Extreme gravity in neutron-star systems with XEUS
|
|
- Benedict Owens
- 5 years ago
- Views:
Transcription
1 Extreme gravity in neutron-star systems with XEUS Mariano Méndez Kapteyn Astronomical Institute, University of Groningen, The Netherlands
2 Probing strong gravitational fields Adapted from Kramer et al. (2004) & Psaltis (2004)
3 NS and strong gravitational fields 1. Kilohertz Quasi-Periodic Oscillations (khz QPOs) as basic General Relativistic (GR) frequencies. 2. khz QPOs and the Innermost Stable Circular Orbit (ISCO). 3. Surface (absorption) lines. 4. Emission lines from the inner accretion disc.
4 Strong gravitational field: khz QPOs width ν 1 ν 2 amplitude Central freq. van der Klis (1997)
5 1. The 3 basic GR frequencies ν z : vertical ν θ : azimuthal ν θ κ: Periastron precession κ: radial ν z ν θ : Lense-Thirring
6 2. The ISCO As the inner edge of the disc moves inwards, driven by mass accretion rate, the azimuthal frequency at that radial position in the disc increases. Maximum orbital frequency is the Keplerian frequency at the ISCO.
7 2. The ISCO Oct March Sept Feb 1997 Quality factor = frequency / width 1000 Freq (Hz) U Intensity (c/s) Frequency (Hz) 4U Zhang et al. (1998); Barret et al. (2006)
8 2. The ISCO Quality factor = frequency / width Frequency (Hz) 4U U Barret et al. (2006)
9 khz QPOs: Complications 1. No unique identification of QPOs with the basic GR (or other) frequencies Possible solution: Simultaneous timing and spectroscopy (see below). 2. Identification of the ISCO requires that: From pair of QPOs, the one at higher frequencies is the Keplerian (vertical) GR frequency (most, but not all, models propose this), and Keplerian (vertical) frequency is the highest frequency in the disc. True for test particles; super- Keplerian frequencies may appear in real discs.
10 khz QPOs: Complications 3. ISCO complications: High amplitude above ~10 15 kev Modulated flux not from the disc, but due to inverse Compton. Oscillator Modulator Accretion disc No clean test-particle dynamics. Frequency ceiling and drop of Quality factor due (in part) to changes in the modulator?
11 3. Surface (absorption) lines Scalar-Tensor extensions to Einstein s theory Extra scalar field described in terms of the parameter β. From binary-pulsar timing β 8. Dedeo & Psaltis (2003)
12 Gravitational redshift
13 khz QPOs: Complications (revisited) 1. No unique identification of QPOs with the basic GR (or other) frequencies Possible solution using spectroscopy Surface spectral lines may help resolve this. Lines are broadened by: longitudinal and transverse Doppler shifts, special relativistic beaming, gravitational redshifts, light-bending, frame-dragging (Lense- Thirring). Bhattacharyya et al. (2006)
14 4. Emission lines from the inner disc Suzaku XMM-Newton Serpens X-1 Serpens X-1 Cackett et al. (2008); Bhattacharyya & Strohmayer (2007)
15 Emission lines: Complications 4U XMM-Newton/Epic-PN σ Counts cm -2 s -1 kev Energy (kev) Energy (kev) Left: Right: Continuum emission + Line from 6 r g (Continuum emission + Line from 12 r g ) photo-ionized absorption
16 Instrument requirements: Timing 1. Kilohertz Quasi-Periodic Oscillations (khz QPOs) as basic General Relativistic (GR) frequencies. 2. khz QPOs and the Innermost Stable Circular Orbit (ISCO). HTRS: Band pass: 1 25keV Amplitude increases with energy Effective area: At least 4 RXTE (/4 m 2 ) Spectral resol.: ~20% Energy-dependent time lags Max. count rate: 10 6 c/s Bright sources Time resol.: τ.10 μs
17 Instrument requirements: Spectroscopy 3. Surface (absorption) lines. 4. Emission lines from the inner accretion disc. WFI + NFI: Band pass: kev Redshifted Oxygen; continuum around Fe K Effective area: /5 m 2 Absorption lines in individual X-ray bursts (~10 s) Spectral resol.: 2 3 ev at 1 kev Resolve line profile (eg. L-T) Max. count rate: 10 5 counts/s during 1 5 s X-ray bursts; Defocusing?
Probing Neutron Star Physics using Thermonuclear X-ray Bursts
Probing Neutron Star Physics using Thermonuclear X-ray Bursts Sudip Bhattacharyya University of Maryland (CRESST) NASA s Goddard Space Flight Center Outline Neutron Stars: why do we care? Thermonuclear
More informationThe geometric origin of quasi-periodic oscillations in black hole binaries
X-ray Universe 2014 Dublin - 17 th June The geometric origin of quasi-periodic 6000 oscillations in black hole binaries GRS1915+105 Adam Ingram Michiel van der Klis, Chris Done Time (s) 15 5 10 20 Black
More informationFocussing on X-ray binaries and microquasars
Focussing on X-ray binaries and microquasars Didier BARRET Centre d Etude Spatiale des Rayonnements Toulouse, France Thank you Peter and Dolorès and the organizing committee I will start with the conclusions
More informationProbing general relativistic precession with tomography and polarimetry
Probing general relativistic precession with tomography and polarimetry Adam Ingram Michiel van der Klis, Matt Middleton, Chris Done, Diego Altamirano, Phil Uttley, Magnus Axelsson, Tom Maccarone, Juri
More informationCitation for published version (APA): Wang, Y. (2018). Disc reflection in low-mass X-ray binaries. [Groningen]: Rijksuniversiteit Groningen.
University of Groningen Disc reflection in low-mass X-ray binaries Wang, Yanan IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check
More informationProbing Relativistic Gravity with the Double Pulsar
Probing Relativistic Gravity with the Double Pulsar Marta Burgay INAF Osservatorio Astronomico di Cagliari The spin period of the original millisecond pulsar PSR B1937+21: P = 0.0015578064924327 ± 0.0000000000000004
More informationEvidence of a decrease of khz quasi-periodic oscillation peak separation towards low frequencies in 4U (GX 354 0)
Mon. Not. R. Astron. Soc. 345, 35 39 (2003) Evidence of a decrease of khz quasi-periodic oscillation peak separation towards low frequencies in 4U 1728 34 (GX 354 0) S. Migliari, M. van der Klis and R.
More informationTime lags of the kilohertz quasi-periodic oscillations in the low-mass X-ray binaries 4U and 4U
Universidade de São Paulo Biblioteca Digital da Produção Intelectual - BDPI Departamento de Astronomia - IAG/AGA Artigos e Materiais de Revistas Científicas - IAG/AGA 2013 Time lags of the kilohertz quasi-periodic
More informationConstraints on the Equation of State of Neutron Star Matter From Observations of Kilohertz QPOs
1 Constraints on the Equation of State of Neutron Star Matter From Observations of Kilohertz QPOs M. Coleman Miller a Frederick K. Lamb b and Dimitrios Psaltis c a University of Chicago, Department of
More informationGravity in the strong field regime & Matter at supra-nuclear density
Gravity in the strong field regime & Matter at supra-nuclear density Science topics for a large area X-ray Telescop" Didier Barret On behalf of M. Abramowicz, J.L. Atteia, D. Barret, T. Belloni, G. Bignami,
More informationJanuary 20, Doctoral Thesis Defense. Jeremy Schnittman. Radiation Transport Around Kerr Black Holes
Radiation Transport Around Kerr Black Holes Jeremy Schnittman Doctoral Thesis Defense January 20, 2005 Massachusetts Institute of Technology Outline Background/Motivation Ray Tracing Hot Spot Model Peak
More informationMeasuring MNS, RNS, MNS/RNS or R
Measuring MNS, RNS, MNS/RNS or R Sebastien Guillot Advisor: Robert Rutledge Galileo Galilei Institute, Firenze March 2014 Some Reviews Lattimer and Prakash, 2007 Miller C., 2013 Heinke et al., 2013 Reminder
More informationSpectra and variability properties of accretion flows: testing QPO models with Athena
Spectra and variability properties of accretion flows: testing QPO models with Athena Chris Done Adam Ingram Chris Fragile Mari Kolehmainen, Aya Kubota Transients Huge amounts of data, long term variability
More informationarxiv:astro-ph/ v1 17 Dec 2003
Interpreting QPOs from Accreting Neutron Stars M. Coleman Miller University of Maryland at College Park arxiv:astro-ph/0312449 v1 17 Dec 2003 Abstract. The high time resolution and large area of the Rossi
More informationPoS(INTEGRAL 2012)049
Testing reflection features in 4U 175 44 with XMM-Newton, BeppoSAX, and RXTE in the hard and soft states Università di Cagliari - Italy E-mail: emailelise.egron@dsf.unica.it Tiziana Di Salvo Università
More informationModels of Kilohertz Quasi-Periodic Brightness Oscillations
Models of Kilohertz Quasi-Periodic Brightness Oscillations M. Coleman Miller University of Chicago, Dept. of Astronomy and Astrophysics 5640 S. Ellis Ave., Chicago, IL 60637 Abstract. The remarkable discovery
More informationSOFT X-RAY LAGS AND THE CORRELATION WITH BH MASS IN RADIO QUIET AGN
SOFT X-RAY LAGS AND THE CORRELATION WITH BH MASS IN RADIO QUIET AGN flux time Barbara De Marco (Centro de Astrobiología, CSIC-INTA) Collaborators: G. Ponti, P. Uttley, M. Cappi, G. Miniutti, M. Dadina,
More informationMeasuring the Spin of the Accreting Black Hole In Cygnus X-1
Measuring the Masses and Spins of Stellar Black Holes Measuring the Spin of the Accreting Black Hole In Cygnus X-1 Lijun Gou Harvard-Smithsonian Center for Astrophysics Collaborators: Jeffrey McClintock,
More informationkhz quasi-periodic oscillations in the low-mass X-ray binary 4U
Mon. Not. R. Astron. Soc. 399, 1901 1906 (2009) doi:10.1111/j.1365-2966.2009.15430.x khz quasi-periodic oscillations in the low-mass X-ray binary 4U 0614+09 Martin Boutelier, 1,2 Didier Barret 1,2 and
More informationThe time derivative of the kilohertz quasi-periodic oscillations in 4U Sanna, Andrea; Mendez, Mariano; Belloni, Tomaso; Altamirano, Diego
University of Groningen The time derivative of the kilohertz quasi-periodic oscillations in 4U 1636-53 Sanna, Andrea; Mendez, Mariano; Belloni, Tomaso; Altamirano, Diego Published in: Monthly Notices of
More informationX-ray spectroscopy of low-mass X-ray binaries
X-ray spectroscopy of low-mass X-ray binaries Laurence Boirin Observatoire astronomique de Strasbourg (Handout version) Artistic impression of a low-mass X-ray binary An X-ray binary spectrum (from the
More information3.1.1 Lightcurve, colour-colour and hardness intensity diagram
Chapter 3 X ray data analysis methods 3.1 Data Analysis Procedure The analysis and reduction procedure of astronomical data can be broadly classified into two categories - (1) count rate variations as
More informationNeutron star mass and radius constraints from millisecond X-ray pulsars and X-ray bursters
Neutron star mass and radius constraints from millisecond X-ray pulsars and X-ray bursters Juri Poutanen (University of Turku, Finland) Collaborators:! Valery Suleimanov (Univ. Tübingen, Germany), Joonas
More informationFrontiers: Observational Signatures of Strong Gravity
Frontiers: Observational Signatures of Strong Gravity As we said a few lectures ago, general relativity is in a unique position among theories of fundamental interactions, because of the relative weakness
More informationSpacecraft clocks and General Relativity
Raymond Angélil Prasenjit Saha May 22, 2013 Clocks in space - nothing new universe s expansion history stellar composition binary neutron star orbit determination galaxy rotation curves exoplanet discovery
More informationThe correlations between the twin khz quasi-periodic oscillation frequencies of low-mass X-ray binaries
Mon. Not. R. Astron. Soc. 366, 1373 1377 (2006) doi:10.1111/j.1365-2966.2006.09920.x The correlations between the twin khz quasi-periodic oscillation frequencies of low-mass X-ray binaries C. M. Zhang,
More informationAtomic Structure & Radiative Transitions
Atomic Structure & Radiative Transitions electron kinetic energy nucleus-electron interaction electron-electron interaction Remember the meaning of spherical harmonics Y l, m (θ, ϕ) n specifies the
More informationObservational appearance of strong gravity in X-rays
Observational appearance of strong gravity in X-rays Compact object Companion star (5000 K) Schwarzschild radius Schwarzschild metric R s 2GM Schwarzschild radius (= 2.95 km for 1М ) c 2 Accretion Black
More informationSpectral Lines from Rotating Neutron Stars
Submitted to The Astrophysical Journal Letters Spectral Lines from Rotating Neutron Stars Feryal Özel1 and Dimitrios Psaltis Institute for Advanced Study, School of Natural Sciences, Einstein Dr., Princeton,
More informationGIORGIO MATT (DIP. FISICA, UNIVERSITÀ ROMA TRE, ITALY)
PROBING STRONG GRAVITY AROUND BLACK HOLES (WITH E.M. RADIATION) GIORGIO MATT (DIP. FISICA, UNIVERSITÀ ROMA TRE, ITALY) Plan of the talk Black holes : general properties Strong gravity effects on e.m. radiation
More informationv Characteristics v Possible Interpretations L X = erg s -1
Ultra Luminous X-ray sources v Characteristics L X = 39-41 erg s -1 >> M black hole(bh) L Edd = 39 erg s -1. Usually seen in star forming regions. On arms of spiral galaxies (right). In starburst or irregular
More informationPost-Keplerian effects in binary systems
Post-Keplerian effects in binary systems Laboratoire Univers et Théories Observatoire de Paris / CNRS The problem of binary pulsar timing (Credit: N. Wex) Some classical tests of General Relativity Gravitational
More informationMILLISECOND PULSARS. Merve Çolak
MILLISECOND PULSARS Merve Çolak OUTLINE Corbet Diagram (again) P-P(dot) Diagram MSPs and Their History Properties of MSPs Spin-up of Neutron Stars Spin-down of MSPs MSP Evolution Recent MSP Evolution Model
More informationAn abrupt drop in the coherence of the lower khz quasi-periodic oscillations in 4U
Mon. Not. R. Astron. Soc. 361, 855 860 (2005) doi:10.1111/j.1365-2966.2005.09214.x An abrupt drop in the coherence of the lower khz quasi-periodic oscillations in 4U 1636 536 Didier Barret, 1 Jean-Francois
More informationX-ray Timing of Stellar Mass Black Holes
X-ray Timing of Stellar Mass Black Holes a white paper for the 2010 Decadal Review by: John A. Tomsick UC Berkeley/Space Sciences Laboratory Ronald A. Remillard and Jeroen Homan MIT/Kavli Institute for
More informationSonic-Point and Spin-Resonance Model of the Kilohertz QPO Pairs
Submitted to ApJ(Letters). Sonic-Point and Spin-Resonance Model of the Kilohertz QPO Pairs Frederick K. Lamb 1 Center for Theoretical Astrophysics, University of Illinois at Urbana-Champaign, 1110 W. Green
More informationarxiv: v1 [astro-ph.he] 5 Jan 2015
Draft Version December 8, 0. Preprint typeset using L A TEX style emulateapj v. // PULSE AMPLITUDE DEPENDS ON KHZ QPO FREQUENCY IN THE ACCRETING MILLISECOND PULSAR SAX J808. 8 Peter Bult and Michiel van
More informationMAPPING THE INNERMOST REGIONS OF AGNS WITH SHORT TIMESCALE FE LINE VARIABILITY
1 MAPPING THE INNERMOST REGIONS OF AGNS WITH SHORT TIMESCALE FE LINE VARIABILITY Giovanni Miniutti, Kazushi Iwasawa, and Andrew C. Fabian Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK ABSTRACT
More informationGetting to Grips with X-ray Reverberation and Lag Spectra. Dan Wilkins with Ed Cackett, Erin Kara, Andy Fabian
Getting to Grips with X-ray Reverberation and Lag Spectra Dan Wilkins with Ed Cackett, Erin Kara, Andy Fabian X-ray BunClub May 212 Outline 1. Observing X-ray reverberation and lag spectra 2. Simulating
More informationResolving the Space-Time Around Black Holes
Resolving the Space-Time Around Black Holes Kendrah Murphy & Tahir Yaqoob Johns Hopkins University Image from Dovciak et al. (2004) Introduction Black holes are defined by their mass, charge, and angular
More informationNuSTAR + XMM Observations of NGC 1365: A Constant Inner Disc
NuSTAR + XMM Observations of NGC 1365: A Constant Inner Disc Dom Walton Caltech G. Risaliti, F. Harrison, E. Kara, M. Parker, E. Rivers, on behalf of the NuSTAR active galaxy working groups Black Hole
More informationX-ray Emission from Compact Objects
X-ray Emission from Compact Objects Lynn Cominsky XXVI SLAC Summer Institute on Particle Physics August 4, 1998 Lecture 2 8/4/98 L. Cominsky/SSI 1 Introduction How X-ray data are used to determine fundamental
More informationBLACK HOLES (AND NEUTRON STARS) IN X-RAY BINARIES: Evolution and Accretion states TEO MUÑOZ DARIAS MARIE CURIE FELLOW. Oxford Astrophysics
BLACK HOLES (AND NEUTRON STARS) IN X-RAY BINARIES: Evolution and Accretion states TEO MUÑOZ DARIAS MARIE CURIE FELLOW Oxford Astrophysics ESAC 2014 Low Mass X-ray Binaries (LMXBs) Normal (
More informationUsing Microlensing to Probe Strong Gravity Near Supermassive Black Holes
Using Microlensing to Probe Strong Gravity Near Supermassive Black Holes Interstellar: Kip Thorne and Double Negative visual-effects team Presented by: George Chartas Chris Kochanek (OSU) Henric Krawczynski
More informationarxiv:astro-ph/ v1 5 Jan 1998
Discovery of KiloHertz Quasi-Periodic Oscillations in 4U 1735 44 Rudy Wijnands 1, Michiel van der Klis 1, Mariano Méndez 1,2, Jan van Paradijs 1,3, Walter H. G. Lewin 4, Frederick K. Lamb 5, Brian Vaughan
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 informationX-ray Nova XTE J : Discovery of a QPO Near 185 Hz
X-ray Nova XTE J1550-564: Discovery of a QPO Near 185 Hz Ronald A. Remillard Center for Space Research, Massachusetts Institute of Technology, Room 37-595, Cambridge MA 02139 Jeffrey E. McClintock Harvard-Smithsonian
More informationNon-linear resonance model for black hole and neutron star QPOs: observation and theory
Non-linear resonance model for black hole and neutron star QPOs: observation and theory Gabriel Török 1,2, Marek A. Abramowicz 1,2,3, Włodek Kluźniak 2,4, Zdeněk Stuchlík 1, Eva Šrámková 1,2 1 Institute
More informationQuasi-Periodic Brightness Oscillations from Accreting Neutron Stars and Black Holes
Quasi-Periodic Brightness Oscillations from Accreting Neutron Stars and Black Holes M. Coleman Miller 1 1 University of Maryland, Department of Astronomy, College Park, MD 20742-2421, USA; miller@astro.umd.edu
More informationA relativistically smeared line profile in the spectrum of the bright Z-source GX 340+0
A relativistically smeared line profile in the spectrum of the bright Z-source GX 340+0 Dipartimento di Scienze Fisiche ed Astronomiche. Università degli Studi di Palermo, Italy E-mail: dai@fisica.unipa.it
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 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 informationNeutron Star Seismology with Accreting Millisecond Pulsars
Neutron Star Seismology with Accreting Millisecond Pulsars Simin Mahmoodifar University of Maryland July 14, 2014 T. Strohmayer & S. Mahmoodifar, ApJ 784, 72 (2014) [arxiv:1310.5147 [astro-ph.he]] T. Strohmayer
More informationDiscovery of KiloHertz Quasi-Periodic Oscillations in the Z source Cygnus X-2
Discovery of KiloHertz Quasi-Periodic Oscillations in the Z source Cygnus X-2 Rudy Wijnands 1, Jeroen Homan 1, Michiel van der Klis 1, Erik Kuulkers 2, Jan van Paradijs 1,3, Walter H. G. Lewin 4, Frederick
More informationTime lags and reverberation in the lamp-post geometry of the compact corona illuminating a black-hole accretion disc
Time lags and reverberation in the lamp-post geometry of the compact corona illuminating a black-hole accretion disc Michal Dovčiak Astronomical Institute Academy of Sciences of the Czech Republic, Prague
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 informationarxiv: v1 [astro-ph.he] 28 Mar 2019
Astronomy & Astrophysics manuscript no. 33163arxiv c ESO 2019 March 29, 2019 Red-skewed Kα iron lines in GX 13+1. T. Maiolino, 1 P. Laurent, 2,3 L. Titarchuk, 1 M. Orlandini, 4 F. Frontera. 1,4,5 1 University
More informationarxiv:astro-ph/ v1 7 Aug 2006
arxiv:astro-ph/68145v1 7 Aug 26 Quasi Periodic Oscillations (QPOs) and frequencies in an accretion disk and comparison with the numerical results from non-rotating black hole computed by the GRH code Orhan
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 informationFundamental Physics, Astrophysics and Cosmology with ET
Fundamental Physics, Astrophysics and Cosmology with ET B.S. Sathyaprakash (CU) and Bernard Schutz (CU, AEI) based on a Living Review article with a similar title (in preparation) ET Science Summary Fundamental
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 informationAccreting Black Holes and Neutron Stars: a Unified View. Teo Muñoz Darias. Instituto de Astrofísica de Canarias
Accreting Black Holes and Neutron Stars: a Unified View Teo Muñoz Darias Instituto de Astrofísica de Canarias (Low Mass) X-ray Binaries Low-mass star transferring matter onto Black Hole / Neutron Star
More informationA Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 4151
A Suzaku, NuSTAR, and XMM-Newton view on variable absorption and relativistic reflection in NGC 411 T. Beuchert, A.G. Markowitz, T. Dauser, J.A. García, M.L. Keck, J. Wilms, M. Kadler, L.W. Brenneman,
More informationAccretion in Binaries
Accretion in Binaries Two paths for accretion Roche-lobe overflow Wind-fed accretion Classes of X-ray binaries Low-mass (BH and NS) High-mass (BH and NS) X-ray pulsars (NS) Be/X-ray binaries (NS) Roche
More informationarxiv:astro-ph/ v1 4 Jan 2007
Frequency Correlations of QPOs Based on a Disk Oscillation Model in Warped Disks Shoji Kato Department of Informatics, Nara Sangyo University, Ikoma-gun, Nara 636-8503 kato@io.nara-su.ac.jp, kato@kusastro.kyoto-u.ac.jp
More informationarxiv:astro-ph/ v1 31 Dec 1997
Oceanography of Accreting Neutron Stars: Non-Radial Oscillations and Periodic X-Ray Variability arxiv:astro-ph/9712358v1 31 Dec 1997 Lars Bildsten, Andrew Cumming, & Greg Ushomirsky Department of Physics,
More informationKilohertz QPO and Atoll Source States in 4U
Kilohertz QPO and Atoll Source States in 4U 0614+09 M. Méndez 1,2,M.vanderKlis 1,J.vanParadijs 1,3, W.H.G. Lewin 4,F.K.Lamb 5, B.A. Vaughan 6, E. Kuulkers 7, D. Psaltis 5 ABSTRACT We report three RXTE/PCA
More informationModelling Light Curves of Millisecond Period X-Ray Pulsars
Modelling Light Curves of Millisecond Period X-Ray Pulsars C. Cadeau and S.M. Morsink Theoretical Physics Institute, Department of Physics, University of Alberta, Edmonton, AB, T6G 2J, Canada Light curves
More informationimin...
Pulsar Timing For a detailed look at pulsar timing and other pulsar observing techniques, see the Handbook of Pulsar Astronomy by Duncan Lorimer and Michael Kramer. Pulsars are intrinsically interesting
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 informationEchoes of Black Holes: In Search of Rapidly Spinning Black Holes with Timing Observations. White Paper Submission to
Echoes of Black Holes: In Search of Rapidly Spinning Black Holes with Timing Observations White Paper Submission to Astro 2010: The Astronomy and Astrophysics Decadal Survey Stars and Stellar Evolution,
More informationA Multiwavelength Study of the Gamma-ray Binaries 1FGL J and LMC P3
A Multiwavelength Study of the Gamma-ray Binaries 1FGL J1018.6-5856 and LMC P3 1 Joel B. Coley NASA Postdoctoral Fellow, Mail Code 661, Astroparticle Physics Laboratory NASA Goddard Space Flight Center,
More informationEinstein, Black Holes and the Discovery of Gravitational Waves. Malcolm Longair University of Cambridge
Einstein, Black Holes and the Discovery of Gravitational Waves Malcolm Longair University of Cambridge Programme What are Black holes? Astronomical Evidence What are Gravitational Waves? The LIGO experiment
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 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 informationObservational Evidence of Black Holes Kolkata (India), Feb 2008
Observational Evidence of Black Holes Kolkata (India), Feb 2008 S Chakrabarti L Titarchuk R Kerr F Mirabel T Belloni S Zhang E Koerding T Alexander G Bisnovatyi-Kogan M DellaValle Z Paragi T Alexander
More informationPulsars. in this talk. Pulsar timing. Pulsar timing. Pulsar timing. Pulsar timing. How to listen to what exotic. are telling us! Paulo César C.
How to listen to what exotic Pulsars are telling us! in this talk 1. 2. 3. Test of gravitational theories using binary pulsars 4. Probing the equation of state of super-dense matter Paulo César C. Freire
More informationCenter for Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139; Jeffrey E.
The Astrophysical Journal, 580:1030 1042, 2002 December 1 # 2002. The American Astronomical Society. All rights reserved. Printed in U.S.A. EVIDENCE FOR HARMONIC RELATIONSHIPS IN THE HIGH-FREQUENCY QUASI-PERIODIC
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 informationMAXI and AGN X-ray Variability
MAXI and AGN X-ray Variability Ian M c Hardy 1 1 School of Physics and Astronomy, University of Southampton, University Road, Southampton SO17 1BJ, UK E-mail(IM): imh@astro.soton.ac.uk Abstract The X-ray
More informationCyclotron Line Science with LAXPC. Dipankar Bhattacharya IUCAA, Pune
Cyclotron Line Science with LAXPC Dipankar Bhattacharya IUCAA, Pune Workshop on Science with LAXPC/Astrosat, Hyderabad, 16 December 2014 A High Mass X-ray Binary Cyclotron Resonant Scattering Features
More informationEXTREME NEUTRON STARS
EXTREME NEUTRON STARS Christopher Thompson Canadian Institute for Theoretical Astrophysics University of Toronto SLAC Summer Institute 2005 Extreme Magnetism: B ~ 10 8-9 G (Low-mass X-ray binaries, millisecond
More informationAn explanation for the soft X-ray excess in AGN. Jamie Crummy collaborators: Andy Fabian, Luigi Gallo, Randy Ross Suzaku Team
An explanation for the soft X-ray excess in AGN Jamie Crummy collaborators: Andy Fabian, Luigi Gallo, Randy Ross Suzaku Team Soft excess The soft excess is at a constant temperature over a large range
More informationA search for burst spectral features with NICER. Jérôme Chenevez Gaurava Jaisawal DTU Space
A search for burst spectral features with NICER Jérôme Chenevez Gaurava Jaisawal DTU Space OUTLINE Why NICER? What: Absorption features during thermonuclear X-ray bursts Models Observations Prospects of
More informationAC Fabian, M. Cappi, J Sanders. Cosmic Feedback from AGN
AC Fabian, M. Cappi, J Sanders Cosmic Feedback from AGN AC Fabian, M Cappi, J Sanders, S Heinz, E Churazov, B McNamara, J Croston, D Worrall, F Humphrey, F Tombesi, J Reeves, M Giustini, P O Brien, T Reiprich
More informationarxiv: v2 [astro-ph.he] 27 Jan 2016
Draft version September 24, 2018 Preprint typeset using L A TEX style emulateapj v. 5/2/11 X-RAY BURST OSCILLATIONS: FROM FLAME SPREADING TO THE COOLING WAKE Simin Mahmoodifar and Tod Strohmayer Astrophysics
More informationarxiv:astro-ph/ v1 6 Jan 2000
Neutron Star Mass Determinations M. H. van Kerkwijk Utrecht University, P. O. Box 80000, 3508 TA Utrecht, The Netherlands arxiv:astro-ph/0001077v1 6 Jan 2000 Abstract. I review attempts made to determine
More informationAngular momentum conservation of bursting shell during the Type I X-ray burst
On the angular momentum conservation of bursting shell during the Type I X-ray bursts Vahid Rezania Theoretical Physics Institute Department of Physics University of Alberta Edmonton, Alberta Based on:
More informationNeutron star mass and radius constraints from X-ray bursts, accreting millisecond pulsars and X-ray polarization. Juri Poutanen
Neutron star mass and radius constraints from X-ray bursts, accreting millisecond pulsars and X-ray polarization Juri Poutanen University of Turku, Finland Nordita, Stockholm, Sweden Collaborators: Joonas
More informationX-ray Binaries: Spectroscopy & Variability
X-ray Binaries: Spectroscopy & Variability Michael Nowak (MIT-CXC) Jörn Wilms (Bamberg) Katja Pottschmidt (GSFC-UMBC) Sera Markoff (University of Amsterdam)... M Equilibrium 1.44 Star Black Stars End
More informationThe NuSTAR view of Radio-quiet AGN
The NuSTAR view of Radio-quiet AGN (Università degli Studi Roma Tre) on behalf of the NuSTAR AGN Physics WG Active Galactic Nuclei 11 Where Black Holes and Galaxies meet Trieste, 23-26 September 2014 Outline
More informationKilo-Hertz QPO and X-ray Bursts in 4U in Low Intensity State
Kilo-Hertz QPO and X-ray Bursts in 4U 1608-52 in Low Intensity State arxiv:astro-ph/9710069v2 9 Oct 1997 W. Yu, S. N. Zhang, B. A. Harmon, W. S. Paciesas, C. R. Robinson, J. E. Grindlay, P. Bloser, D.
More informationX-ray Outbursts from Black Hole Binaries. Ron Remillard Center for Space Research, MIT
X-ray Outbursts from Black Hole Binaries Ron Remillard Center for Space Research, MIT Outline Status Report on Black Hole Binaries X-ray States of Accreting Black Holes Modified State Definitions Outline
More informationUvA-DARE (Digital Academic Repository)
UvA-DARE (Digital Academic Repository) The beat frequency interpretation of kilohertz QPO's in neutron star low-mass X-ray binaries Psaltis, D.; Mendez, R.M.; Wijnands, R.A.D.; Homan, J.; Jonker, P.G.;
More informationBinary Pulsars and Evidence for Gravitational Radiation
Binary Pulsars and Evidence for Gravitational Radiation Matthew S. Paoletti Physics 798G March 29, 2007 http://www.rowes.com.au/csiro.htm Motivation Three classical tests of GR Bending of light as it passes
More informationCharged particle motion around magnetized black hole
Charged particle motion around magnetized black hole Martin Kološ, Arman Tursunov, Zdeněk Stuchĺık Silesian University in Opava, Czech Republic RAGtime workshop #19, 23-26 October, Opava 2017 Black hole
More informationX-ray spectroscopy of nearby galactic nuclear regions
X-ray spectroscopy of nearby galactic nuclear regions 1. How intermittent are AGNs? 2. What about the silent majority of the SMBHs? 3. How do SMBHs interplay with their environments? Q. Daniel Wang University
More informationTHE ATOLL SOURCE STATES OF 4U Steve van Straaten, 1 Michiel van der Klis, 1 and Mariano Méndez 2
The Astrophysical Journal, 596:1155 1176, 2003 October 20 # 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE ATO SOURCE STATES OF 4U 1608 52 Steve van Straaten, 1 Michiel
More informationUniversity of Groningen
University of Groningen Discovery of a Kilohertz Quasi-periodic Oscillation in 2S 0918-549 Jonker, Peter G.; van der Klis, Michiel; Homan, Jeroen; Méndez, Mariano; van Paradijs, Jan; Belloni, Tomaso; Kouveliotou,
More informationRadiation-hydrodynamic Models for ULXs and ULX-pulsars
Radiation-hydrodynamic Models for ULXs and ULX-pulsars Tomohisa KAWASHIMA Division of Theoretical Astrophysics, NAOJ in collaboration with Ken OHSUGA, Hiroyuki TAKAHASHI (NAOJ) Shin MINESHIGE, Takumi OGAWA
More information