Black-hole binaries in the ASTROSAT era

Tomaso Belloni (INAF - Osservatorio Astronomico di Brera)(Visiting Professor, University of Southampton)

TIFR Mumbai20 JANUARY 2016

Soft state

• Thin disk model a spectacular success

• Still an additional component is present(always?)

Davis et al. (2005)

Gro

ve e

t al.

(199

8)

• A quiet disk

• Lots of complications

• Hybrid models

• Jet models

Hard state

Sunyaev & Trümper (1979)Sunyaev & Titarchuk (1980)

Zdziarski & Gierliński (2004)

• A restless flow

Geometry unclear

Petrucci (2009)

Thermal

disk

photon

Hard

Comptonized

Photon

Soft disk Hard e –

Same kT,τ Same kT

Hybrid plasma?

Del Santo (2008)

Jet contribution

Markoff (2009)

We need more information: timing

Grove et al. (1998)

Low-Hard State (Cygnus X-1)

High-Soft State (GX 339-4)

Pow

er

10-4

10-3

10-2

10-1

100

101

102

Pow

er

0.001

0.01

0.1

1

10

100

1000

Frequency (Hz)0.01 0.1 1 10 100

Belloni (2010)

Spectra Timing

THE RXTE BLACK-HOLE PARADIGM

Fender & Belloni (2012)

A YEAR IN THE LIFE OF GX 339-4

SOME OPEN QUESTIONS

• Hysteresis: why and how?

• Why not clockwise?

• Nature of hard components

• Transitions

• Jet connection (Rob’s talk)

• Wind connection (Joel’s talk)

Esin et al. (1997)

Grove et al. (1998)

Middleton et al. (2006)

Motta, TMB, Homan (2009)

Stiele et al. (2011)

Jet line

SPECTRA

HIGH-ENERGY EVOLUTION

Motta et al. (2009)

TIMING

Jet line

QPOs

• Type-C: relativistic precessions

• Type-A: type-C

• Type-B: jet?

• HFQPO: relativistic precession/orbit

GRO J1655-40: UNIQUE SOURCE

MOTTA, BELLONI ET AL. (2014A)

Only source which shows simultaneous type-C and 2xHFQPO

type-C

XTE J1550-564: THE NEXT BEST

MOTTA ET AL. (2014B)

It shows simultaneous type-C and 1xHFQPO

type B

typeC = 13.08 +- 0.08 Hz HFQPO = 183 +/- 5 Hz

RELATIVISTIC MODEL: SPIN!

Solution for

a = 0.29 +/- 0.01

M = 5.31 +/- 0.07 M⊙

R = 5.68 +/- 0.04 Rg

Dynamical mass:

M = 5.4 +/- 0.3 M⊙

Solution for

a = 0.34 +/- 0.01

R = 5.47 +/- 0.12 Rg

Dynamical mass:

M = 9.1 +/- 0.6 M⊙

GRO J1655-40 XTE J1550-564MOTTA ET AL. (2014A,B)

EVEN LOW FREQUENCIESGRO J1655-40 XTE J1550-564

MOTTA ET AL. (2014A,B)

QPOs

• Type-B: jets

MOTTA ET AL. (2015)

ANOMALOUS STATE

• If Ṁ does not stop

• Here HFQPO: no disk

• Energy spectrum isdifferent

• Timing is different

ANOMALOUS STATE: SPECTRUM

• Hybrid plasma

• At peak, slim disk model BELLODI ET AL. (2015)

A ZEROTH-LEVEL MODEL

• Accretion rate vs. time: bell-shaped (up then down)

• High accretion rate: S&S disk

• Low-accretion rate: ADAF

KYLAFIS & BELLONI (2015)

Jet LineHSS

HIMSSIMS

LHS

HIMS

HIMS-SIMSRapid transitionswith radio flares

Hardness

LX/LEdd

0.1

0.01

0.001

QS

SIMSrms

1%

10%

40%

ASIMS

B

C

D

ABEC

D

E

Rtr

A ZEROTH-LEVEL MODEL

KYLAFIS & BELLONI (2015)

Jet LineHSS

HIMSSIMS

LHS

HIMS

HIMS-SIMSRapid transitionswith radio flares

Hardness

LX/LEdd

0.1

0.01

0.001

QS

SIMSrms

1%

10%

40%

ASIMS

B

C

D

ABEC

D

E

Ṁ

Rtr

RISCO

A

B

CD

E

}

JETS AND HYSTERESIS

KYLAFIS & BELLONI (2015)

• Cosmic Battery mechanism

• System memory

A WORD ON NEUTRON STAR BINARIES

BELLONI, PSALTIS & VAN DER KLIS (2002)

BU ET AL (2015)

SOME QUESTIONS

• How is the transition between thermal and non-thermal?

• What is the geometry?

• What is the jet contribution?

• Where does the variability come from and who makes it?

• What is the soft-state variability?

• Are the QPOs from GR and jet effects?

• How can we answer these questions?

ASTROSAT

HTRA - Άγιος Νικόλαος

PCA LAXPC

PDS

CZTI

Timing software