1. The jets of the microquasars during giant radio flares and quiet state (long-term radio monitoring)
Sergei Trushkin , N. Nizhelskij , P. Tsybulev,
G. Zhekanis
Polarised emission from astrophysical jets Ierapetra, June 2017

2. RATAN-600 radio telescope
Monitoring of mqso: SS433, GRS , Cyg X-1,
Cyg X-3, LSI+61d303, LS4039, V404 Cyg
daily at 2-30 GHz (S >5 mJy & 4.7 GHz)

3. Cyg X-1
Stirling et al.‘01
GRS
Mirabel et al. ‘94
SS433
Blundell et al. 2004 1E
Mirabel et al. al ‘99

4. Cyg X-3 with eEVN in 2006

5. SS433 (BH+A*): no clear evidence of disk-jets coupling
Weak modulation with the orbit = 13.1d

6. Cyg X-1 (BH+O8.5V): persistent
Weak radio/Xrays correlation (rho= ) in a hard Xray state

7. Cyg X-3 (WR-star + BH)
First flaring Galactic source (Nature) 1972 – during 44 yr ~20 flares (2006: 6, : 0 !, : 2)
P_orb = 4.8h (IR/Xray) P/Pdot~10^6 years
Variable velocity of jets: c, 0.5c - as a rule
Very clear «classic» synchrotron radio flares + linear polarization %.
Radio flux drops down before strong flares during: ~1- 6 weeks = ‘hypersoft’ X-ray state

8. X-ray spectra of the Cyg X-3 states
Blue – quite state; red -- pre-flare; green – flare!

9. Cyg X-3 light curves RATAN+XTE in 2005-2006

10. Spectra of the 2006 May flare

11. Modelling of a flare based on synchrotron emission evolution

12. Cyg X-3: 2016-17 RATAN+Swift/BAT
USS!

13. Giant flares: RATAN multi-frequency data
SMA+ IRAM + EMI+ EMERLIN+ RATAN

14. The daily spectra in the Apr.2017 flare

15. Be star + NS or BH Г-ray/TeV + X-ray binary: P_orb=26
Be star + NS or BH Г-ray/TeV + X-ray binary: P_orb=26.5d & super-orb P2=1667d, detected by B.Gregory
LSI+61d303
Orbital VLBA data by Dhawan+

16. LSI+61d303: 1300-days light curves
Mysterious dependence of radio flares on super-orbital period =4.6 yr

17. V404 Cyg: Wake-up after 26 years sleeping!
Jets on the start!

18. Radio photometry of mqso.
Light curves – best tracers of the jets activity, but LP/CP required!
Very close relation: X-ray & radio (dm-mm) emission (X-ray states <=> internal shocks) (see HIDs, fundamental plane).
‘Multi-frequency-ness’ gives us the spectral data in optically thick & thin regime, where an initial acceleration of electrons occurs.
We collaborated with teams of AGILE, MAGIC, Fermi, LOFAR, SMA, EMI, Swift, SRT64m, ATCA, EVN, nu-Star: 16 papers for last 8 yr + (3 prepared) + tens of ATels .
We can predict giant flares (at least in Cyg X-3 :))
ADVENTURE CONTINUES!