40 years of microquasars
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40 Years of Microquasars. Ralph Spencer Jodrell Bank Observatory School of Physics and Astronomy University of Manchester Ierapetra June 2014. Radio Emitting X-ray binaries (REXRB). 1968: discovery of radio emission from Sco X-1 (Andrew and Purton 1968) - PowerPoint PPT PresentationTRANSCRIPT
40 Years of MicroquasarsRalph Spencer
Jodrell Bank Observatory
School of Physics and Astronomy
University of Manchester
Ierapetra June 2014
Radio Emitting X-ray binaries (REXRB)
• 1968: discovery of radio emission from Sco X-1 (Andrew and Purton 1968)
• 1971: radio emission from X-ray binaries detected by Westerbork Array and GB Interferometer at ~ mJy levels (Braes and Miley 1971, Hjellming and Wade1971)
April 1971 John applies to Jodrell Bank for a place on the MSc course, joins in Sept 1971
Cygnus X-3 Goes Bang!
• Jan 1972: Detection of Cyg X-3 with GBI (Hjellming and Wade 1972) 0.1-0.3 Jy at 11 and 4 cm
• September 1972: –outburst on Cyg X-3 reaching > 20 Jy. Many observatories took part.
Gregoryet al 1972
Oct 1972 John starts PhD
Nova Monoceros 1975 A0620-00
• Rapid increase in X-ray emission reported by Leicester group (Ariel)
• Triggered radio obs at JBO (Davis et al. 1975)
• Kuulkers et al. 1999 revisited data
Oct 1975 John completes PhD
X-Ray Binaries
• ~300 X-ray emitting binary stars (XRBS) found in our own Milky Way galaxy, detected by X-ray satellites at ~1-10 kev (van Paradis 1995, Liu et al. 2000, 2001 catalogues)
• High Mass ~ 10 Msun• Low Mass ~ 1 Msun• .All powered by accretion onto a
compact object (neutron star or black hole).
• Roche Lobe overflow or wind?
• ~20 % have been found to have radio emission
Low Mass XRBs
• Companions around 1 Msun, with a neutron star or BHC secondary
• Neutron star binaries– Type I X-ray bursts– Soft X-ray emission (few kev
brightness temp.)– Short orbital period of < 12 hours
• BHCs : no Type 1 bursts, hard X-rays, transients
• X-ray colour-colour diagram useful diagnostic
• Quasi period oscillations in X-ray intensity
X-ray bursts from Circ X-1
High Mass X-ray binaries: HMXRB
• Indicators:– O, B, Be or Wolf-Rayet stellar spectrum– Strong flaring and absorption variability on a timescale of
minutes– Transient outbursts– Hard 1-10 kev spectrum with a power law index at higher
energies of ~0-1
• Periods range from 4.8 hrs (Cygnus X-3) to 187 days (Hen 715)
• N- star or BHC compact secondaries• Generally wind fed.
The discovery of radio jets• SS433 in 1979• Moving optical lines suggest
precessing jets at 0.26 c with a period of 162.5 days (Abell and Margon 1979)
• Cambridge 5km observations of compact objects < 1 arcsec, Ryle et al 1978
• Interesting X-ray behaviour – Dennis Walsh suggested we observed it at JB
• Discovered extension in PA ~100 deg – jets? (Spencer 1979)
Margon and Anderson 1989
MkI-Defford 74-cm 1979 visibility curve
SS433 radio jets
• Hjellming and Johnston 1981 VLA results
• MERLIN 5 GHz Jowett PhD 1999 Stirling et al 2002
Radio Emission
• ~50 sources have radio emission
• Most radio emitters are Low Mass XRBs with BHC
I. Brown 2006 PhD Thesis
Microquasars
• Term first used by Martin Elvis 1984 “Microquasars and the X-ray Background” (Weak AGN)
• First used in the context of X-ray binaries: Geldzahler, Fomalont and Cohen 1984, “Sco X-1 The Microquasar”
• Now thought to be unrelated background sources
VLA 4.8 GHZ
Microquasars
• Why microquasar?– Radio jets– Relativistic velocities– Powered by accretion– 106 times closer
• Mirabel et al. 1992
1E1740.7-2942
Year
No. of papers
Number of papers with ‘microquasar’ in the title or abstract
Fundamental plane of black holes
• Radio/X-ray correlation found in XRBS can be extended to AGN by the inclusion of a mass term.
• Correlation very tight for LLAGN
Merloni, Heinz et al. 2003, Falcke, Koerding, Markoff 2004,Koerding et al. 2006
Some Individual Objects
• Cygnus X-3
• SS433
• Cygnus X-1
• GRS1915+105
• Cygnus X-2
Cygnus X-3• Greenbank Interferometer
Waltman et al 1995• 1983 MERLIN 5 GHz –
model fitting N-S double showed expansion at 0.3 c Johnston et al. 1983
• Infra red and radio flares Fender, Bell-Burnell, Ogley et al. 1994,1995, 1996, 2001
• 10 Msun WR star and 2.4 Msun BH Zdziarski et al. 2013
Fender et al 1996
7 103 7.5 10
3 8 103 8.5 10
3 9 103
0
5
10
15
20
Cygnus X-3 Green Bank Interferometer S-band data
MJD
Flu
x de
nsity
Jy
Si
Ti
Relationship to X-rays
• Ryle telescope and RXTE (Pooley)
• Quenching of radio before outburst
• Hardening of X-rays
Radio/Hard X and γ-ray Quenching
• Corbel et al 2012- hard X-rays and γ-rays suppressed just before a major flare
Cygnus X-3 Images• Mioduszewski et al
2001• 15 GHz VLBA• Evolving N-S jet
• 2-sided N-S structure also seen in 5 GHz VLA images (AM).
• Expansion at ~0.5 c (Marti et al 2002)
www.aoc.nrao.edu/~amiodusz/NB 90 deg rotation
• EVN at 5 GHZ
1st e-VLBI observations at 5 GHz
Complex changes in the core- more to do!
SS433• Another WR star and compact companion• 24 Msun WR and 16 Msun BH• 162.5 d precession period• 13 d binary period• Proper motion if at 0.26 c gives distance
of 4.6 kpc
VLA 5 GHz Blundell and Bowler 2004
The Ruff – Equatorial emission
MERLIN+EVN 18 cm June 1998Stirling et al 2004
VLA, MERLIN VLBA 6 cm March 1998 Blundell et al 2001
Present in ~25% of images, no obvious relationship to jet knots and PA Spencer 2006
W50 and SS433 – the jets slow down?
Velocity of filaments in the ears < 0.04c Goodhall et al. 2011
Fit to ephemeris including nutation suggests deceleration at 0.04c/yr Stirling et al. 2004More observations needed!
Cygnus X-1 – a radio jet in a persistent black hole XRB
VLBA 8.4 GHzAugust 1998-discovery of jet in Cyg X-1 on ~15 mas scale(Stirling et al 2001)
VLBA 15 GHzShowing compact jet~3 mas long
(in low/hard X-ray state)
Also a weak compact jet in the soft state (Rushton et al 2012
15 Msun Black hole +19 Msun O star companion
Optical line emission
White: continuum
Red: Ha
Green: O[III](Russell, Fender et al. 2007)
1.4 GHz Westerbork imageGallo et al 2005
Cyg X-1 Nebula
GRS1915+10510 Msun BH +2 Msun companion
Superluminal expansionMirabel & Rodriguez 1994
Fender et al 1999 0.9c, 11kpc
Radio emission in plateau states (Migliari & Belloni 2003 Xray state χ)
Rushton et al 2010
Typically 1-3 months
0.2-0.4 Jy Flaresand 0.05-0.1 Jyplateaus
Flares decay in 3-4 days, followed by a suppressed flux before recoveringOccurs during plateau state as well as at beginning or end
GRS1915 – log normal flux distribution
Compare with power law for Cyg X-3
A Radio Jet in the Cyg X-2 Neutron Star X-ray BinarySpencer et al. MNRAS 435L, 48, 2013
Horizontal Branch (HB) -jet launched here
Normal Branch (NB) -mass accretion rate increases
Flaring Branch (FB) -unstable nuclear burningon the neutron star
Z-track on hardness-intensity diagram
6 cm EVN 22 Feb 2013
23 Feb 2013
Hard Apex - Jet ejected
SWIFT hardness – intensity diag. Source in HB
Jet ejected
X-ray, UV and radio vs time
1.7 Msun neutron starand a 0.6 Msun companion
To summarise so far
• Radio emission can be relatively steady or in flares
• Flaring often associated with the formation of relativistic jets on > 100 mas scales
• Steady mas (10’s au) jets can also occur• At least one object shows precessing jets• Strong association with X-ray emission: jet-disk
coupling• Changing accretion conditions have a causal
relationship with the radio jets
q- diagram or Turtles Head
Gallo, Fender et al 2005
O Starcompanion
wind
disk
0.3c
>0.3c
HardX-rays
Radio
ReflectedX-rays
Magnetic loops
Hot e+- plasma lifted by unstable loops formed by magnetic rotational instability
Miller et al. 2012 model for CygX-1
GRS1915 evolutionHigh Soft X-ray stateNo radio
Low Hard X-rays
Weak inner jet Stronger inner jet
Flaring outburst withrelativistic ejection
Inner disk instability leads tomajor ejection
Dominated by radiation form disk
Hot corona and jet formed- Blandford Znajek 1977 mechanism
Plateau state
X-ray Intensity
Hardness
Future• Do all galactic XRBs have radio emission at some level?
Need much better sensitivity to bring the 20% detections up!
• Microquasars in other galaxies e.g. M31 (Middleton et al 2013), IC10 (Bernard et al 2008), NGC300 (Crowther et al. 2010) – should be lots, especially in star forming galaxies.
• E.g. an equivalent 10 Jy flare in IC10 from a CygX-3 type object would give 240 microJy on Earth – can be studied with JVLA and e-MERLIN, but not quiescent emission
• Relationship to ULXs – extending the fundamental plane• Need the SKA!!