1. Jets and environment of microquasars
Jingfang Hao 郝景芳
Adivisor: Shuang Nan Zhang 张双南
Tsinghua University, Beijing, China
University of Alabama in Huntsville, China
Collaborators: Zhixing Ling

2. 1. Large Scale Jets in XTE J1550-564

3. XTE J : radio
XTE J is a BH candidate at a distance ~5.3 kpc.
A strong and brief (about 1 day) x-ray flare was observed on 20 September 1998
Radio jets with apparent superluminal velocities (2 c) were observed beginning 24 September 1998
1 June 2000
29 January 2002
(Corbel et al. Science 2002/10)

4. XTE J1550-564: Chandra Observations
X-ray jets was discovered.
Separation to the source:
Eastern jet:
~23.4 arcsec (2000/09/11)
~29 arcsec (2002/03/11)
Clear evidence for jet deceleration: jet interaction with surrounding medium
Western jet:
~23 arcsec (2002)
Corbel et al. Science 2002/10: discovery
Wang et al 2003: GRB reverse shock model

5. XTE J1550-564: More Chandra data

6. GRB external/reverse shock model
EXTERNAL SHOCK MODEL FOR THE LARGE-SCALE, RELATIVISTIC X-RAY JETS FROM THE MICROQUASAR XTE J ,X. Y. Wang, Z. G. Dai, and T. Lu, 2003, ApJ
The interaction between the relativistic ejecta and the surrounding medium is analogous to GRB external shock.
A relativistic forward shock expands into the ISM and a reverse shock moves into and heats the original ejecta.

7. Result of eastern jet in Wang et al (2003)
Resulted parameters:
E0=3.6*1044 ergs,θ=50°,
n=1.5*10-4 cm-3, θj=1.5°

8. If we apply the same result to the western jet
It is quite impossible to fit the data, assuming the jet was interacting with the medium from R=0!
Change the kinematic equation to:
And leave all the parameters the same as for the eastern jet

9. The cavity model
A relatively low density region around the black hole.
The emission comes from the interaction between the jet and the dense environment outside.

10. Fitting results of both jets together
Attempt 1:
Ra=Rr=15 (arcsec)
0.4 pc
n(east)=0.015 cm^(-3); n(west)=0.06 cm^(-3)

11. Fitting results of both jets together
Attempt 2:
Ra=14 (arcsec)
Rr=16 (arcsec)
n(east)= cm^(-3); n(west)=0.06 cm^(-3)

12. Fitting motions of two jets separately
Eastern Jet
Ra=16 arcsec, n(east)=0.015cm^(-3)
Western Jet  Rr=18arcsec, n(west)=0.195cm^(-3)

13. Summary of fitting the proper motion data with the external shock model
It can describe the proper motion data consistently for both eastern and western jets.
However, no unique solution is found
The corresponding X-ray flux data fitting is required.

14. External shock model fitting to the eastern jet
 Forward shock model.
synchrotron radiation from medium heated by the forward shock.
Reverse shock model
synchrotron radiation from the adiabatically expanding ejecta heated by the reverse shock.

15. Best fitting result combining proper motion and light curves
Eastern
jet
Western
jet
Eastern
jet
Western
jet
Flux
Proper motion

16. Best fitting result combining proper motion and light curves

17. 2. Large Scale Jets in H

18. X-ray jets from H1743-322 data from Corbel et al. Science 05
Deceleration obviously required

19. X-ray jets from H1743-322 data from Corbel et al. Science 05
Jets in low density medium
Gamma0=1.65
theta=73
E=1E44
n=3E-4

20. X-ray jets from H1743-322 data from Corbel et al. Science 05
Jets in cavity with a radius of 0.12 pc
Gamma0=1.65
theta=73
R=3 arcsec
Approaching
Receding
E=1E44
n=3E-3

21. 3. General Properties of Microquasar Jets

22. ~20 BH BINARIES KNOWN SO FAR IN THE GALAXY:
MBH = M¤; Porb = (0.2-50) days
McClintock & Remillard (2006)
OUTFLOWS AND JETS ARE ALWAYS COUPLED WITH DISK ACCRETION
> 50% OF THE RELEASED
ENERGY IS NOT RADIATED
Analogous large-scale bow-shocks in Cyg X-3 ? & GRS ? ( Marti et al.) (Mirabel & Rodriguez)
(Indicating large-scale cavities)
Gallo, Fender et al. Nature (2005)
Ring diameter ~ 5 pc

23. Jets length scaled by mass
If scaled by central mass to AGN scale, the length of these jets will be translated to ~10Mpc. Heinz (2002)
Heins(2002) estimate the density for GRS :

24. General classification of microquasar jets
There are roughly three dynamical types of jets.
Type
Source name
Jet size
Dynamical property
small
GRS , GRO J ,
Cyg X-3
0-0.05pc
Relativistic jets without decelerating
middle
XTE J ,
H ,
GX 339-4 pc
Relativistic jets with decelerating
large
Cygnus X-1,
Cir X-1, SS433 , 1E
1-30pc
Not moving, diffuse
Ring or Nebula like

25. Summary of environments of microquasars
Direct evidence of very low density cavity
XTE : cavity radius of ~0.4 pc
H : low density region surrounding the source, or cavity radius of ~0.12 pc
Even outside the cavity the ISM density is still much lower than the average ISM density
Cyg X-1: cavity radius of >5 pc; low density dust region up to 260 pc
Hot nebula (low density) region surrounding SS433, GRS and perhaps Cyg X-3
Here we can further argue that the lack of deceleration of many microquasar jets is a signature of cavity surrounding them.

26. Possible interpretations of larger scale cavities surrounding microquasars
Recent supernovae that produced the BHs or NSs
Unlikely, because Cygnus X-1 and GRS most likely never had supernovae (low proper motion and large BH mass), or those had supernovae may have left the SNRs.
Wind of the progenitors of BHs or NSs
Unlikely, because the cavities created by their winds cannot survive very long (<~106 yrs)
Jets of microquasars
Would only work for persistent jet sources
Accretion disk wind
Plausible

27. Winds are common for microquasars and quasars
Young et al, 2007, Science

28. Wind cavity model for microquasars
Depending upon the values of R0 and φ, RT can easily range from ~pc to 100 pc
Then the question is: what controls the values of R0 and φ?

29. Wind properties of microqusars:
Source name
Equip.
M/Msun
rg(km)
wind velocity (km/s)
line width (km/s)
r/rg
V_escape (km/s)
GRO J
Chandra
2*10^4
10.5
10^4.7
1894
10^5.7
189
XMM-
Newton
5*10^3
6145
3072 H
10(?) 15
700±200
1800±400
10^4
4240
GRS
14+/-4 21
1000
10^5
1340
Cir X-1
1.4
2.1
The wind velocity is just comparable to the escape velocity at the referred radius

30. 4. Two Controvertial Sources

31. On the “original” microquasars in the Galactic center region
Transitions from normal hard state to unusual “soft” state (Zhang et al 1996 with GRO/BATSE data)
Very similar to Cygnus X-1?
Persistent pc scale well collimated radio lobes (also from GRS , Marti et al. 1998)
Current large scale jets ruled out for lack of flux decaying
Continuous injection from a stellar mass BH also unlikely
Lack of SS433-like nebula or Cygnus X-1 type bow shock structure
What are these two sources?
Mirabel, Rodriguez, et al, 1992

32. First intermediate mass BHs in the Milky Way?
Radio lobes of 1E & GRS as the Sedov phase of supersonic expansion of jet running into a medium
If ts > 1 year for them and L39=1-10 (ULXs), then E44>30-300
Since E~ MBH and E44=1 for BHXB mQSOs, then MBH > 3x102-3 solar masses
Are 1E & GRS the first IM BHs in the Milky Way?
Analysis X-ray timing, spectrum and radio flux monitoring required to confirm or reject this hypothesis
Nature of the past jet ejection event?
IMBH tidal disruption of a passing star or even its own companion: agrees with lack of companion of in 1E
Or currently the binary systems (with low mass companion) is in their quiescent state.

33. 5. Summary and Conclusions

34. Summary and conclusions/speculations
Jets of microquasars are powerful probes of their surrounding environments
Motion and extension of jets from mQSOs indicate that mQSOs are located in pc scale very low density cavities, compared to the average ISM,

35. Summary and conclusions/speculations
Disk winds are the most plausible source of these cavities
Persistent pc scale radio lobes of 1E & GRS , suggesting that they likely contain intermediate mass BHs
Three classes: microquasars, milliquasars and quasars.

36. Thank you!