Short and Long Radio Bursts
|
|
- Sheila Baldwin
- 5 years ago
- Views:
Transcription
1 Short and Long Radio Bursts Binary mergers as ``naked inner engines to short and long GRBs Maurice HPM van Putten Le Studium Chair d Astrophysique Le Studium IAS Université d Orléans van Putten - PSR Workshop 008
2 Outline Radio-bursts and GRBs from rotating black holes Comparison with HETE-II and Swift data Long duration bursts from mergers with Kerr BHs Comparison with BATSE light curves Conclusions and Outlook van Putten - PSR Workshop 008
3 Stellar mass transient: 5 ms extragalactic radio burst if not instrumental! (Gilles Theureau, 008, priv. comm.) van Putten - PSR Workshop Lorimer et al., 007, Science, 38, 585
4 Stellar mass transients: GRBs 967 Discovery by Vela (US) /Konus (USSR) 99 BATSE Catalogue 997 Redshifts by Beppo-Sax 997 Afterglows by Beppo-Sax 005 Afterglows to short bursts by HETE-II 003 Long GRBs with SN: HETE II GRB03039/SN003dh (confirmed GRB98045/SN998bw) 006 Long GRB without SN: Swift event GRB06064) Present: IPN, HETE II, Swift, GLAST/Fermi van Putten - PSR Workshop 008 4
5 Black Holes with Spin Spin- energy and frame dragging van Putten - PSR Workshop 008 5
6 Orbital motion in flat and curved spacetime Orbits of any size Newton ISCO ISCO Schwarzschild Kerr van Putten - PSR Workshop 008 6
7 Magnetic Flares ( Corona Ejections ) as X-ray sources X-ray line-emission by fluorescence B R van Putten - PSR Workshop Fabian, 005, at KerrFest
8 flux R Iron line-emissions B 4keV energy Doppler line-splitting, Newtonian Splitting + beaming + gravitational redshift MCG Tanaka et al. 995 van Putten - PSR Workshop After Fabian 005 KerrFest
9 Tanaka et al. 995 Iwasawa etal. 996 R B R Kerr Schwarzschild B Compact ISCO by frame-dragging Kα line emission in MCG (Seyfert I in a low state) observed by ASCA van Putten - PSR Workshop 008 9
10 Active Nuclei from spinning black holes Spin Energy f s (Van Putten 999,008) E spin = Ω cos( λ / ) 54 = (sinλ = a / M ) E 4 0 cos( / 4) spin λ 7 H If s M M sun erg Bekenstein- Hawking Entropy S H = 4πM cos ( λ / ) Bekenstein 973; Bardeen et al. 973; Hawking, 973, Strominger & Vafa 996 Kerr BHs can radiate Penrose (969) conform the Rayleigh criterion a M > M p a H van Putten - PSR Workshop 008 0
11 Angular momentum coupling to Riemann curvature force J = ±ea ϕ F c = *R abcd J a u b u d Papapetrou 956 Blanchet, OSUC Mass Motion 008 Unfortunately, in practical situations it is so weak that nobody has ever found any significant application for it. Thorne, Price & McDonald (986) p56 Line integral E = J Riemann ds =ωj r van Putten, Il. Nuov. Cim. 005 cm /cm van Putten - PSR Workshop 008
12 Relativistic capillary effect UHECR Linear accelerator Stable against pair-cascade, nearly charge-free A [ V] r A ~ VH Outflow by relativistic capillary effect Van Putten 008 bounded by Alfven surfaces (``Blandford-Znajek limit ) Approx zero potential drop [ V] θh 0 =VH van Putten - PSR Workshop 008
13 -0 Myr Transiet source during spin-down of SMBH E B M T B B 5 (torus magnetosph ere) E (disk) M AGN = = 9 B M = 5 9 T 7 k G M T M Solar yr,, 5 Van Putten & Gupta (008), submitted Van Putten & Levinson (003) AGN T 7 ~ 0.- (-0 million years), based on 3 FR II Radio Galaxies O Dea C.P. et al. (008) van Putten - PSR Workshop 008 3
14 Energetic output in leptonic jet Gamma-rays by dissipation of kinetic energy in ultra-relativistic baryon poor in internal shocks Shemi & Piran 990, Rees & Meszaros 99,... E E p γ = c = c E LT 90 ( E = ωj, J = eaϕ) ( L= Ω A, Goldreich & Julian 969; Blandford & Znajek 977, Thorne et al.987) F ϕ c c, ω, Ω F ~ Ω H E p T / 90 = eke / γ / ( k = cc ) Ep E c E 0.7 γ 3/ p (Eichler &Juntof (Ghirlanda et al. 004) -Hutter 005) ; k E / 40 γ E / γ E p T / 90 E γ V H 3 0 M 7M H Sun B 6 0 G θh 0.5 ev van Putten - PSR Workshop 008 van Putten et al., PRD (004) 4
15 Correlation to HETE-II and Swift data Pearson coeff: 0.85 Pearson coeff E p T / 90 E γ van Putten - PSR Workshop van Putten, 008
16 Topology of black hole torus formation GRB03039/SN003dh GRB06064 A common inner engine to long GRBs with & without SNe Van Putten Science 999 Van Putten & Ostriker ApJ L 00 van Putten & Levinson ApJ 003 van Putten - PSR Workshop 008 6
17 Bi-modal distribution in durations from slowly and rapidly rotating BHs ΩH < ΩISCO T90 hyper-accretion (accelerated by shedding of angular momentum in magnetic winds) ΩH > ΩISCO T90 viscous timescale of BH spin-down (by horizon Maxwell stresses) van Putten - PSR Workshop Van Putten & Ostriker 00
18 Suspended accretion state by powerful spin-connection BH PSR PSR + - asymptotic infinity PSR Ω + PSR Ω Ω H Ω=0 Spin-up Spin-down Topological equivalence to pulsar magnetospheres when viewed in poloidal cross-section van Putten, Science (999) van Putten & Ostriker ApJL 00 van Putten & Levinson ApJ 003 van Putten & Levinson, Science (00) van Putten - PSR Workshop 008 8
19 Equations of BH spin-down in suspended accretion Position of the ISCO (rel. M ) : z Specific energy and angular momentum at ISCO: e= Ω T Z / = + (-a 3 l = M z 3, + a ) 3 3 ((+ a) Ω 3 + ( a) = 3+ Z ), ((3 Z = (3a ( a= M, z= ; a= 0, z= 6) H tan( λ / ) = M 3 Z Ω η = Ω T H = )(3+ Z + Z ) ; 3z + Z )) ( ) z + a tan( λ/) 3 l = - 3 [ ] + (3z ) : Bardeen et al.97 Van Putten 999 Balance of E Balance of J dm dt dj dt = e = e ( ) ηηω ( η) Ω H H Van Putten, 008 van Putten - PSR Workshop 008 9
20 Model light-curve compared with normalized GRB light curves van Putten - PSR Workshop 008 0
21 Matched Filtering to BATSE light curves of long GRBs van Putten - PSR Workshop 008 Van Putten & Gupta, 008, under review
22 Matched Filtering with Kerr and Block-type template van Putten - PSR Workshop 008
23 Matched Filtering to BATSE light curves of long GRBs van Putten - PSR Workshop Van Putten & Gupta, 008, under review Van Putten, in Orleans School of Mass and Motion in GR (008)
24 Conclusions and Outlook Binary mergers of neutron stars and BHs produce an energetic (``explosive ) events with a bi-modal distribution of durations similar to those of GRBs in the BATSE catalogue from systems with BH angular velocities smaller and larger than that of the ISCO As a ``naked inner engines (would make aspherical radio-loud Ib/c in CC-SNe) are intrinsically radio-loud: energy output in magnetic winds from the accretion disk is about e5 erg for long bursts, and less for short bursts. Binary mergers in low-density host environments Radio emissions from the magnetic winds may be un-absorbed and detectable Outlook Archive searches in radio may reveal long-duration counterparts to the Lorimer at al. 007 event van Putten - PSR Workshop 008 4
High Energy Astrophysics
High Energy Astrophysics Gamma-ray Bursts Giampaolo Pisano Jodrell Bank Centre for Astrophysics - University of Manchester giampaolo.pisano@manchester.ac.uk May 2011 Gamma-ray Bursts - Observations - Long-duration
More informationGRB history. Discovered 1967 Vela satellites. classified! Published 1973! Ruderman 1974 Texas: More theories than bursts!
Discovered 1967 Vela satellites classified! Published 1973! GRB history Ruderman 1974 Texas: More theories than bursts! Burst diversity E peak ~ 300 kev Non-thermal spectrum In some thermal contrib. Short
More informationarxiv: v2 [astro-ph.he] 4 Feb 2010
Multi-messenger emissions from Kerr black holes Maurice H.P.M. van Putten arxiv:0905.3367v2 [astro-ph.he] 4 Feb 2010 Abstract Kerr black holes are energetically similar to spinning tops accompanied by
More informationHypernovae: : GRB-supernovae as LIGO/VIRGO sources of gravitational radiation
Hypernovae: : GRB-supernovae as LIGO/VIRGO sources of gravitational radiation Maurice H.P.M. van Putten (MIT-LIGO) in collaboration with Paris 003 Amir Levinson (Tel Aviv) Stephen Eikenberry (U Florida)
More informationGamma-Ray Astronomy. Astro 129: Chapter 1a
Gamma-Ray Bursts Gamma-Ray Astronomy Gamma rays are photons with energies > 100 kev and are produced by sub-atomic particle interactions. They are absorbed by our atmosphere making observations from satellites
More informationI : Probing the formation and growth of black holes using spin
Astro2010 Science White Paper (submitted to both CFP and GCT) Spin and Relativistic Phenomena Around Black Holes L. Brenneman, J. Miller, P. Nandra, M. Volonteri, M. Cappi, G. Matt, S. Kitamoto, F. Paerels,
More informationAGN in hierarchical galaxy formation models
AGN in hierarchical galaxy formation models Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. Frenk Physics of Galactic Nuclei, Ringberg Castle, June 18, 2009 Outline Brief introduction
More informationObserving GRB afterglows with SIMBOL-X
Observing GRB afterglows with SIMBOL-X Frédéric Daigne (daigne@iap.fr) (Institut d Astrophysique de Paris - Université Paris 6) Gamma-ray bursts : prompt emission Highly variable time profile Non-thermal
More informationChapter 18 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. The Bizarre Stellar Graveyard Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition The Bizarre Stellar Graveyard 18.1 White Dwarfs What is a white dwarf? What can happen to a white dwarf in a close binary system? What supports
More informationSpecial Relativity. Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers.
Black Holes Special Relativity Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers. 2. The speed of light is the same for all inertial observers regardless
More informationChapter 14. Outline. Neutron Stars and Black Holes. Note that the following lectures include. animations and PowerPoint effects such as
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 14 Neutron
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 informationQuasars ASTR 2120 Sarazin. Quintuple Gravitational Lens Quasar
Quasars ASTR 2120 Sarazin Quintuple Gravitational Lens Quasar Quasars Quasar = Quasi-stellar (radio) source Optical: faint, blue, star-like objects Radio: point radio sources, faint blue star-like optical
More informationAccretion Disks. 1. Accretion Efficiency. 2. Eddington Luminosity. 3. Bondi-Hoyle Accretion. 4. Temperature profile and spectrum of accretion disk
Accretion Disks Accretion Disks 1. Accretion Efficiency 2. Eddington Luminosity 3. Bondi-Hoyle Accretion 4. Temperature profile and spectrum of accretion disk 5. Spectra of AGN 5.1 Continuum 5.2 Line Emission
More informationLecture 20 High-Energy Astronomy. HEA intro X-ray astrophysics a very brief run through. Swift & GRBs 6.4 kev Fe line and the Kerr metric
Lecture 20 High-Energy Astronomy HEA intro X-ray astrophysics a very brief run through. Swift & GRBs 6.4 kev Fe line and the Kerr metric Tut 5 remarks Generally much better. However: Beam area. T inst
More informationarxiv: v1 [astro-ph.he] 12 Jan 2009
Non-thermal transient sources from rotating black holes Maurice H.P.M. van Putten Le Studium IAS, 3D Avenue Recherche Scientifique, 45071 Orléans Cedex 2, France arxiv:0901.1674v1 [astro-ph.he] 12 Jan
More informationImplications of GW observations for short GRBs
Implications of GW observations for short GRBs Resmi Lekshmi Indian Institute of Space Science & Technology Trivandrum What are Gamma Ray Bursts? What are short GRBs? Open Questions : Central engine of
More informationThe Discovery of Gamma-Ray Bursts
The Discovery of Gamma-Ray Bursts The serendipitous discovery of Gamma-Ray Bursts (GRBs) in the late sixties puzzled astronomers for several decades: GRBs are pulses of gamma-ray radiation (typically lasting
More information!Basic Properties of Black Holes. !Electrically Charged Black Holes. !Structure of a Simple Black Hole. Agenda for Ast 309N, Dec.
Agenda for Ast 309N, Dec. 4!Basic Properties of Black Holes Repeat of the first-day survey (partic. credit) Thurs: Exam 3 (no make-up available). Office hours, help session on Tues., Wed. afternoons Quiz
More informationNews from the Niels Bohr International Academy
News from the Niels Bohr International Academy What is a gamma-ray burst? The development of our understanding of the phenomenon illustrated by important events (including very recent results on gravitational
More informationGW from GRBs Gravitational Radiation from Gamma-Ray Bursts
GW from GRBs Gravitational Radiation from Gamma-Ray Bursts Tsvi Piran Racah Inst. of Jerusalem, Israel Dafne Guetta,, Ehud Nakar, Reem Sari Once or twice a day we see a burst of low energy gamma-rays from
More informationHigh-Energy Astrophysics Lecture 6: Black holes in galaxies and the fundamentals of accretion. Overview
High-Energy Astrophysics Lecture 6: Black holes in galaxies and the fundamentals of accretion Robert Laing Overview Evidence for black holes in galaxies and techniques for estimating their mass Simple
More informationGamma-ray Astrophysics
Gamma-ray Astrophysics AGN Pulsar SNR GRB Radio Galaxy The very high energy -ray sky NEPPSR 25 Aug. 2004 Many thanks to Rene Ong at UCLA Guy Blaylock U. of Massachusetts Why gamma rays? Extragalactic Background
More informationLearning Objectives: Chapter 13, Part 1: Lower Main Sequence Stars. AST 2010: Chapter 13. AST 2010 Descriptive Astronomy
Chapter 13, Part 1: Lower Main Sequence Stars Define red dwarf, and describe the internal dynamics and later evolution of these low-mass stars. Appreciate the time scale of late-stage stellar evolution
More informationFormation of lamp-post coronae in Seyfert Galaxies and X-ray binaries
NASA/NuSTAR, Wilkins et al 2015 Formation of lamp-post coronae in Seyfert Galaxies and X-ray binaries Yajie Yuan (Spitzer Fellow, Princeton) In collaboration with: Roger Blandford, Dan Wilkins (Stanford)
More informationACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT
Julian H. Krolik ACTIVE GALACTIC NUCLEI: FROM THE CENTRAL BLACK HOLE TO THE GALACTIC ENVIRONMENT PRINCETON UNIVERSITY PRESS Princeton, New Jersey Preface Guide for Readers xv xix 1. What Are Active Galactic
More informationAstronomy. Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes
Astronomy Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes are hot, compact stars whose mass is comparable to the Sun's and size to the Earth's. A. White dwarfs B. Neutron stars
More informationGamma Ray Bursts. Progress & Prospects. Resmi Lekshmi. Indian Institute of Space Science & Technology Trivandrum
Gamma Ray Bursts Progress & Prospects Resmi Lekshmi Indian Institute of Space Science & Technology Trivandrum Why study GRBs? to study GRBs end stages of massive star evolution jet launching, collimation
More informationA zoo of transient sources. (c)2017 van Putten 1
A zoo of transient sources (c)2017 van Putten 1 First transient @ first light UDFj-39546284, z~10.3 Bouwens, R.J., et al., Nature, 469, 504 Cuchiara, A. et al., 2011, ApJ, 736, 7 z=9.4: GRB 090429B, z~9.4
More informationShort GRB and kilonova: did observations meet our theoretical predictions?
Short GRB and kilonova: did observations meet our theoretical predictions? Riccardo Ciolfi INAF - Astronomical Observatory of Padova INFN - Trento Institute for Fundamental Physics and Applications GW170817
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 informationGravitational Wave Astronomy using 0.1Hz space laser interferometer. Takashi Nakamura GWDAW-8 Milwaukee 2003/12/17 1
Gravitational Wave Astronomy using 0.1Hz space laser interferometer Takashi Nakamura GWDAW-8 Milwaukee 2003/12/17 1 In 2001 we considered what we can do using 0.1 hertz laser interferometer ( Seto, Kawamura
More informationSPECIAL RELATIVITY! (Einstein 1905)!
SPECIAL RELATIVITY! (Einstein 1905)! Motivations:! Explaining the results of the Michelson-Morley! experiment without invoking a force exerted! on bodies moving through the aether.! Make the equations
More informationStellar Binary Systems and CTA. Guillaume Dubus Laboratoire d Astrophysique de Grenoble
Stellar Binary Systems and CTA Guillaume Dubus Laboratoire d Astrophysique de Grenoble Barcelona Cherenkov Telescope Array Meeting, 24-25 January 2008 X-ray binaries picture by H. Spruit relativistic outflow
More informationCosmological Fast Radio Bursts from Binary White Dwarf Mergers
Cosmological Fast Radio Bursts from Binary White Dwarf Mergers Kunihito Ioka (KEK) Kashiyama, KI & Mészáros 13 ~10 yr ago GRB Cosmology Massive star origin High redshift GRBs Like QSO Like SN Star formation
More informationBlack Holes and Active Galactic Nuclei
Black Holes and Active Galactic Nuclei A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping. The theory of general relativity predicts that a sufficiently
More informationProbing Extreme Physics with Compact Objects
Probing Extreme Physics with Compact Objects Dong Lai Department of Astronomy Cornell University Extremes in Astrophysics: Most energetic particles: 10 20 ev Most energetic photons: 10 14 ev Highest temperature:
More informationElectromagnetic counterparts to binary neutron star mergers. Koutarou Kyutoku (KEK) Collaborators: Kunihito Ioka (KEK), Masaru Shibata (YITP)
Electromagnetic counterparts to binary neutron star mergers Koutarou Kyutoku (KEK) Collaborators: Kunihito Ioka (KEK), Masaru Shibata (YITP) Summary Electromagnetic counterparts to gravitational waves
More informationActive Galactic Nuclei
Active Galactic Nuclei Prof. Jeff Kenney Class 18 June 20, 2018 the first quasar discovered 3C273 (1963) very bright point source (the quasar ) jet the first quasar discovered 3C273 (1963) very bright
More informationTesting the nature of astrophysical black hole candidates. Cosimo Bambi (Fudan University, Shanghai)
Testing the nature of astrophysical black hole candidates Cosimo Bambi (Fudan University, Shanghai) 8 June 2013, Annual Meeting of the Physics Department Fudan University, Shanghai Tests of General Relativity
More informationInterpretation of Early Bursts
Gamma-Ray Bursts Discovery The early years BATSE Fast versus slow bursts Uniformity and log N log S relation BeppoSAX and discovery of afterglows Redshift measurements Connection of long GRBs to supernovae
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 informationNeutron Stars. Properties of Neutron Stars. Formation of Neutron Stars. Chapter 14. Neutron Stars and Black Holes. Topics for Today s Class
Foundations of Astronomy 13e Seeds Phys1403 Introductory Astronomy Instructor: Dr. Goderya Chapter 14 Neutron Stars and Black Holes Cengage Learning 2016 Topics for Today s Class Neutron Stars What is
More informationSpins of Supermassive Black Holes. Ruth A. Daly
Spins of Supermassive Black Holes Ruth A. Daly Three key quantities characterize a black hole: mass, spin, and charge. Astrophysical black holes are thought to have zero net charge, and thus are characterized
More informationStrong gravity and relativistic accretion disks around supermassive black holes
Strong gravity and relativistic accretion disks around supermassive black holes Predrag Jovanović Astronomical Observatory, Volgina 7, 11060 Belgrade 38, SERBIA Abstract Here we used numerical simulations
More informationThomas Tauris MPIfR / AIfA Uni. Bonn
Thomas Tauris MPIfR / AIfA Uni. Bonn 1: Introduction Degenerate Fermi Gases Non-relativistic and extreme relativistic electron / (n,p,e - ) gases : White Dwarfs Structure, cooling models, observations
More informationRotating RAdio Transients (RRATs) ApJ, 2006, 646, L139 Nature, 2006, 439, 817 Astro-ph/
Rotating RAdio Transients (RRATs) ApJ, 2006, 646, L139 Nature, 2006, 439, 817 Astro-ph/0608311 Introduction 11 Rotating RAdio Transients (RRATs) (Mclaughlin et al 2006) Repeated, irregular radio bursts
More informationDistribution of X-ray binary stars in the Galaxy (RXTE) High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars
High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars Distribution of X-ray binary stars in the Galaxy (RXTE) Robert Laing Primary Compact accreting binary systems Compact star WD NS BH
More informationGamma-ray Bursts. Chapter 4
Chapter 4 Gamma-ray Bursts At the moment, the most important application of the theory of relativistic shock waves is in explaining the radiation from Gamma-ray Burst sources. I will briefly introduce
More informationTesting the nature of astrophysical black hole candidates. Cosimo Bambi Fudan University
Testing the nature of astrophysical black hole candidates Cosimo Bambi Fudan University http://www.physics.fudan.edu.cn/tps/people/bambi/ 26 September 2013, National Astronomical Observatories, Beijing
More informationNeutron Stars. Neutron Stars and Black Holes. The Crab Pulsar. Discovery of Pulsars. The Crab Pulsar. Light curves of the Crab Pulsar.
Chapter 11: Neutron Stars and Black Holes A supernova explosion of an M > 8 M sun star blows away its outer layers. Neutron Stars The central core will collapse into a compact object of ~ a few M sun.
More informationCosmic Explosions. Greg Taylor (UNM ) Astro 421
Cosmic Explosions Greg Taylor (UNM ) Astro 421 1 Cassiopeia A: Supernova Remnant E total ~ 10 46 J 2 An early gamma ray-burst Vela satellite 3 A Gamma Ray Burst Sampler 4 Burst Alert 5 The BeppoSAX Satellite
More informationEvolution of High Mass stars
Evolution of High Mass stars Neutron Stars A supernova explosion of a M > 8 M Sun star blows away its outer layers. The central core will collapse into a compact object of ~ a few M Sun. Pressure becomes
More informationLobster X-ray Telescope Science. Julian Osborne
Lobster X-ray Telescope Science Julian Osborne What we want The whole high-energy sky right now 1.00E+13 1.00E+12 1 / f_lim (100 s) 1.00E+11 1.00E+10 1.00E+09 1.00E+08 0.0000001 0.000001 0.00001 0.0001
More informationChapter 17. Active Galaxies and Supermassive Black Holes
Chapter 17 Active Galaxies and Supermassive Black Holes Guidepost In the last few chapters, you have explored our own and other galaxies, and you are ready to stretch your scientific imagination and study
More informationMeasuring Black Hole Spin in AGN. Laura Brenneman (Harvard-Smithsonian CfA)
Measuring Black Hole Spin in AGN Laura Brenneman (Harvard-Smithsonian CfA) Single and Double Special Massive thanks Black to: Holes in Galaxies Chris Reynolds, University Andy Fabian, of Michigan Martin
More informationRELATIVISTIC SPECTROSCOPY OF BLACK HOLES
RELATIVISTIC SPECTROSCOPY OF BLACK HOLES Michael Parker ESAC science seminar 24/5/18 BLACK HOLES 101 For an object to just escape a massive body, it needs the sum: Kinetic energy + gravitational binding
More informationTesting astrophysical black holes. Cosimo Bambi Fudan University
Testing astrophysical black holes Cosimo Bambi Fudan University http://www.physics.fudan.edu.cn/tps/people/bambi/ 29 October 2015 Interdisciplinary Center for Theoretical Studies (USTC, Hefei) Plan of
More informationStellar Evolution: Outline
Stellar Evolution: Outline Interstellar Medium (dust) Hydrogen and Helium Small amounts of Carbon Dioxide (makes it easier to detect) Massive amounts of material between 100,000 and 10,000,000 solar masses
More informationLecture 19. Gamma-Ray Bursts
Lecture 19 Gamma-Ray Bursts First Gamma-Ray Burst The Vela 5 satellites functioned from July, 1969 to April, 1979 and detected a total of 73 gamma-ray bursts in the energy range 150 750 kev (n.b,. Greater
More informationNew Suzaku Results on Active Galaxies. or Reflections on AGN. James Reeves (Keele) and Suzaku team (given by Lance Miller)
New Suzaku Results on Active Galaxies or Reflections on AGN James Reeves (Keele) and Suzaku team (given by Lance Miller) Overview Overview of Suzaku and instrument performance. Why Suzaku is important
More informationHow do disks transfer angular momentum to deliver gas onto compact objects? How do accretion disks launch winds and jets?
Astro2010 Science White Paper (GCT) Fundamental Accretion and Ejection Astrophysics J. Miller, M. Nowak, P. Nandra, N. Brandt, G. Matt, M. Cappi, G. Risaliti, S. Kitamoto, F. Paerels. M. Watson, R. Smith,
More informationThis is a vast field - here are some references for further reading
This is a vast field - here are some references for further reading Dippers: Smale et al. 1988 MNRAS 232 647 Black hole transient lmxbs: Remillard and McClintock, 2006 ARAA 44, 49 Color-color diagrams
More informationOverview of Stellar Evolution
Overview of Stellar Evolution Walter Baade 1893-1960 With Fritz Zwicky first proposed that neutron stars could be formed by supernovae in 1934 Iron core collapse E+p->n+ Degenerate neutrons limit size
More informationThe Gravitational Radiation Rocket Effect. Marc Favata Cornell University GR17, Dublin, July 2004
The Gravitational Radiation Rocket Effect recoil Marc Favata Cornell University GR17, Dublin, July 004 Favata, Hughes, & Holz, ApJL 607, L5, astro-ph/040056 Merritt, Milosavljevic, Favata, Hughes, & Holz,
More informationTheoretical aspects of microquasars
Theoretical aspects of microquasars Bingxiao Xu Department of Physics & Astronomy, GSU ABSTRACT: Microquasars (black hole X-ray binaries with relativistic jets) are first found by means of multiwavelengths
More informationfrom Fermi (Higher Energy Astrophysics)
Particle Acceleration Results from Fermi (Higher Energy Astrophysics) Roger Blandford KIPAC Stanford 3 viii 2011 SLAC SSI 1 Fermi Joint NASA-DOE-Italy- France-Japan- Sweden, Germany mission Launch June
More informationTransient Events from Neutron Star Mergers
Transient Events from Neutron Star Mergers Li-Xin Li Kavli Institute for Astronomy and Astrophysics Peking University, Beijing Transient Astronomical Events Transient astronomical events include all astronomical
More informationCompact Binaries - 3 ASTR2110 Sarazin
Compact Binaries - 3 ASTR2110 Sarazin Zoology of Binary Stars X-ray Binary Pulsar Spin-Up Accreted material has high angular momentum Spins up neutron star (true of ~all X-ray binary pulsars) Millisecond
More informationActive galactic nuclei (AGN)
Active galactic nuclei (AGN) General characteristics and types Supermassive blackholes (SMBHs) Accretion disks around SMBHs X-ray emission processes Jets and their interaction with ambient medium Radio
More informationSPIN PRECESSION IN A 2 BODY SYSTEM: A NEW TEST OF GENERAL RELATIVITY R. F. O CONNELL DEPT. OF PHYSICS & ASTRONOMY LOUISIANA STATE UNIVERSITY
SPIN PRECESSION IN A 2 BODY SYSTEM: A NEW TEST OF GENERAL RELATIVITY R. F. O CONNELL DEPT. OF PHYSICS & ASTRONOMY LOUISIANA STATE UNIVERSITY 1 1. Newtonian Theory (p. 2) 2. General Relativistic Corrections
More informationAge-redshift relation. The time since the big bang depends on the cosmological parameters.
Age-redshift relation The time since the big bang depends on the cosmological parameters. Lyman Break Galaxies High redshift galaxies are red or absent in blue filters because of attenuation from the neutral
More informationX-ray Binaries. Image credit: Robert Hynes (2002)
Ramesh Narayan X-ray Binaries Image credit: Robert Hynes (2002) Galactic Nuclei Image credit: Lincoln Greenhill, Jim Moran Outline Measuring BH mass Estimating BH spin Testing Relativity Evidence for the
More informationEvidence for BH: Active Galaxies
Evidence for BH: Active Galaxies This is the first of two lectures in which we ll talk about evidence for the existence of black holes in the universe. It is actually in the next lecture, where we ll talk
More informationChapter 18 The Bizarre Stellar Graveyard
Chapter 18 The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White
More informationOutflows & Jets: Theory & Observations
Outflows & Jets: Theory & Observations Lecture winter term 008/009 Henrik Beuther & Christian Fendt 10.10 17.10 4.10 31.10 07.11 14.11 1.11 8.11 05.1 1.1 19.1 6.1 09.01 16.01 3.01 30.01 Introduction &
More informationFORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS
FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS Main Categories of Compact Systems Formation of Compact Objects Mass and Angular Momentum Loss Evolutionary Links to Classes of Binary Systems Future Work
More informationBlack Holes ASTR 2110 Sarazin. Calculation of Curved Spacetime near Merging Black Holes
Black Holes ASTR 2110 Sarazin Calculation of Curved Spacetime near Merging Black Holes Test #2 Monday, November 13, 11-11:50 am Ruffner G006 (classroom) Bring pencils, paper, calculator You may not consult
More informationGamma-Ray Bursts: The Central Engine
Gamma-Ray Bursts: The Central Engine S. E. Woosley Astronomy Department, UCSC 1 Abstract. A variety of arguments suggest that the most common form of gamma-ray bursts (GRBs), those longer than a few seconds,
More informationThe Supernova/Gamma-Ray Burst Connection. Jens Hjorth Dark Cosmology Centre Niels Bohr Institute University of Copenhagen
The Supernova/Gamma-Ray Burst Connection Jens Hjorth Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Galama et al. 1998; Fynbo et al. 2000 SN 1998bw/GRB 980425 Galama et al. 1998 Collapsar
More informationBroadband X-ray emission from radio-quiet Active Galactic Nuclei
29 th ASI Meeting ASI Conference Series, 2011, Vol. 3, pp 19 23 Edited by Pushpa Khare & C. H. Ishwara-Chandra Broadband X-ray emission from radio-quiet Active Galactic Nuclei G. C. Dewangan Inter-University
More informationFinal States of a Star
Pulsars Final States of a Star 1. White Dwarf If initial star mass < 8 MSun or so. (and remember: Maximum WD mass is 1.4 MSun, radius is about that of the Earth) 2. Neutron Star If initial mass > 8 MSun
More informationGuiding Questions. Active Galaxies. Quasars look like stars but have huge redshifts
Guiding Questions Active Galaxies 1. Why are quasars unusual? How did astronomers discover that they are extraordinarily distant and luminous? 2. What evidence showed a link between quasars and galaxies?
More informationEric Howell University of Western Australia
Using temporal distributions of transient events to characterize cosmological source populations AIGO Conference 22-24 February 2010 Eric Howell University of Western Australia Plan Brief overview cosmological
More informationIron line profiles including emission from within the innermost stable orbit of a black hole accretion disc
Mon. Not. R. Astron. Soc. 000, 000 000 (1998) Iron line profiles including emission from within the innermost stable orbit of a black hole accretion disc A.J. Young 1, R.R. Ross 1,2 and A.C. Fabian 1 1
More informationChapter 14: The Bizarre Stellar Graveyard
Lecture Outline Chapter 14: The Bizarre Stellar Graveyard 14.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf?
More informationSources of GeV Photons and the Fermi Results
Sources of GeV Photons and the Fermi Results 1. GeV instrumentation and the GeV sky with the Fermi Gamma-ray Space Telescope 2. First Fermi Catalog of Gamma Ray Sources and the Fermi Pulsar Catalog 3.
More informationCOSMIC RAYS DAY INTRODUCTION TO COSMIC RAYS WINDWARD COMMUNITY COLLEGE - SEPTEMBER 26, 2015 VERONICA BINDI - UNIVERSITY OH HAWAII
COSMIC RAYS DAY WINDWARD COMMUNITY COLLEGE - SEPTEMBER 26, 2015 VERONICA BINDI - UNIVERSITY OH HAWAII INTRODUCTION TO COSMIC RAYS MAJOR QUESTIONS: Are there forms of matter in the Universe that do not
More informationGAMMA-RAY BURSTS. mentor: prof.dr. Andrej Čadež
GAMMA-RAY BURSTS author: Uroš Kostić mentor: prof.dr. Andrej Čadež Abstract Gamma-ray bursts (GRB) are sudden, intense flashes of gamma rays which, for a few seconds, light up in otherwise dark gamma-ray
More informationGRAVITATIONAL COLLAPSE
GRAVITATIONAL COLLAPSE Landau and Chandrasekhar first realised the importance of General Relativity for Stars (1930). If we increase their mass and/or density, the effects of gravitation become increasingly
More informationGravitational Radiation from Gamma-Ray Bursts Tsvi Piran Λ The Racah Institute of Physics, Hebrew University, Jerusalem, Israel Lecture given at the C
Gravitational Radiation from Gamma-Ray Bursts Tsvi Piran Λ The Racah Institute of Physics, Hebrew University, Jerusalem, Israel Lecture given at the Conference on Gravitational Waves: A Challenge to Theoretical
More informationAGN Feedback In an Isolated Elliptical Galaxy
AGN Feedback In an Isolated Elliptical Galaxy Feng Yuan Shanghai Astronomical Observatory, CAS Collaborators: Zhaoming Gan (SHAO) Jerry Ostriker (Princeton) Luca Ciotti (Bologna) Greg Novak (Paris) 2014.9.10;
More informationHigh-Energy Plasma Astrophysics and Next Generation Gamma-Ray Observatory Cherenkov Telescope Array
High-Energy Plasma Astrophysics and Next Generation Gamma-Ray Observatory Cherenkov Telescope Array FAPESP CUNY Week, New York, November 2018 M82 Star Formation- Clouds-SNRturbulence connection Sun & Stars
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 informationRosalba Perna. (University of
Rosalba Perna (University of Colorado@Boulder) Swift observations opened a new window Pre-Swift Pre-Swift Pre-Swift belief belief belief [figure courtesy of R. Mockovitch]. of surprises.with PLATEAUS &
More informationMass ejection from neutron-star mergers in numerical relativity
Mass ejection from neutron-star mergers in numerical relativity Masaru Shibata Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University I. Brief introduction Outline
More informationThe X-Ray Universe. The X-Ray Universe
The X-Ray Universe The X-Ray Universe Potsdam University Dr. Lidia Oskinova Sommersemester 2017 lida@astro.physik.uni-potsdam.de astro.physik.uni-potsdam.de ~lida/vorlesungxrayso17.html Chandra X-ray,
More informationEvidence for BH: Active Galaxies
Evidence for BH: Active Galaxies This is the second lecture in which we ll talk about evidence for the existence of black holes in the universe. Here we focus on active galactic nuclei, or AGN. Black holes
More informationProspects in space-based Gamma-Ray Astronomy
Prospects in space-based Gamma-Ray Astronomy On behalf of the European Gamma-Ray community Jürgen Knödlseder Centre d Etude Spatiale des Rayonnements, Toulouse, France Gamma-Ray Astronomy in Europe Europe
More informationMHD simulation for merger of binary neutron stars in numerical relativity
MHD simulation for merger of binary neutron stars in numerical relativity M. SHIBATA (Yukawa Institute for Theoretical Physics, Kyoto University) In collaboration with K. Kiuchi, L. Baiotti, & Y. Sekiguchi
More information