OUTLINE

X-RAY STATES & RADIO JETS (BLACK HOLES)Radio phenomenology vs accretion modes

LUMINOSITY CORRELATIONS (BLACK HOLES)radio/X-rayNIR/X-raydependence on X-ray binary parameters (lack thereof)Update: clustering algorithms, Bayesian analysis, linear regression

BLACK HOLES VS NEUTRON STARSradio luminosity, bulk velocity

BLACK HOLE SPIN & JET POWER

cf. Sera Markoff

Cyg X-1Stirling et al.‘01

GRS1915+105Mirabel et al. ‘94

1E140.7-2942 Mirabel et al. al ‘99

SS433Blundell et al. 2004

Meyer, Liu & Meyer-Hofmeister 2006

Radiatively inefficient inflow (ADAF, CDAF, JDAF, ADIOS..)

McClintock & Remillard 2006

Meyer, Liu & Meyer-Hofmeister 2006

McClintock & Remillard 2006

Cyg X-1Stirling et al.‘01

Radiatively inefficient inflow (ADAF, CDAF, JDAF, ADIOS..)

X-ray states: high/soft (thermal dominat)

Radiatively efficient inflow (thin disc)

McClintock & Remillard 2006

Meyer, Liu & Meyer-Hofmeister 2006

X-ray states: high/soft (thermal dominat)

Radiatively efficient inflow (thin disc)

SUPPRESSED

McClintock & Remillard 2006

Meyer, Liu & Meyer-Hofmeister 2006

X-ray states: hard to soft transition

McClintock & Remillard 2006

JETS DURING HARD-TO-SOFT TRANSITIONS

GRS1915+105Mirabel et al 1994

Meyer, Liu & Meyer-Hofmeister 2006

Fender Belloni Gallo 2004; Fender Homan Belloni 2009

Corbel et al. 2003

4U1755-33 Angelini et al. 2003

Corbel et al. 2005

Gallo et al. 2005

Jet-powered nebulae

Cygnus X-1, Isaac Newton Russell et al. 2006

SS433 W50, VLA, Dubner et al. 1998

Cyg X-1, WRST

Luminosity correlations I. X-ray/radio

Corbel et al 2003, Gallo et al 2003, Gallo 2007

Luminosity correlations II. NIR/radio

Russell et al 2006

Soleri & Fender 2010

Roche lobe radius Orbital period

(No) Orbital parameters dependence

Soleri & Fender 2010

(Weak) Inclination dependence (NIR/X-ray)

Coriat et al. 2011

2 Tracks & Accretion mode transition ?

Gallo et al. in prep.

Black hole X-ray binaries in the radio/X-ray domain: a statistical approach

Gallo et al. in prep.

Black hole X-ray binaries in the radio/X-ray domain: a statistical approach

Gallo et al. in prep.

Black hole X-ray binaries in the radio/X-ray domain: a statistical approach

Gallo et al. in prep.

Black hole X-ray binaries in the radio/X-ray domain: a statistical approach

Black Holes vs Neutron Stars I.

• Black points: BHs• Red points: NS atoll sources• Blue points: NS Z sources

after Migliari & Fender 2006

Black Holes vs Neutron Stars II.

Fender et al 2004

Cyg X-1Stirling et al.‘01

GRS1915+105Mirabel et al. ‘94

1E140.7-2942 Mirabel et al. al ‘99

SS433Blundell et al. 2004

Fabian et al 2000

obs/em

Cyg X-1Stirling et al.‘01

Cf. Miller, Fabian, Cackett, Miniutti, Reis, Reynolds et al.

Cyg X-1Stirling et al.‘01

RISCO a*

H1743-322 (Kubota et al 2004)

Teff4

..after color correction (cf. S. Davis)

cf. McClintock, Shafee, Narayan, Steiner, Gou, Liu, Done, Gierlinski, Middleton

Constraints on spin powering of jets

Fender Gallo Russell 2010

Fender Gallo Russell 2010

Hard state: Steady jets

Reflection Disk

Fender Gallo Russell 2010

No apparent jet/spin correlation

State transitions: Transient jets

Reflection Disk

Fender Gallo Russell 2010

No apparent jet/spin correlation

X-RAY STATES & RADIO JETS (BLACK HOLES)Phenomenology – well understood.

LUMINOSITY CORRELATIONS (BLACK HOLES)No dependence on X-ray binary orbital parameters, nor

outburst properties. Very weak dependence on jet axis.Statistically significant evidence for 2 separate clusters in the

radio/X-ray domain. Universal correlation..no longer such.

BLACK HOLES VS NEUTRON STARSNSs factor ~30 fainter in radioHowever: the most relativistic jet source in the Galaxy is aneutron star

BLACK HOLE SPIN & JET POWERNo apparent relation: IF the measurements are robust (..)=> Jets are not powered by BH rotational energy

SUMMARY