae (PWNe) Mostly
More informationObservations of. Pulsar Wind Nebulae
Observations of Pulsar Wind Nebulae I. Injection Spectrum I. Late-Phase Evolution II. PWNe and Magnetars PWNe and Their SNRs PWN Shock Reverse Shock Forward Shock Pulsar Wind Pulsar Termination Shock PWN
More informationCooling Limits for the
Cooling Limits for the Page et al. 2004 Youngest Neutron Stars Cooling from the Youngest NSs SNR Zone NSs younger than ~50 kyr offer strong constraints on rapid cooling - the associated physical processes
More informationX-ray emission properties vary with spin-down age. Crab-like pulsars (< 10 4 yrs)
X-ray emission properties vary with spin-down age Crab-like pulsars (< 10 4 yrs) X-ray emission properties vary with spin-down age Crab-like pulsars (< 10 4 yrs) Cooling neutron stars ( ~10 5-10 6 yrs)
More informationPulsar Wind Nebulae as seen by Fermi-Large Area Telescope
Pulsar Wind Nebulae as seen by Fermi-Large Area Telescope Marie-Hélène Grondin Centre d'etudes Nucléaires de Bordeaux- Gradignan SNR/PWN Workshop Montpellier, 2010 June 1 th M.-H. Grondin, SNR/PWN Wokshop,
More informationLecture 3 Pulsars and pulsar wind nebulae
Lecture 3 Pulsars and pulsar wind nebulae Pulsars Characteristic parameters Pulsar wind nebulae Properties Evolution Exotic central compact objects - Magnetars The Crab Pulsar http://www.jb.man.ac.uk/~pulsar/education/sounds/sounds.html
More informationProgress in Pulsar detection
Progress in Pulsar detection With EINSTEIN & EXOSAT: 7 radio pulsars detected in X-rays With ROSAT, ASCA & BSAX: 33 radio pulsars detected in X-rays After ~8 yrs with XMM & Chandra: 81 radio pulsars detected
More informationRemnants and Pulsar Wind
High Energy Supernova Remnants and Pulsar Wind Nebulae F. Giordano Dipartimento Interateneo di Fisica and INFN Sez. Bari For the Fermi-LAT Collaboration Scineghe 2010 The Afterlife of a star IC443 Crab
More informationFermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars
Fermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars Marie-Hélène Grondin CENBG, Bordeaux (France) on behalf of the Fermi-LAT Collaboration and the Pulsar Timing
More informationPulsar Wind Nebulae. Pennsylvania State University. General outlook Chandra results Polarization in radio and optical X-ray polarization
Pulsar Wind Nebulae George Pavlov & Oleg Kargaltsev Pennsylvania State University General outlook Chandra results Polarization in radio and optical X-ray polarization Pulsar Wind Nebulae: extended objects
More informationComposite Supernova Remnants: Multiwavelength Observations and Theoretical Modelling
Composite Supernova Remnants: Multiwavelength Observations and Theoretical Modelling Okkie de Jager & Stefan Ferreira (NWU, South Africa) Regis Terrier & Arache Djannati-Ataï (Univ. of Paris VII, France)
More informationThe Time Evolution of Pulsar Wind Nebulae
The Time Evolution of Pulsar Wind Nebulae Okkie de Jager, S. Ferreira (NWU, South Africa) Science with the New Generation of High Energy Gamma-Ray Experiments (6th Workshop), Padova 8 10 October 2008 Contents
More informationHESS discovery of VHE γ-ray emission of a remarkable young composite SNR
HESS discovery of VHE γ-ray emission of a remarkable young composite SNR Arache Djannati-Ataï*, V. Marandon, R. Chaves, R. Terrier & N. Komin for the HESS Collaboration *Laboratoire d'astroparticule et
More informationH.E.S.S. Unidentified Gamma-ray Sources in a Pulsar Wind Nebula Scenario And HESS J
H.E.S.S. Unidentified Gamma-ray Sources in a Pulsar Wind Nebula Scenario And HESS J1303-631 Matthew Dalton Humboldt University at Berlin For the H.E.S.S. Collaboration TeV Particle Astrophysics, Paris.
More informationExtended X- ray emission from PSR B /LS 2883 and other gamma- ray binaries
Extended X- ray emission from PSR B1259-63/LS 2883 and other gamma- ray binaries George Pavlov (Pennsylvania State University) Oleg Kargaltsev (George Washington University) Martin Durant (University of
More informationX-ray Properties of Rotation Powered Pulsars and Thermally Emitting Neutron Stars
X-ray Properties of Rotation Powered Pulsars and Thermally Emitting Neutron Stars George Pavlov (Penn State; Polytech.Univ SPb) Collaborators: Oleg Kargaltsev (George Washington Univ.) Bettina Posselt
More informationX-ray and multiwavelength observations of pulsarwind
X-ray and multiwavelength observations of pulsarwind nebulae. Oleg Kargaltsev (George Washington University) Collaborators: Martin Durant ( University of Toronto) George Pavlov (Penn State University)
More informationPulsar Winds in High Energy Astrophysics
Pulsar Winds in High Energy Astrophysics Dmitry Khangulyan Institute of Space and Astronautical Science (ISAS/JAXA) The extreme Universe viewed in very high energy gamma-rays, Kashiwa 09/25/2012 OUTLINE
More informationThe Neutron Star Zoo. Stephen C.-Y. Ng ( 吳志勇 ) HKU
The Neutron Star Zoo Stephen C.-Y. Ng ( 吳志勇 ) HKU Overview Introduction to neutron stars Different classes of neutron stars: Radio Pulsars MSPs Magnetars DINS CCOs Unification 6/12/2017 NAOC Stephen Ng
More informationA Detailed Study of. the Pulsar Wind Nebula 3C 58
A Detailed Study of Collaborators: D. J. Helfand S. S. Murray S. Ransom F. D. Seward B. M. Gaensler E. V. Gotthelf E. van der Swaluw the Pulsar Wind Nebula 3C 58 Pulsar Wind Nebulae Young NS powers a particle/magnetic
More informationX-ray Observations of Rotation Powered Pulsars
X-ray Observations of Rotation Powered Pulsars George Pavlov (Penn State) Oleg Kargaltsev (George Washington Univ.) Martin Durant (Univ. of Toronto) Bettina Posselt (Penn State) Isolated neutron stars
More informationNew measurements of pulsar braking indices (obtained via phase-coherent timing)
New measurements of pulsar braking indices (obtained via phase-coherent timing) Collaborators: Vicky Kaspi (McGill) Fotis Gavriil (GSFC) Richard Manchester (ATNF) Eric Gotthelf (Columbia) Lucien Kuiper
More informationFermi Large Area Telescope:
Fermi Large Area Telescope: Early Results on Pulsars Kent Wood Naval Research Lab kent.wood@nrl.navy.mil for the Fermi LAT Collaboration Tokyo Institute of Technology 7 March 2009 K. Wood (NRL) 1/30 Fermi
More informationX-ray and Gamma-ray. Emission Pulsars and Pulsar Wind Nebulae. K.S. Cheng Department of Physics University of Hong Kong Hong Kong, China
X-ray and Gamma-ray Emission Pulsars and Pulsar Wind Nebulae K.S. Cheng Department of Physics University of Hong Kong Hong Kong, China X-ray luminosity (L x ) vs spin-down power (L sd ) Becker and Trumper
More informationPulsars and Pulsar-Wind Nebulae: TeV to X-Ray Connection. Oleg Kargaltsev (University of Florida) George Pavlov (Penn State University)
Pulsars and Pulsar-Wind Nebulae: TeV to X-Ray Connection Oleg Kargaltsev (University of Florida) George Pavlov (Penn State University) Pulsar Wind Nebulae. All active pulsars emit relativistic winds c
More informationMagnetic Fields in Supernova Remnants and Pulsar Wind Nebulae: Deductions from X ray (and gamma ray) Observations
Magnetic Fields in Supernova Remnants and Pulsar Wind Nebulae: Deductions from X ray (and gamma ray) Observations Stephen Reynolds (NC State U) 1. Introduction 2. Determining B in SNRs SED modeling Thin
More informationCosmic Ray Electrons and GC Observations with H.E.S.S.
Cosmic Ray Electrons and GC Observations with H.E.S.S. Christopher van Eldik (for the H.E.S.S. Collaboration) MPI für Kernphysik, Heidelberg, Germany TeVPA '09, SLAC, July 2009 The Centre of the Milky
More informationProbing the Pulsar Wind in the TeV Binary System
Probing the Pulsar Wind in the TeV Binary System -PSR B1259-63/SS2883- Jumpei Takata (University of Hong Kong) Ronald Taam (TIARA, Taiwan) 1 Outline 1, Introduction -TeV binaries -Fermi observation -PSR
More informationShota Kisaka (ICRR, Univ. of Tokyo) with Norita Kawanaka (Hebrew Univ. of Jerusalem) Toshio Terasawa (ICRR, Univ. of Tokyo) Takayuki Saito (MPI)
Shota Kisaka (ICRR, Univ. of Tokyo) with Norita Kawanaka (Hebrew Univ. of Jerusalem) Toshio Terasawa (ICRR, Univ. of Tokyo) Takayuki Saito (MPI) Outline 1. IntroducHon 2. AcceleraHon region : Pairstarved
More informationStudies of Pulsar Wind Nebulae in TeV γ-rays with H.E.S.S.
Studies of Pulsar Wind Nebulae in TeV γ-rays with H.E.S.S. Y.A. Gallant 1, S. Klepser, K. Valerius, M. Mayer, M. Tsirou, R. Terrier, R. Zanin for the H.E.S.S. Collaboration 1 LUPM, CNRS/IN2P3, U. Montpellier,
More informationすざく ( と XMM) による広がった TeV ガンマ 線放射 VER J の X 線観測 (3) Suzaku (and XMM) Observation of the extended TeV gamma-ray source VER J (3)
すざく ( と XMM) による広がった TeV ガンマ 線放射 VER J2019+368 の X 線観測 (3) Suzaku (and XMM) Observation of the extended TeV gamma-ray source VER J2019+368(3) September 23, 2016@JPS meeting, Miyazaki Tsunefumi Mizuno (Hiroshima
More informationProbing Pulsar Winds With X-rays!
Probing Pulsar Winds With X-rays! Collaborators:! Bryan Gaensler! Steve Reynolds! David Helfand! Stephen Ng! Anne Lemiere! Okkie de Jager! Stephanie LaMassa! Jack Hughes! PWNe and Their SNRs! PWN Shock
More informationWhat We Can Learn from High-Resolution Observations of Pulsar Wind Nebulae
What We Can Learn from High-Resolution Observations of Pulsar Wind Nebulae Noel Klingler The George Washington University Oleg Kargaltsev The George Washington University George Pavlov Pennsylvania State
More informationPulsar Wind and pulsar wind nebulae
Pulsar Wind and pulsar wind nebulae Takata Jumpei 1 Outline S1, Pulsar Wind (PW) and Pulsar Wind Nebula(PWN) around isolate pulsars. -PWN nebula around the Crab pulsar -Formation of PW and PWNe -Kennel
More informationVictoria Kaspi (McGill University, Montreal, Canada)
Victoria Kaspi (McGill University, Montreal, Canada) C. Espinoza M. Gonzalez M. Kramer M. Livingstone A. Lyne M. McLaughlin S. Olausen C.Y. Ng G. Pavlov W. Zhu Victoria Kaspi (McGill University, Montreal,
More informationMillisecond Pulsar Populations in Globular Clusters
Millisecond Pulsar Populations in Globular Clusters David C. Y. Hui Department of Astronomy & Space Science Chungnam National University 1. Introduction 2. Dynamical formation of millisecond pulsars (MSPs)
More informationRecent Observations of Supernova Remnants
1 Recent Observations of Supernova Remnants with VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (http://veritas.sao.arizona.edu) 2 Contents Supernova Remnants
More informationInfrared-Optical observations of magnetars
Infrared-Optical observations of magnetars Mikio Morii Tokyo Institute of Technology 2012.09.01 @ Rikkyo Univ. Contents Search for Near-Infrared Pulsation of the AXP 4U 0142+61 M. M., N. Kobayashi, N.
More information* What are Jets? * How do Jets Shine? * Why do Jets Form? * When were Jets Made?
* What are Jets? * How do Jets Shine? * Why do Jets Form? * When were Jets Made? 1 * Galaxies contain massive black holes which power AGN * Gas accretes through a magnetized disk * Blazars are relativistically
More informationMagnetic Fields in Pulsar Wind Nebulae: an observer s point of view
Magnetic Fields in Pulsar Wind Nebulae: an observer s point of view Dr. Roland Kothes Dominion Radio Astrophysical Observatory Emergin Technologies National Science Infrastructure National Research Council
More informationPulsar Winds. John Kirk. Max-Planck-Institut für Kernphysik Heidelberg, Germany. < > p.1/18
Pulsar Winds John Kirk Max-Planck-Institut für Kernphysik Heidelberg, Germany < > p.1/18 About 50 years after... The Crab Nebula Central star is source of particles and magnetic field (Piddington 1957)
More informationStudy of the very high energy gamma-ray diffuse emission in the central 200 pc of our galaxy with H.E.S.S.
Study of the very high energy gamma-ray diffuse emission in the central 200 pc of our galaxy with H.E.S.S. Lemière A., Terrier R., Jouvin L., Marandon V, Lefranc V., Viana A. For the H.E.S.S. Collaboration
More informationFermi-LAT and WMAP observations of the SNR Puppis A
Fermi-LAT and WMAP observations of the SNR Puppis A Marie-Hélène Grondin & Marianne Lemoine-Goumard Hewitt, J., Grondin, MH, et al. 2012, ApJ, accepted (arxiv:1210.4474) MODE-SNR-PWN workshop - November
More informationHigh Energy Emissions from the PSR /SS2883 Binary System
High Energy Emissions from the PSR1259 63/SS2883 Binary System A. Kawachi, T. Naito and S. Nagataki Institute for Cosmic Ray Research, University of Tokyo, Chiba 277-8582, Japan Faculty of Management Information,
More informationParticle acceleration during the gamma-ray flares of the Crab Nebular
Particle acceleration during the gamma-ray flares of the Crab Nebular SLAC Accelerator seminar SLAC 15 June 2011 R. Buehler for the LAT collaboration and A. Tennant, E. Costa, D. Horns, C. Ferrigno, A.
More informationGAMMA-RAYS FROM MASSIVE BINARIES
GAMMA-RAYS FROM MASSIVE BINARIES W lodek Bednarek Department of Experimental Physics, University of Lódź, Poland 1. Sources of TeV gamma-rays PSR 1259+63/SS2883 - (HESS) LS 5039 - (HESS) LSI 303 +61 o
More informationPulsars with MAGIC. Jezabel R. Garcia on behalf of the MAGIC collaboration
Pulsars with MAGIC Jezabel R. Garcia on behalf of the MAGIC collaboration Introduction to MAGIC - Energy range: ~50 GeV to 50 TeV - Energy resolution: 15% (@1TeV) 23% (@100 GeV) - Angular resolution: 0.06
More informationSynchrotron Radiation: II. Spectrum
Synchrotron Radiation: II. Spectrum Massimo Ricotti ricotti@astro.umd.edu University of Maryland Synchrotron Radiation: II. Spectrum p.1/18 ds=v dt_em dt=ds cos(theta)/c=v/c cos(theta)dt_em Synchrotron
More informationCrab Pulsar. Chandra Image of the Crab Nebula. Crab is the most famous pulsar, which is studied in detail across the entire energy spectrum
Crab Pulsar Chandra Image of the Crab Nebula Crab is the most famous pulsar, which is studied in detail across the entire energy spectrum Conventional view on the Crab Pulsar Related Emitting Zones Pulsar(Massaro+)
More informationProbing Pulsar Winds with Gamma Rays
Probing Pulsar Winds with Gamma Rays Dmitry Khangulyan Institute of Space and Astronautical Science (ISAS/JAXA) in coll. with Felix Aharonian&Sergey Bogovalov International School on Neutron Star Matter
More information12 Pulsars: overview and some physics
Physics 426 Notes Spring 2009 59 12 Pulsars: overview and some physics Carroll & Ostlie present the basic picture in some detail; another good reference is Longair s High Energy Astrophysics. In these
More informationSpectral Analysis of the Double Pulsar PSR J with XMM-Newton
Spectral Analysis of the Double Pulsar PSR J0737-3039 with XMM-Newton * E. Egron, A. Pellizzoni, M.N. Iacolina, A. Pollock, et al. INAF - Osservatorio Astronomico di Cagliari, Italy * ESAC, Madrid, Spain
More informationTeV Gamma Rays from Synchrotron X-ray X
TeV Gamma Rays from Synchrotron X-ray X SNR Kyoto University Department of Physics Toru Tanimori (CANGAROO Collaboration) Introduction TeV Gamma Ray emissions in celestial objects Results of CANGAROO The
More informationVERITAS Observations of Supernova Remnants
VERITAS Observations of Supernova Remnants Reshmi Mukherjee 1 for the VERITAS Collaboration 1 Barnard College, Columbia University Chandra SNR Meeting, Boston, Jul 8, 2009 Outline (Quick) introduction
More informationExploring the powering source of the TeV X-ray binary LS 5039
Exploring the powering source of the TeV X-ray binary LS 5039 Javier Moldón Marc Ribó Josep Maria Paredes Josep Martí (Univ. Jaén) Maria Massi (MPIfR) 9th European VLBI Network Symposium Bologna, Italy
More informationMagnetohydrodynamics of pulsar winds and plerions Yuri Lyubarsky
Magnetohydrodynamics of pulsar winds and plerions Yuri Lyubarsky Ben-Gurion University, Israel Pulsar magneto sphere e Pulsar wind +, e, (ions?), electro-magnetic fields Pulsar wind nebula j j v B v v
More informationGamma-ray binaries as pulsars spectral & variability behaviour Guillaume Dubus. Laboratoire d Astrophysique de Grenoble UMR 5571 UJF / CNRS
Gamma-ray binaries as pulsars spectral & variability behaviour Guillaume Dubus Laboratoire d Astrophysique de Grenoble UMR 5571 UJF / CNRS Image: Mirabel 2006 1 Pulsars & massive stars Young pulsars, magnetic
More informationPulsars & Double Pulsars:! A Multiwavelength Approach!
Pulsars & Double Pulsars:! A Multiwavelength Approach! Marta Burgay INAF, Cagliari Observatory! X-Ray Astronomy 2009 Bologna 08/09/2009! Spin-Powered Pulsars! Radio! High Energy! RRATs! Magnetars! XDINS!
More informationarxiv: v1 [astro-ph] 7 Nov 2007
Recent Progress in Studies of Pulsar Wind Nebulae Patrick Slane arxiv:0711.1002v1 [astro-ph] 7 Nov 2007 Harvard-Smithsonian Center for Astrophysics Abstract. The synchrotron-emitting nebulae formed by
More informationThe double pulsar as Jupiter: tomography of magnetosphere and a new test of General Relativity. Maxim Lyutikov (Purdue U.)
The double pulsar as Jupiter: tomography of magnetosphere and a new test of General Relativity Maxim Lyutikov (Purdue U.) The Double Pulsar: sixth most important scientific discovery of 2004 (Science)
More informationPulsars. The maximum angular frequency of a spinning star can be found by equating the centripetal and gravitational acceleration M R 2 R 3 G M
Pulsars Pulsating stars were discovered in 1967 via radio dipole antennae by Jocelyn Bell and Anthony Hewish Pulse period of PSR 1919+21 is 1.337 s Most pulsars have periods between 0.25 s and 2 s The
More informationThe magnetic properties of Main Sequence Stars, White Dwarfs and Neutron Stars
The magnetic properties of Main Sequence Stars, White Dwarfs and Neutron Stars Lilia Ferrario Mathematical Sciences Institute Australian National University Properties of MWDs High Field MWDs ~ 10 6-10
More informationA pulsar wind nebula associated with PSR J as the powering source of TeV J
A pulsar wind nebula associated with PSR J2032+4127 as the powering source of TeV J2032+4130 Javier Moldón Netherlands Institute for Radio Astronomy Extreme Astrophysics in an Ever-Changing Universe Crete,
More informationThe Secret Life of Neutron Stars. Jeremy Heyl Harvard-Smithsonian CfA
The Secret Life of Neutron Stars Jeremy Heyl Harvard-Smithsonian CfA The Life of a 10 M Star PNS 10 5 yr 10 6 yr 10 7 yr 10 8 yr 10 9 yr 10 10 yr PMS MS Radio Pulsars Thermal Accretion-, Nuclear-, GWpowered
More informationA few issues in CSM interaction signals (and on mass loss estimates) Keiichi Maeda
A few issues in CSM interaction signals (and on mass loss estimates) Keiichi Maeda Radio/X constraints on CSM around SNe Ia Useful limit for SN 2011fe: Mdot/v w < ~10-8 M yr -1 /100km s -1 Radio Chomiuk+
More informationDiversity of Multi-wavelength Behavior of Relativistic Jet in 3C 279 Discovered During the Fermi Era
Diversity of Multi-wavelength Behavior of Relativistic Jet in 3C 279 Discovered During the Fermi Era Rapid Variability of Blazar 3C 279 during Flaring States in 2013-2014 with Joint Fermi-LAT, NuSTAR,
More informationSupernova Remnants and Pulsar Wind Nebulae observed in TeV γ rays
Supernova Remnants and Pulsar Wind Nebulae observed in TeV γ rays NOW 2014 Conca Specchiulla, Sept 7-14, 2014 Kathrin Valerius Erlangen Centre for Astroparticle Physics Univ. Erlangen-Nürnberg KCETA Karlsruhe
More informationUHECR from Pulsars/Magnetars based on An Auroral Accelerator Model for Gamma Ray Pulsars
UHECR from Pulsars/Magnetars based on An Auroral Accelerator Model for Gamma Ray Pulsars Jonathan Arons University of California, Berkeley Bai & Spitkovsky 2010 Collaborators: N. Bucciantini, A. Spitkovsky
More informationarxiv: v1 [astro-ph.he] 5 Sep 2017
VHE gamma-ray study of the composite SNR MSH 15-52 with H.E.S.S. arxiv:1709.01422v1 [astro-ph.he] 5 Sep 2017 LUPM, CNRS-IN2P3 / University of Montpellier, France E-mail: michelle.tsirou@etu.umontpellier.fr
More informationTeV Galactic Source Physics with CTA
TeV Galactic Source Physics with CTA Yves Gallant, Matthieu Renaud LPTA, CNRS/IN2P3, U. Montpellier 2, France for the CTA consortium TeV Particle Astrophysics 2010 Multimessenger HE astrophysics session
More informationVHE γ-ray emitting pulsar wind nebulae discovered by H.E.S.S.
SLAC-PUB-13255 VHE γ-ray emitting pulsar wind nebulae discovered by H.E.S.S. Y.A. Gallant, S. Carrigan, A. Djannati-Ataï, S. Funk, J.A. Hinton, S. Hoppe, O.C. de Jager, B. Khélifi, Nu. Komin, K. Kosack,
More informationX-ray Radiation, Absorption, and Scattering
X-ray Radiation, Absorption, and Scattering What we can learn from data depend on our understanding of various X-ray emission, scattering, and absorption processes. We will discuss some basic processes:
More informationCTB 37A & CTB 37B - The fake twins SNRs
Annecy le vieux CTB 37A & CTB 37B - The fake twins SNRs LAPP Annecy CTB 37: a complex complex 843 MHz MGPS map (Green et al. 1999) Bright region in radio emission Thought to be 2 SNRs plus a bridge and
More informationThe Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley)
The Black Hole in the Galactic Center Eliot Quataert (UC Berkeley) Why focus on the Galactic Center? The Best Evidence for a BH: M 3.6 10 6 M (M = mass of sun) It s s close! only ~ 10 55 Planck Lengths
More informationWhite dwarf pulsar as Possible Cosmic Ray Electron-Positron Factories
White dwarf pulsar as Possible Cosmic Ray Electron-Positron Factories 2010 7/9 Kazumi Kashiyama (Kyoto University) Kunihito Ioka & Norita Kawanaka (KEK) arxiv:1009.1141 (submitted to PRD) http://www.nasa.gov/centers/goddard/news/topstory/2007/whitedwarf_pulsar.html
More informationPulsar Observations with the Fermi Large Area Telescope
Pulsar Observations with the Fermi Large Area Telescope First Light sky survey (4 days of exposure)) Launch: 11 June 2008 Gottfried Kanbach & Matthew Baring for the Fermi-LAT Collaboration 1 The high-energy
More informationINTEGRAL & Magnetars: a high energy approach to extreme neutron stars
INTEGRAL & Magnetars: a high energy approach to extreme neutron stars Diego Götz CEA - Saclay - Irfu/Service d Astrophysique N. Rea (UvA), S. Zane (MSSL), R. Turolla (Uni Padova), M. Lyutikov (Purdue Univ.)
More information(Anomalous) X-Ray Pulsars. Vicky Kaspi. Montreal, Canada. Stanford December 16, 2004
(Anomalous) X-Ray Pulsars Vicky Kaspi Montreal, Canada Texas @ Stanford December 16, 2004 Summary Introduction to AXPs Evidence that AXPs are magnetars Open Issues and Recent Results: IR emission Transient
More informationCosmic Pevatrons in the Galaxy
Cosmic Pevatrons in the Galaxy Jonathan Arons UC Berkeley Cosmic Rays Acceleration in Supernova Remnants Pulsar Wind Nebulae Cosmic rays Cronin, 1999, RMP, 71, S165 J(E) = AE! p, p " 2.7,1GeV < E
More informationThe 2006 Giant Flare in PKS and Unidentified TeV Sources. Justin Finke Naval Research Laboratory 5 June 2008
The 2006 Giant Flare in PKS 2155-304 and Unidentified TeV Sources Justin Finke Naval Research Laboratory 5 June 2008 Outline Part I: The SSC Model Part II: The giant flare in PKS 2155-304 Part III: Blazars
More informationYoung Neutron Stars and the Role of Magnetic Fields in their Evolution
Young Neutron Stars and the Role of Magnetic Fields in their Evolution Eric Gotthelf (Columbia University) The X-ray Universe 2011 28 June 2011, Berlin Germany Talk Outline Recent Highlights of Young Isolated
More informatione - -e + pair production in pulsar magnetospheres
e - -e + pair production in pulsar magnetospheres Kouichi HIROTANI TIARA/ASIAA-NTHU, Taiwan IPMU December 8, 2009 Crab nebula: Composite image of X-ray [blue] and optical [red] 1 Introduction: The γ-ray
More informationExtended X-ray object ejected from the PSR B /LS 2883 binary
Extended X-ray object ejected from the PSR B1259-63/LS 2883 binary Oleg Kargaltsev (George Washington University) George Pavlov (Pennsylvania State University) Jeremy Hare (George Washington University)
More informationIonization Feedback in Massive Star Formation
Ionization Feedback in Massive Star Formation Thomas Peters Institut für Theoretische Astrophysik Zentrum für Astronomie der Universität Heidelberg Ralf Klessen, Robi Banerjee (ITA, Heidelberg) Mordecai-Mark
More informationParticle Transport in Young Pulsar Wind Nebulae
Particle Transport in Young Pulsar Wind Nebulae Xiaping Tang and Roger A. Chevalier University of Virginia August 26, 2012, IAU symposium 291 Tang, Chevalier (UVA) PWN IAU 2012 1 / 12 Schematic view of
More informationarxiv: v1 [astro-ph] 12 Nov 2008
High Energy Studies of Pulsar Wind Nebulae Patrick Slane Harvard-Smithsonian Center for Astrophysics arxiv:0811.1954v1 [astro-ph] 12 Nov 2008 Abstract. The extended nebulae formed as pulsar winds expand
More informationGalactic Accelerators : PWNe, SNRs and SBs
TeV γ-ray Observations and Implications for Galactic Accelerators : PWNe, SNRs and SBs (co-chair, HESS working group on SNRs, pulsars and PWNe) LPTA, Montpellier, France Particle Acceleration in Astrophysical
More informationLecture 8&9: Pulsar Wind Nebulae (Plerions) and Gamma Ray Loud Binary Systems. 40th Saas-Fee Course: Astrophysics at Very High Energies
40th Saas-Fee Course: Astrophysics at Very High Energies Lecture 8&9: Pulsar Wind Nebulae (Plerions) and Gamma Ray Loud Binary Systems F.A. Aharonian, DIAS (Dublin) & MPIK (Heidelberg) Les Diablerets,
More informationNon-thermal emission from Magnetic White Dwarf binary AR Scorpii
Non-thermal emission from Magnetic White Dwarf binary AR Scorpii Jumpei Takata (Huazhong University of Science and Technology, China) On behalf of Y. Hui (HUST), C.-P. Hu, K.S. Cheng (HKU, HK), L.C.C.
More informationRadiative Processes in Astrophysics
Radiative Processes in Astrophysics 11. Synchrotron Radiation & Compton Scattering Eline Tolstoy http://www.astro.rug.nl/~etolstoy/astroa07/ Synchrotron Self-Absorption synchrotron emission is accompanied
More informationGamma rays from supernova remnants in clumpy environments.! Stefano Gabici APC, Paris
Gamma rays from supernova remnants in clumpy environments!! Stefano Gabici APC, Paris Overview of the talk Galactic cosmic rays Gamma rays from supernova remnants Hadronic or leptonic? The role of gas
More informationProgress of Pulsar Astronomy in the Last Decade
Progress of Pulsar Astronomy in the Last Decade David C. Y. Hui On behalf of Fermi Asian Network Department of Astronomy & Space Science Chungnam National University Center of High Energy Astrophysics
More informationarxiv:astro-ph/ v1 2 Jul 2005
Chandra Observation of the Interaction between the Hot Plasma Nebula RCW89 and the Pulsar Jet of PSR B1509 58 Y. Yatsu 1, J. Kataoka 1, N. Kawai 1, and T. Kotani 1 Tokyo Institute of Technology, 2-12-1
More informationSupernova Remnants and Cosmic. Rays
Stars: Their Life and Afterlife Supernova Remnants and Cosmic 68 th Rays Brian Humensky Series, Compton Lecture #5 November 8, 2008 th Series, Compton Lecture #5 Outline Evolution of Supernova Remnants
More informationModelling the synchrotron emission from O-star colliding wind binaries
Modelling the synchrotron emission from O-star colliding wind binaries Delia Volpi 1 1 Royal Observatory of Belgium, Ringlaan 3, 1180 Brussels, Belgium Abstract: Many early-type stars are in binary systems.
More informationThe Mystery of Fast Radio Bursts and its possible resolution. Pawan Kumar
The Mystery of Fast Radio Bursts and its possible resolution Outline Pawan Kumar FRBs: summary of relevant observations Radiation mechanism and polarization FRB cosmology Wenbin Lu Niels Bohr Institute,
More informationAstro2020 Science White Paper Prospects for the detection of synchrotron halos around middle-age pulsars
Astro2020 Science White Paper Prospects for the detection of synchrotron halos around middle-age pulsars Thematic Areas: Planetary Systems Star and Planet Formation Formation and Evolution of Compact Objects
More informationCosmic Accelerators. 2. Pulsars, Black Holes and Shock Waves. Roger Blandford KIPAC Stanford
Cosmic Accelerators 2. Pulsars, Black Holes and Shock Waves Roger Blandford KIPAC Stanford Particle Acceleration Unipolar Induction Stochastic Acceleration V ~ Ω Φ I ~ V / Z 0 Z 0 ~100Ω P ~ V I ~ V 2 /Z
More information