Sergei Trushkin , N. Nizhelskij , P. Tsybulev, G. Zhekanis

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Presentation transcript:

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, 12-16 June 2017

RATAN-600 radio telescope Monitoring of mqso: SS433, GRS1915+105, Cyg X-1, Cyg X-3, LSI+61d303, LS4039, V404 Cyg daily at 2-30 GHz (S >5 mJy & 4.7 GHz)

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

Cyg X-3 with eEVN in 2006

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

Cyg X-1 (BH+O8.5V): persistent Weak radio/Xrays correlation (rho=0.30+-0.05) in a hard Xray state

Cyg X-3 (WR-star + BH) First flaring Galactic source (Nature) 1972 – during 44 yr ~20 flares (2006: 6, 2011-2016: 0 !, 2016-2017 : 2) P_orb = 4.8h (IR/Xray) P/Pdot~10^6 years Variable velocity of jets: 0.1-0.9c, 0.5c - as a rule Very clear «classic» synchrotron radio flares + linear polarization 1-10 %. Radio flux drops down before strong flares during: ~1- 6 weeks = ‘hypersoft’ X-ray state

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

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

Spectra of the 2006 May flare

Modelling of a flare based on synchrotron emission evolution

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

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

The daily spectra in the Apr.2017 flare

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+

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

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

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!