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From Quasars to Microquasars S

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From Quasars to Microquasars S From quasars to microquasars jetted AGN stellar binaries 8 9 BH masses: 10 -10 Msun duty cycles: 107 yrs Radio Luminosity BH masses: 10s Msun duty cycles: month-to-yrs 28-32 Lradio~10 erg/s Mass/variability timescales Jet Flavors in Microquasars compact, persistent transient, relativistic large scale jets, hot spots & radio lobes/ radio jets (~10 AU) radio jets (~100s AU) (up to~10s pc) cavities CygX-1 GRS1915+105 1E 140.7-2942Tetarenko+’18 CygX-1 Stirling+’01 Russell+’07 Mirabel & Rodriguez’94 Mirabel & Rodriguez+’92 milli-arcsec arcsec arcmin ->degree accretion & ejection jet power & radio duty cycle relation interaction with the ISM 2 Jets through the BH mass scale Circus X-1 Sell+’10 ljet~0.5 pc jets in 10 Msun BH 2 rg=2MBHG/c ljet/rg ljet~5-50 Mpc jets in 108-9 Msun BH as observing Mpc jets of a radio galaxy moving, varying and changing morphology!(*) (*: jet’s thrust ratio is not the same, Heinz+2013) A Galactic perspective: (micro)quasar large-scale X-ray jets Giulia Migliori (DIFA, INAF-IRA) S.Corbel, J. Tomsick, P. Kaaret, R. Fender, T. Tzioumis, M. Coriat, J. Orosz XTE J1550-564 large scale jets Corbel+’02 Low Mass X-ray Binary: • BH mass: 9.1+/-0.6 Msun (Orosz+’11); • distance: 4.4+/-0.6 kpc; • inclination: 75+/-4 degree; • September 1998: X-ray outburst followed by the detection of relativistic compact jets (vapp~1.7c, Hannikainen+09); Corbel'et'al.'2002' Discovery of large scale (~0.5pc) decelerating jets following the 1998 outburst 5 XTE J1550-564 large scale jets Dynamical Model: the jets propagate unseen in an under-dense ISM cavity and become visible when they impact the cavity’s boundaries (Wang ’03; Hao&Zhang ’09, Steiner+’12). -3 nISM: 1 cm receding western jet approaching eastern jet low density cavity X-ray/Chandra ✓ X-ray follow-up: 8 Chandra observations; ★ Radio follow-up: 24 ATCA observations at 4 frequencies (1.4 GHz, 2.5 GHz, 4.8 GHz, 8.6 GHz). 6 Corbel'et'al.'2002' 18 Migliori G. et al. Jets’ dynamics (quasi) ballistic motion jet deceleration cavity’s eastern boundary eastern jet western jet cavity’s western boundary Fig. 7.— Fit of the radio spectrum of obs17 (upper panel) and obs18 (lower panel). The flux densities are reported in Table 1. first detection beginning of the deceleration phase of the western <vapp,eastjet>=1.0c to 0.1c; jet in 2001 <vapp,westjet>=0.55c to 0.4c. Fig. 8.— Natural weighted ATCA map at 8.6 GHz of the field of XTE J1550-564 on 2001 February 9 and 20. Crosses indicate the position of XTE J1550-564 (center), the eastern (left)andwestern(right)jets.Contoursareplottedat 3, −1 3, 4, 5, 6, 7, 9, 11, 13, 15, 18, 21, 25, 30, 35, 40, 50, 60, 70, 80, 90, 100 times the rms noise level of 0.035 mJy beam− . The synthesize beam (lower right corner) is 12.8 10.5 arcsec2. ⇥ Western Jet: X-ray morphology Migliori+2017 XTE J1550-564 western jet March 11 2002 ~23’’/0.5pc June 19 2002 Spatially resolved, evolving X-ray morphology Sept 24 2002 June 28 2003 0.3-8.0 keV 0ct. 23 2003 Jet–Environment Interactions as Diagnostics of Jet Physics 2.1.1 Jet Stopping For jet material to be affected meaningfully by its interaction with the environment, a sig- nificant fraction of its momentum must be transferred to environmental gas. Before this happens, the jet simply bores through the environment unhindered, creating a strong bow shock ahead of it but not slowing down. Let us first consider a magnetized jet fluid that is kept from mixing with the gas it is interacting with by flux freezing. In this case, the two fluids (jet and ISM) will occupy separate volumes. This approximation is appropriate for the discussion of lobe/cocoon formation, but jet propagation itself may be affected by mass loading (see Sect. 2.2). The propagation of the leading edge of the jet, henceforth referred to as the jet “head”, is governed by ram pressure balance in the bow shock. Roughly speaking, the momentum 2 2 flux of the jet into the bow shock is p , P/(πl θ c),whereP is the power and l is ram jet ≈ jet the length of the jet. The ram pressure of the ISM that must balance this momentum flux is 2 p , ρ v .Thesenon-relativisticexpressionsassumethattheheadmovesslowly ram ism ≈ ISM head compared to the jet, i.e., that the jet is effectively slowed down by the ISM; before that, the jet deposits relativily little plasma along its path which slowly expands sideways into a cocoon that shrouds the jet (see cartoon in the left panel of Fig. 1). The propagation velocity of the head is then simply P 1 vhead (1) ∼ !πρISMc lθjet and the condition that the jet is stopped by the ISM is simply that vhead c.Thejethead 1/2 ≪ then propagates with a velocity v t − . The stopping length for a relativistic jet can head ∝ then be defined as P l (2) Westerns Jet morphology3 2 ≡ !πρISMc θjet helical X-ray morphology? 0ct. 23 2003 X-rays ? 25 24.5 Radio 24 23.5 Heinz+’13 23 Fig. 1 Left:22.5 Cartoon of the early momentum-driven phase of jet head propagation (production of a narrow Projected ang. separation (arcsec) cocoon) at22 close to the jet velocity; Right: cartoon of the “dentist drill effect”, which explains the observed aspect ratios of lobes (close to unity) by dynamical instabilities or precession spreading the jet thrust effec- tively over21.5 a much larger are than the jet cross section and leading to an earlier onset of the energy drive phase of lobe evolution21 1200 1300 1400 1500 1600 1700 1800 1900 Days from flare [MJD-51077.8] projected ang. separation (arcsec) projected 407 Reprinted from the journal 1616 Migliori G. et al. 16 Migliori G. et al. 1616 Migliori Migliori G. G. et et al. al. Fig.Fig. 3.— 3.— ComparisonComparison between the X-ray morphologies of the eastern and western jets: in the left panel, the smoothed Chandra ACIS-S imageimage of of the the eastern eastern jet observed September 11th 2000 and on the right panel the western jet observed on January 28th, 2003. Fig. 3.— Comparison between the X-ray morphologies of the eastern and western jets: in the left panel, the smoothed Chandra ACIS-S image of the eastern jet observed September 11th 2000 and on the right panel the western jet observed on January 28th, 2003. 6060 ObsID 3448 50 March 11 2002 60 ObsID 3448 50 March 11 2002 Fig.Fig. 3.— 3.— ComparisonComparison50 between the the X-ray X-ray morphologies morphologies of of the the eastern eastern and and western western jets: jets: in in the the left left panel, panel, the the smoothed smoothedChandraChandraACIS-SACIS-S 4040 imageimage of of the the eastern eastern jet observed September September 11th 11th 2000 2000 and and on on the the right right panel panel the the western western jet jet observed observed on on January January 28th, 28th, 2003. 2003. 40 3030 30 Counts/bin Counts/bin 2020 Counts/bin 20 1010 Western Jet: X-ray profiles 10 00 0 ObsID 3672 6060 ObsIDObsID 34483448 3807 tail peak ObsID 3672 ObsID 3807 3030 Jun 19 2002 MarchObsIDSept 24 11113672 2002 20022002 503050 Jun 19 2002 Sept 24 2002 4040 2020 302030 • progressive deceleration of the main peak Counts/bin Counts/bin Counts/bin Counts/bin 2020 10 Counts/bin 10 10 (vapp~0.06c); 1010 • formation of an apparently 00 0 0 receding tail (vapp~-0.10c); ObsIDObsID 3672 5190 vapp~-0.10c vapp~0.06c ObsIDObsID 3807 3807 ObsID 4368 ObsIDObsIDObsID 43683672 5190 ObsID 5190 15 30 JunOct 19 23 2002 2003 SeptSept 24 24 2002 2002 15 Jan 28 2003 3015 JanJunOct 2819 23 2003 2002 2003 Oct 23 2003 1010 201020 Counts/bin Counts/bin Counts/bin Counts/bin 55 Counts/bin 10105 00 0 10 15 20 25 10 15 15 20 20 25 25 10 15 20 25 ObsID 4368 ObsIDObsID 5190 5190 Displacement along the jet axis (arcsec)15 DisplacementObsID 4368 alongalong thethe jetjet axis axis (arcsec) (arcsec) Displacement along the jet axis (arcsec) 15 Jan 2828 20032003 10 OctOct 23 23 2003 2003 Fig.Fig. 4.— 4.— LongitudinalLongitudinal profiles of the western X-ray jet in theFig. 0.3-8 4.— keVLongitudinal10 energy range profiles for the of five the westernChandra X-raydetections, jet in the using 0.3-8 a bin keV size energy range for the five Chandra detections, using a bin size of 0.25 .ThedashedredlineistheprofileofXTEJ1550-564atthesameepoch,whichhasbeenshiftedandre-normalizedtomatchthe10 ofof 0.25 0.250000.ThedashedredlineistheprofileofXTEJ1550-564atthesameepoch,whichhasbeenshiftedandre-normalizedtomatchthe.ThedashedredlineistheprofileofXTEJ1550-564atthesameepoch,whichhasbeenshiftedandre-normalizedtomatchthe00 westernwestern X-ray X-ray jet jet peak. The vertical solid orange line and dashedwestern cyan X-ray line mark jet peak. the positionsThe vertical of the solid peak orange and line of tail, and respectively, dashed cyan atline the mark the positions of the peak and of tail, respectively, at the epoch of the first detection. epoch of the first detection. epoch of the first detection. Counts/bin Counts/bin 5 0 10 15 15 20 20 25 25 1010 15 15 20 20 25 25 Displacement alongalong thethe jetjet axis axis (arcsec) (arcsec) DisplacementDisplacement along along the the jet jet axis axis (arcsec) (arcsec) Fig. 4.— Longitudinal profiles of the western X-ray jet in the 0.3-8 keV energy range for the five Chandra detections, using a bin size Fig.
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