Light Curves These light curves were taken by the Swift Gamma-Ray Burst Explorer & Rossi X-Ray Timing Explorer Each graph plots the counts of x-rays with.

Slides:



Advertisements
Similar presentations
X-ray pulsars in wind-fed accretion systems 王 伟 (NAOC) July 2009, Pulsar Summer School Beijing.
Advertisements

Vela X-1: Flares & Off States West Orange High School Manthan Kothari, Lucy Zipf, Neil Savalia, Brian Meise, Krish Pillai.
Ryo Yamazaki (Osaka University, Japan) With K. Ioka, F. Takahara, and N. Shibazaki.
Suzaku studies of SFXTs The X-ray Universe 2011 The University of Tokyo M.Sasano K.Nakajima, S.Yamada, T. Yuasa, K.Nakazawa, K. Makishima.
Bruce Gendre Osservatorio di Roma / ASI Science Data Center Recent activities from the TAROT/Zadko network.
Swift observations of black hole candidate XTE J with P. Casella. T.J. Maccarone & P.A. Evans Peter A. Curran Laboratoire AIM, Irfu /Service d'Astrophysique.
Mass transfer in a binary system
Neutron Stars and Black Holes
Neutron Stars Chapter Twenty-Three.
INPE Advanced Course on Compact Objects Course IV: Accretion Processes in Neutron Stars & Black Holes Ron Remillard Kavli Center for Astrophysics and Space.
Outbursts and State Transitions in Black Hole Candidates observed by MAXI Hitoshi Negoro (Nihon U.) & MAXI Team.
RHESSI 2003 October 28 Time Histories Falling fluxes following the peak Nuclear/511 keV line flux delayed relative to bremsstrahlung Fit to 511 keV line.
Working Group 2 - Ion acceleration and interactions.
Vojtech Simon v Monitoring of the X-ray long- term activity of Aquila X-1 v Astronomical Institute, The Czech Academy of Sciences, Ondrejov, Czech.
What Are the Faint X-ray Transients Near the Galactic Center? Michael Muno (UCLA/Hubble Fellow) Fred Baganoff (MIT), Eric Pfahl (UVa), Niel Brandt, Gordon.
QUASARS Monsters of the ancient Universe Professor Jill Bechtold Steward Observatory Tucson Amateur Astronomers, Dec. 6, 2002.
1. White Dwarf If initial star mass < 8 M Sun or so. (and remember: Maximum WD mass is 1.4 M Sun, radius is about that of the Earth) 2. Neutron Star If.
The Nature of γ-ray Source 3EG J 陳致維 Chen Chih-Wei.
Neutron Stars and Black Holes PHYS390: Astrophysics Professor Lee Carkner Lecture 18.
Late-phase hard X-ray emission from flares The prototype event (right): March 30, 1969 (Frost & Dennis, 1971), a very bright over-the-limb event with a.
Chapter 10 – part 3 - Neutron stars and Black Holes Neutron stars.
The general theory of relativity is our most accurate description of gravitation Published by Einstein in 1915, this is a theory of gravity A massive object.
Gamma Ray Bursts and LIGO Emelie Harstad University of Oregon HEP Group Meeting Aug 6, 2007.
Constraints on X-ray polarization of synchrotron jets from stellar-mass BHs Dave Russell niversity of Amsterdam In collaboration with: Dipankar Maitra,
HETE- 2 OBSERVATIONS OF THE EXTREMELY SOFT X-RAY FLASH XRF Liang Jau-shian Institute of Physics, NTHU.
Neutron star low-mass X-ray binaries Rudy Wijnands Anton Pannekoek Institute for Astronomy University of Amsterdam 3 August 2015Lorentz center, Leiden.
Discovery and Evolution of a New Galactic Black Hole Candidate XTE J Discovery and Evolution of a New Galactic Black Hole Candidate XTE J
Black holes: do they exist?
Light and the Electromagnetic Spectrum. Light Phenomenon Isaac Newton ( ) believed light consisted of particles By 1900 most scientists believed.
Conclusions We established the characteristics of the Fe K line emission in these sources. In 7 observations, we did not detect the source significantly.
An absorbed view of a new class of INTEGRAL sources.
Multiwaveband Opportunities to Study AGN (Mostly Blazars) Detected by Fermi Alan Marscher Boston University, Incoming Chair of Fermi Users Group Research.
Gamma-Ray Bursts observed with INTEGRAL and XMM- Newton Sinead McGlynn School of Physics University College Dublin.
Abstract LS 5039 and LS I are exceptionally rare examples of HMXBs with MeV-TeV emission, making them two of only four known "  -ray binaries".
Discovery of powerful millisecond flares from Cyg X-1 Marek Gierliński University of Durham, England Andrzej Zdziarski N. Copernicus Astronomical Center,
Death of Stars III Physics 113 Goderya Chapter(s): 14 Learning Outcomes:
Gamma-Ray Bursts observed by XMM-Newton Paul O’Brien X-ray and Observational Astronomy Group, University of Leicester Collaborators:- James Reeves, Darach.
Sub-Eddington accretion flows in neutron-star low-mass X-ray binaries Rudy Wijnands Astronomical Institute “Anton Pannekoek” University of Amsterdam 25.
The X-ray Universe Sarah Bank Presented July 22, 2004.
CEA DSM Dapnia SAp Diego Gotz - Hard X-ray tails in Magnetars 15/05/ Hard X-ray Tails in Magnetars A Case Study for Simbol-X Diego Götz CEA Saclay.
A Tidal Disruption model for gamma-ray burst of GRB YE LU National Astronomical Observatories, Chinese Academy of Sciences June 22-27, 2008 Nanjing.
Isolating the jet in broadband spectra of XBs Dave Russell niversity of Amsterdam In collaboration with: Fraser Lewis, Dipankar Maitra, Robert Dunn, Sera.
INPE Advanced Course on Compact Objects Course IV: Accretion Processes in Neutron Stars & Black Holes Ron Remillard Kavli Center for Astrophysics and Space.
Historical SN and their properties Total energy released ~10 54 erg in a few hours.
Stochastic Wake Field particle acceleration in GRB G. Barbiellini (1), F. Longo (1), N.Omodei (2), P.Tommasini (3), D.Giulietti (3), A.Celotti (4), M.Tavani.
Jets Two classes of jets from X-ray binaries
MAGNETARS Vicky Kaspi Montreal, Canada STScI May 10, 2006.
The black hole X-ray nova XTE J was discovered by RXTE (Atel #2258) on October 23, The Gas Slit Camera (GSC) on-board the Monitor of All-sky.
Abbas Askar University of Belgrade 12 th November 2011 Astronomy Workshop Presentation Belgrade, Serbia.
1 Chang-Hwan Spin of Stellar Mass Black Holes: Hypernova and BH Spin Correlation in Soft X-ray BH Binaries.
The Character of High Energy Emission From The Galactic Binary LS Andy Smith Smithsonian Astrophysical Observatory (for the VERITAS collaboration)
Stellar Corpses and Other Space Oddities
The central engine: relativistic effects Giovanni Miniutti AGN IX – Ferrara – May 2010.
Gamma-Ray Bursts. Short (sub-second to minutes) flashes of gamma- rays, for ~ 30 years not associated with any counterparts in other wavelength bands.
Jérôme Chenevez INTEGRAL monitoring of unusually Long X-ray bursts Maurizio Falanga Erik Kuulkers Søren Brandt Niels Lund Andrew Cumming Duncan Galloway.
Star Gobbles Up Its Friend by Universe today Star Eats Companion by ESA news 6 September 2005 Integral and RXTE observations of accreting millisecond pulsar.
Exploring an evidence of supermassive black hole binaries in AGN with MAXI Naoki Isobe (RIKEN, ) and the MAXI
Chapter 21 Galaxy Evolution Looking Back Through Time Our goals for learning How do we observe the life histories of galaxies? How did galaxies.
Stochastic wake field particle acceleration in Gamma-Ray Bursts Barbiellini G., Longo F. (1), Omodei N. (2), Giulietti D., Tommassini P. (3), Celotti A.
W.Becker 1, M.C.Weisskopf 2, Z.Arzoumanian 3, D.Lorimer 4, F.Camilo 5, R.F.Elsner 2, G.Kanbach 1, O.Reimer 6, D.A.Swartz 2, A.F.Tennant 2, S.L.O’Dell 2.
High Energy Observational Astrophysics. 1 Processes that emit X-rays and Gamma rays.
Gamma-ray bursts Tomasz Bulik CAM K, Warsaw. Outline ● Observations: prompt gamma emission, afterglows ● Theoretical modeling ● Current challenges in.
Gamma-Ray Bursts Please press “1” to test your transmitter.
RXTE Spectral Observations of the Galactic Microquasar GRO J1655-40
Black Hole Binaries in Quiescence
Observation of microquasars with the MAGIC telescope
Light and the Electromagnetic Spectrum
Correlation Time Scales of the X-ray Flux in Low Mass X-ray Binary
Black Hole Jets Acceleration of jets Collimation of jets
Black Hole Jets Acceleration of jets Collimation of jets
Presentation transcript:

Light Curves These light curves were taken by the Swift Gamma-Ray Burst Explorer & Rossi X-Ray Timing Explorer Each graph plots the counts of x-rays with a particular energy per second over the duration of the event Before the outburst, the flux from the system was consistently 1/100 th of the peak ‘Hard’ x-rays are higher energy than ‘soft’ x-rays As we will see in the next slide, we care about the ratio of the hard flux (E > 5 keV) to the soft flux (E <5keV) This ratio is called the hardness Light curves of the outburst taken from Krimm et al.

Current Interpretation The outburst decay rate was consistent with an x-ray burst transient The spectra 1 showed what Krimm et al. interpreted as an iron line at 6.72 ±.58 keV Observations have found have found very low flux at quiescence This suggests that the companion star is of low mass Hardness vs. Flux (Intensity), taken from Krimm et al. Two possibilities for a LMXRB – a black hole or a neutron star Neutron star x-ray hardness/intensity curves either trace a distinct Z shape (so- called ‘Z Sources’) or lack the observed hard/high flux The transitions from hard to soft- intermediate are thought to be faster with neutron stars 1 The paper did not include individual spectrum

Swift J shares many traits with confirmed BH outbursts Rapid rise of hard X rays followed by a soft flux about 8 days later is very similar to confirmed BH GRO J Temporary hardening in the middle of the outburst very similar to XTE J PL index, disk fraction, and rms power all correlate with X-ray hardness in a way that is indicative of a black hole (see figure) In addition to these shared traits, no pulsations were observed during the recorded outburst Further Evidence for Candidacy Hardness vs. key features from Krimm et al.

Mass from the companion star falls onto the compact object until an outburst occurs The properties of the outburst can help identify the compact object The outburst of Swift J shows several features of a BH, but no high-energy radio jet was observed This is a problem because these jets are an integral part of BHs Due to the power of a BH’s magnetic field, you would not expect to see a BH without seeing a jet in every wavelength! Without a jet in the radio we can’t define of Swift J as a BH Jet of M87’s Supermassive BH Could Swift J be a neutron star or an anomalous nova? (most likely not) An Unresolved Issue

Detecting High Energy Radio Jets Proving this anomaly is indeed a BH. Typical radio images from a BH. 1)Material rotates around BH, some of which is Ionized. 2)Ionized Material causes moving charges, which in-turn creates a B-field which in this case twists causing streams of jets that can be observed by ground-based radio observatories. Very Large Array Reason why H. A. Krimm et al. did not have radio data. Lack of observation time needed to confirm that this is a BH. However there is really sufficient evidence to deduce that it most probably is a BH without radio data.