BLACK HOLES (AND NEUTRON STARS) IN X-RAY BINARIES: Evolution and Accretion states TEO MUÑOZ DARIAS MARIE CURIE FELLOW. Oxford Astrophysics

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1 BLACK HOLES (AND NEUTRON STARS) IN X-RAY BINARIES: Evolution and Accretion states TEO MUÑOZ DARIAS MARIE CURIE FELLOW Oxford Astrophysics ESAC 2014

2 Low Mass X-ray Binaries (LMXBs) Normal (<1M SUN ) star transferring matter onto a compact object (Black hole / Neutron star) XRBs provide the best laboratories to study BH/NS 2

3 Most of the BLACK HOLES are TRANSIENT Quiescence / Outburst Credit: R. Hynes Credit: R. Hynes Dynamical Studies Accretion Processes General relativity

4 Most of the BLACK HOLES are TRANSIENT Quiescence / Outburst Credit: R. Hynes Credit: R. Hynes Dynamical Studies Accretion Processes General relativity

5 OUTLINE I. Accretion state picture for black hole Binaries: similarities to Neutron stars II. Inclination effects: how they do affect the Observed outburst evolution

6 Black Holes in Outburst Credit: R. Hynes Corona Jet Accretion disc Companion star Corona: Hard X-rays (up to 100 kev-1mev) Accretion disc: Soft X-rays (few kev) to Infrared Companion: only through X-ray reprocessing Jet: Radio to infrared/optical to high-energies(?) [NOT ALWAYS]

7 MULTIWAVELENGTH SOURCES Fν Radio IR Opt. X Disc companion Jet Corona Credit: Mickaël Coriat ν

8 MULTIWAVELENGTH SOURCES Fν Radio IR Opt. X Disc companion Accretion (X-ray) states Jet Corona Credit: Mickaël Coriat ν

9 BLACK HOLE IN OUTBURST: HYSTERESIS Daily basis monitoring (RXTE) Hardness-Intensity (Homan et al. 2001) X-ray Luminosity 1000 PCU2 count rate 100 Variability rms (%) Hardness-rms Hardness Belloni 2010 How hard the spectrum is

10 X-ray Luminosity THE VARIABILITY DIAGRAM Muñoz-Darias, Motta & Belloni, 2011 Variability

11 X-ray Luminosity THE VARIABILITY DIAGRAM Muñoz-Darias, Motta & Belloni, 2011 Variability Other state-dependent timing features (e.g. Oscillations)

12 TWO MAIN ACCRETION STATES hard dominates (Low)Hard state: hot corona X-ray Luminosity cold disk, large inner radius Inner hot flow or corona (Hard emission) soft (disk) disk (soft emission) hard Belloni kev 100 kev How hard the spectrum is

13 TWO MAIN ACCRETION STATES Hot inner flow or corona (Hard emission) disk (soft emission) soft (disk) hard X-ray Luminosity 1 kev 100 kev (High)Soft state: corona (different geometry?) hot disk, small inner radius soft dominates Belloni 2010 How hard the spectrum is

14 STATE-DEPENDENT RADIO JETS X-ray Luminosity Compact jet X-ray/Radio correlation (Gallo et al. 2003) soft dominates hard dominates soft (disk) hard Belloni 2010 soft (disk) hard 1 kev 100 kev How hard the spectrum is 1 kev 100 kev

15 STATE-DEPENDENT RADIO JETS Relativistic ejections X-ray Luminosity Compact jet X-ray/Radio correlation (Gallo et al. 2003) soft dominates hard dominates soft (disk) hard Belloni 2010 soft (disk) hard 1 kev 100 kev How hard the spectrum is 1 kev 100 kev

16 STATE-DEPENDENT RADIO JETS Relativistic ejections Soft State: NO JET (e.g. Russell et al 2011) Compact jet X-ray/Radio correlation (Gallo et al. 2003) soft dominates X-ray Luminosity hard dominates soft (disk) hard Belloni 2010 soft (disk) hard 1 kev 100 kev How hard the spectrum is 1 kev 100 kev

17 GLOBAL STUDIES: BLACK HOLES Large data base (~15 years of RXTE monitoring): systematic studies 25 Black Hole candidate studied by Dunn et al. Credit: Nasa Dunn et al. 2010

18 GLOBAL STUDIES: BLACK HOLES Large data base (~15 years of RXTE monitoring): systematic studies 25 Black Hole candidate studied by Dunn et al. Credit: Nasa Dunn et al. 2010

19 GLOBAL STUDIES: BLACK HOLES RXTE monitoring + Detailed studies using XMM and Chandra Credit: Nasa Ponti et al. 2012

20 TOWARDS A MORE COMPLETE PICTURE... Soft State: NO JET (e.g. Russell et al 2011) X-ray Luminosity soft dominates hard dominates soft (disk) hard Belloni 2010 soft (disk) hard 1 kev 100 kev How hard the spectrum is 1 kev 100 kev

21 TOWARDS A MORE COMPLETE PICTURE... Winds: a new key ingredient chandra.harvard Soft State: NO JET (e.g. Russell et al 2011) X-ray Luminosity soft dominates hard dominates soft (disk) hard Belloni 2010 soft (disk) hard 1 kev 100 kev How hard the spectrum is 1 kev 100 kev

22 NEUTRON STARS CAN BE SIMILAR Miller-Jones et al Brightest and more numerous: Studied first More complex behaviour ( Extra ) X-ray Luminosity Aql X-1 M o s t o f t h e m a r e persistent systems (but a few transients as well) Some transients look similar to Black holes X-ray Luminosity hardnesss

23 BLACK HOLE EVOLUTION AND LINE-OF-SIGHTS R.HYNES NASA Muñoz-Darias, Coriat, Plant, Ponti, Fender Dunn, MNRAS, 2013

24 INCLINATION EFFECTS Large data base (~15 years of RXTE monitoring): systematic studies Ponti et al. 2012

25 X-ray Luminosity Inclination effects: how they do affect the Hardness-intensity diagrams 1000 PCU2 count rate Belloni 2010 rms (%) 10 1 How hard the spectrum is Hardness

26 A CLOSER VIEW... RXTE absorption corrected fluxes (Dunn et al. 2010) GX Low Inclination High Inclination GRO Muñoz-Darias et al. 2013

27 A CLOSER VIEW... RXTE absorption corrected fluxes (Dunn et al. 2010) Low Inclination 4U GX XTE J XTE J XTE J XTE J High Inclination XTE J U H GRO

28 A CLOSER VIEW... RXTE absorption corrected fluxes (Dunn et al. 2010) Low Inclination 4U GX XTE J XTE J XTE J XTE J High Inclination XTE J U H GRO

29 ACCRETION DISCS AND GENERAL RELATIVITY Low inclination disc dominated by gravitational redshift R.HYNES NASA Gravitational redshift starts to be compensated by blue shifting when looking at higher inclinations.

ACCRETION DISCS AND GENERAL RELATIVITY Doppler beaming enhances blue-shifted light Low inclination disc dominated by gravitational redshift

30 ACCRETION DISCS AND GENERAL RELATIVITY Doppler beaming enhances blue-shifted light Low inclination disc dominated by gravitational redshift Light bending effects R.HYNES Dauser et al. Gravitational redshift starts to be compensated by blue shifting when looking at higher inclinations. NASA

31 ACCRETION DISCS AND GENERAL RELATIVITY Low inclination disc dominated by gravitational redshift Spin Spin (a) = 0.9M R.HYNES Gravitational redshift starts to be compensated by blue shifting when looking at higher inclinations. Li et al NASA

32 DO WE REALLY SEE THAT? Fits presented in Dunn et al (Newtonian discs (DISKBB)) TOBS = TPEAK fcol fgr [i,spin] (see e.g. Zhang, Cui & Chen 1997; Cunnigham 1975) Low Inclination High Inclination

33 DO WE REALLY SEE THAT? Fits presented in Dunn et al (Newtonian discs (DISKBB)) TOBS = TPEAK fcol fgr [i,spin] (see e.g. Zhang, Cui & Chen 1997; Cunnigham 1975) Low Inclination fgr [i,a=0.0] High Inclination

34 DO WE REALLY SEE THAT? Fits presented in Dunn et al (Newtonian discs (DISKBB)) TOBS = TPEAK fcol fgr [i,spin] (see e.g. Zhang, Cui & Chen 1997; Cunnigham 1975) Low Inclination fgr [i,a=0.998] High Inclination

35 DOES IT EXPLAIN EVERYTHING? Simulations using a KERRBB fully relativistic modeling

36 DOES IT EXPLAIN EVERYTHING? Simulations using a KERRBB fully relativistic modeling Other factors?

Accreting 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