Galloway, “Accreting neutron stars and the equation of state” Accreting neutron star spins and the equation of state Duncan Galloway Monash University.

Slides:

Advertisements

Similar presentations

Envelopes and thermal radiation of neutron stars with strong magnetic fields Alexander Y. Potekhin 1 in collaboration with D.G.Yakovlev, 1 A.D.Kaminker,

Advertisements

The Neutron Star Equation of State- Electromagnetic Observations Frits Paerels Columbia University GWPAW, UW Milwaukee, January 26, 2011.

The Evolution of Stars. Binary Star Evolution About half the stars in the sky are binaries. These stars may begin life as separate entities, but often.

Abstract We present first modeling results of the rapid spectral variability of flares in the X-ray binary Cygnus X-1 in the high/soft state. The coupled.

Mass and Radius Constraints Using Magnetar Giant Flare Oscillations Alex T. Deibel With: Edward F. Brown (Michigan State University) Andrew W. Steiner.

Peeking into the crust of a neutron star Nathalie DegenaarUniversity of Michigan X-ray observations Interior properties Thermal evolution.

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.

Mass transfer in a binary system

Neutron Stars and Black Holes

Athena+, ESA’s next generation X-ray observatory Gregor Rauw High-Energy Astrophysics Group Liège University on behalf of the Athena+ coordination group.

X-ray polarisation: Science

Vicky Kaspi McGill University Lorne Trottier Chair in Astrophysics and Cosmology.

Peeking into the crust of a neutron star Nathalie Degenaar University of Michigan.

Gravitationally Redshifted Absorption Lines in the X-Ray Burst Spectra NTHU Lu, Ting-Ni.

X Ray Astronomy Presented by:- Mohit Shashwat Ankit.

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.

Pulsars in Low-Mass X-Ray Binaries Deepto Chakrabarty Massachusetts Institute of Technology.

Using Observables in LMXBs to Constrain the Nature of Pulsar Dong, Zhe & Xu, Ren-Xin Peking University Sep. 16 th 2006.

Galloway, Nuclear burning on the surface of accreting neutron stars Nuclear burning on the surface of accreting neutron stars Duncan Galloway University.

LIGO-G W What If We Could Listen to the Stars? Fred Raab LIGO Hanford Observatory.

Galloway, “Accreting neutron star spins and the prospects for GW searches” 1 Accreting neutron star spins and the prospects for GW searches Duncan Galloway.

Black Holes Written for Summer Honors Black Holes Massive stars greater than 10 M  upon collapse compress their cores so much that no pressure.

Gravitational waves LIGO (Laser Interferometer Gravitational-Wave Observatory ) in Louisiana. A laser beam is.

The rapid proton capture process (rp-process). Nova Cygni 1992 with HST Sites of the rp-process KS with Chandra E composite Novae -wind.

Neutron Stars and Black Holes PHYS390: Astrophysics Professor Lee Carkner Lecture 18.

Thermonuclear burst spectroscopy with LOFT LOFT meeting Oct 2011, UvA Duncan Galloway Hauke Worpel Monash University

Galloway, Breaking the AMSP mould: HETE J Breaking the AMSP mould: the increasingly strange case of HETE J Duncan Galloway Monash.

Determining the Equation of State of Ultradense Matter with the Advanced X-ray Timing Array (AXTAR) Deepto Chakrabarty (MIT) Paul S. Ray (NRL) Tod Strohmayer.

The Deaths of Stars Chapter 10. Mass Transfer in Binary Stars In a binary system, each star controls a finite region of space, bounded by the Roche Lobes.

Chapter 10 – part 3 - Neutron stars and Black Holes Neutron stars.

Neutron Stars. Discovery of neutron (1932) Neutron Star (1934) –Landau (unpublished) –Baade & Zwicky “With all reserve we advance the view that supernovae.

Neutron Stars and Black Holes Chapter 14. Formation of Neutron Stars Compact objects more massive than the Chandrasekhar Limit (1.4 M sun ) collapse beyond.

Constraining Neutron Star Radii and Equations of State Josh Grindlay Harvard (collaboration with Slavko Bogdanov McGill Univ.)

O n t h e T r a c k o f M o d e r n P h y s i c s Crab Nebula testifies the Supernova explosion in 1054AD, noted in Europe, China and by Indians in New.

Gravitational waves and neutrino emission from the merger of binary neutron stars Kenta Kiuchi Collaboration with Y. Sekiguchi, K. Kyutoku, M. Shibata.

Accretion Phenomena in Accreting Neutron Stars From atol to Z-sources Norbert S. Schulz, L. Ji, M. Nowak Claude R. Canizares MIT Kavli Institute for Astrophysics.

Timing and Spectral Properties of Neutron Star Low-Mass X-ray Binaries Sudip Bhattacharyya Department of Astronomy and Astrophysics Tata Institute of Fundamental.

Plasma universe Fluctuations in the primordial plasma are observed in the cosmic microwave background ESA Planck satellite to be launched in 2007 Data.

Merger of binary neutron stars in general relativity M. Shibata (U. Tokyo) Jan 19, 2007 at U. Tokyo.

COOLING NEUTRON STARS: THEORY AND OBSERVATIONS D.G. Yakovlev Ioffe Physical Technical Institute, St.-Petersburg, Russia Hirschegg – January – 2009 Introduction.

Ann Hornschemeier NASA Deputy Project Scientist NASA GSFC For Jay Bookbinder and the IXO Team.

The cooling-flow problem

Neutron Star Binaries and Related Astrophysical Issues Chang-Hwan 1.

Cosmic Rays GNEP Teacher Workshop Steve Shropshire, July 2007.

Probing the neutron star physics with accreting neutron stars (part 2) Alessandro Patruno University of Amsterdam The Netherlands.

Current Status of Neutron Stars: Astrophysical Point of View Chang-Hwan 1.

Accreting Neutron Stars – tiny Galactic Powerhouses HWWS, July 2010, Woodfield Centre Duncan Galloway Monash University

LIGO- G Z August 19, 2004LIGO Scientific Collaboration 1 The r-modes look good again in accreting neutron stars Ben Owen with Mohit Nayyar.

The RAPTOR (RAPid Telescopes for Optical Response) telescopes and GeV/TeV gamma-ray astronomy vestrandAspen Meeting---Galactic GeV/TeV sources.

Black holes and accretion flows Chris Done University of Durham.

Earth & Space Science March 2015

Abbas Askar University of Belgrade 12 th November 2011 Astronomy Workshop Presentation Belgrade, Serbia.

Goal: To understand special stars. Objectives: 1)To learn about Neutron Stars 2)To learn about Pulsars 3)To understand Stars that erupt.

Nuclear Spectroscopic Telescope Array What can NuSTAR do for thermonuclear X-ray bursts? Jérôme Chenevez 1, J. Tomsick 2, D. Chakrabarty.

Accreting neutron stars as gravitational wave sources Duncan Galloway Andrew Melatos University of Melbourne Ed Morgan Deepto Chakrabarty Center for Space.

The Search for Black Holes

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.

Some theoretical aspects of Magnetars Monika Sinha Indian Institute of Technology Jodhpur.

White dwarfs cool off and grow dimmer with time. The White Dwarf Limit A white dwarf cannot be more massive than 1.4M Sun, the white dwarf limit (or Chandrasekhar.

Chapter 13 Neutron Stars and Black Holes. Optical, Infrared and X-ray Image of Cassiopeia A.

Exploring an evidence of supermassive black hole binaries in AGN with MAXI Naoki Isobe (RIKEN, ) and the MAXI

The Search for Black Holes

Pulsars High Energy Astrophysics

In this talk Deep crustal heating on accreting neutron stars The fate of accreted matter, and deep crustal heating. NEW: heating is sensitive to composition.

Supernova Type 1 Supernova Produced in a binary system containing a white dwarf. The mechanism is the same (?) as what produces the nova event.

Constraining the Equation Of State (EOS) of neutron stars with eXTP/GDP Long Ji.

 Electromagnetic Radiation › Gamma rays, X-rays, UV light, visible light, infrared radiation, microwaves, and radio waves › All energy travels through.

Constraints on the mass and radius of neutron star in Aql X-1 Zhaosheng Li ( 李兆升 ) Department of Astronomy Peking University.

The Centre of the Solar System Earth Science 11

Presentation transcript:

Galloway, “Accreting neutron stars and the equation of state” Accreting neutron star spins and the equation of state Duncan Galloway Monash University Deepto Chakrabarty Center for Space Research, MIT Andrew Cumming McGill University, Canada MAD ‘07, November 2007

Galloway, “Accreting neutron stars and the equation of state” What is a neutron star made of? Theory predicts in detail the likely structure in outer layers Crust (1-2km) nuclei (mainly 56 Fe) plus neutrons ( 1 S 0 superfluid?) Composition of inner & outer cores (up to 99% of mass) however EXTREMELY uncertain; Hyperons? Pions? Kaons? Quark matter? How can we find out? (Figure courtesy D. Page)

Galloway, “Accreting neutron stars and the equation of state” Constraining the equation of state Basically we want a simultaneous mass and radius measurement from a neutron star This can be achieved by Detection of rapidly-rotating neutron stars (in LMXBs or elsewhere) Measurements of the neutron-star radius from the spectrum of thermonuclear (type-I) burst tails Measurement of the Eddington limit from radius-expansion bursts Detecting discrete spectral features from the neutron star surface Measurement of the heat flux from the crust via thermonuclear burst recurrence times & energetics …?

Galloway, “Accreting neutron stars and the equation of state” Low-mass X-ray binaries

Galloway, “Accreting neutron stars and the equation of state” (Some) present-day instruments RXTE, launched 1995 (NASA) large effective area and very high timing resolution but no imaging capability [2-200 keV] Chandra, launched 1999 (NASA), small effective area but very high spatial and spectral resolution (courtesy transmission gratings) [ keV] XMM-Newton, launched 1999 (ESA), moderate effective area, spatial and spectral resolution (reflection gratings) + optical monitor [ keV] INTEGRAL, launched 2002 (ESA), primarily gamma-ray instrument but also wide-field X-ray and optical capability [4 keV - 10 MeV]

Galloway, “Accreting neutron stars and the equation of state” Constraints via rapid spin Allowed region is to the left of the dashed curves While the robust maximum spin rate is still 716 Hz… …a neutron star spinning at 1122 Hz or faster would rule out many EOSs… So it’s not enough to find neutron stars spinning above the present maximum; we really want to be well above 1000 Hz Given the present limit of 716 Hz, this seems unlikely Lattimer & Prakash 2007

Galloway, “Accreting neutron stars and the equation of state” Gravitational wave observatories There are currently ~4 interferometric gravitational wave observatories operational worldwide Candidate sources include binary inspirals, stochastic background and rapidly rotating neutron stars Hotly anticipated first detection of gravitational waves, perhaps within the next decade!

Galloway, “Accreting neutron stars and the equation of state” Examples of X-ray bursts from RXTE

Galloway, “Accreting neutron stars and the equation of state” Constraints from thermonuclear bursts We can measure the radius of the neutron star from the (~blackbody) emission in the burst tail Burst recurrence time depends on the heat flux from the interior -> composition We have lots of good quality (archival) data! (RXTE catalog, MINBAR project)

Galloway, “Accreting neutron stars and the equation of state” For more high-energy fun… Monthly High-Energy Astrophysics Teleconference (HEAT); Stephen Ng to join the mailing list High-energy Astrophysics Workshop, Kialoa, NSW, April ; details TBA research areas & honours/PhD projectshttp://