2. OUTLINE X-RAY STATES & RADIO JETS (BLACK HOLES) Radio phenomenology vs accretion modes LUMINOSITY CORRELATIONS (BLACK HOLES) radio/X-ray NIR/X-ray dependence on X-ray binary parameters (lack thereof) Update: clustering algorithms, Bayesian analysis, linear regression BLACK HOLES VS NEUTRON STARS radio luminosity, bulk velocity BLACK HOLE SPIN & JET POWER

3. cf. Sera Markoff

4. Cyg X-1 Stirling et al.‘01 GRS1915+105 Mirabel et al. ‘94 1E140.7-2942 Mirabel et al. al ‘99 SS433 Blundell et al. 2004

5. Meyer, Liu & Meyer-Hofmeister 2006 Radiatively inefficient inflow (ADAF, CDAF, JDAF, ADIOS..) McClintock & Remillard 2006

6. Meyer, Liu & Meyer-Hofmeister 2006 McClintock & Remillard 2006 Cyg X-1 Stirling et al.‘01 Radiatively inefficient inflow (ADAF, CDAF, JDAF, ADIOS..)

7. X-ray states: high/soft (thermal dominat) Radiatively efficient inflow (thin disc) McClintock & Remillard 2006 Meyer, Liu & Meyer-Hofmeister 2006

8. X-ray states: high/soft (thermal dominat) Radiatively efficient inflow (thin disc) SUPPRESSED McClintock & Remillard 2006 Meyer, Liu & Meyer-Hofmeister 2006

9. X-ray states: hard to soft transition McClintock & Remillard 2006 JETS DURING HARD-TO-SOFT TRANSITIONS GRS1915+105 Mirabel et al 1994 Meyer, Liu & Meyer-Hofmeister 2006

10. Fender Belloni Gallo 2004; Fender Homan Belloni 2009

11. Corbel et al. 2003 4U1755-33 Angelini et al. 2003 Corbel et al. 2005

12. 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

13. Luminosity correlations I. X-ray/radio Corbel et al 2003, Gallo et al 2003, Gallo 2007

14. Luminosity correlations II. NIR/radio Russell et al 2006

15. Soleri & Fender 2010 Roche lobe radius Orbital period (No) Orbital parameters dependence

16. Soleri & Fender 2010 (Weak) Inclination dependence (NIR/X-ray)

17. Coriat et al. 2011 2 Tracks & Accretion mode transition ?

18. Gallo et al. in prep. Black hole X-ray binaries in the radio/X-ray domain: a statistical approach

19. Gallo et al. in prep. Black hole X-ray binaries in the radio/X-ray domain: a statistical approach

20. Gallo et al. in prep. Black hole X-ray binaries in the radio/X-ray domain: a statistical approach

21. Gallo et al. in prep. Black hole X-ray binaries in the radio/X-ray domain: a statistical approach

22. Black Holes vs Neutron Stars I. Black points: BHs Red points: NS atoll sources Blue points: NS Z sources after Migliari & Fender 2006

23. Black Holes vs Neutron Stars II. Fender et al 2004

24. Cyg X-1 Stirling et al.‘01 GRS1915+105 Mirabel et al. ‘94 1E140.7-2942 Mirabel et al. al ‘99 SS433 Blundell et al. 2004 Fabian et al 2000 obs / em

25. Cyg X-1 Stirling et al.‘01 Cf. Miller, Fabian, Cackett, Miniutti, Reis, Reynolds et al.

26. Cyg X-1 Stirling et al.‘01 R ISCO  a * H1743-322 (Kubota et al 2004) T eff 4..after color correction (cf. S. Davis) cf. McClintock, Shafee, Narayan, Steiner, Gou, Liu, Done, Gierlinski, Middleton

27. Constraints on spin powering of jets Fender Gallo Russell 2010

29. Hard state: Steady jets ReflectionDisk Fender Gallo Russell 2010 No apparent jet/spin correlation

30. State transitions: Transient jets ReflectionDisk Fender Gallo Russell 2010 No apparent jet/spin correlation

31. 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 STARS NSs factor ~30 fainter in radio However: the most relativistic jet source in the Galaxy is a neutron star BLACK HOLE SPIN & JET POWER No apparent relation: IF the measurements are robust (..) => Jets are not powered by BH rotational energy SUMMARY