Jets from X-ray binaries
Jets from X-ray binaries
Jets from X-ray binaries
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<strong>Jets</strong> <strong>from</strong> X-<strong>ray</strong> <strong>binaries</strong><br />
Simone Migliari<br />
ESAC
“<strong>Jets</strong> are possibly the most spectacular and powerful<br />
phenomena in astrophysics; they are ubiquitous in the universe,<br />
common to a number of different accreting systems”
“<strong>Jets</strong> are possibly the most spectacular and powerful<br />
phenomena in astrophysics; they are ubiquitous in the universe,<br />
common to a number of different accreting systems”
spectacular
Stirling et al 2001<br />
1 arcmin (2 light years)<br />
spectacular<br />
Gallo et al. 2005<br />
F (<br />
!<br />
Miller-Jones, Migliari et al. 2007
Powerful<br />
Special relativity in action<br />
Mirabel & Rodriguez 1992 Biretta et al. 1999
powerful
Gizani et al. 2002<br />
Powerful<br />
Gallo et al. 2005<br />
1 arcmin (2 light years)<br />
CygX-1<br />
F (Jy)<br />
!<br />
>20% Accreting Power<br />
Hercules A
AGN<br />
X-<strong>ray</strong> <strong>binaries</strong><br />
WD <strong>binaries</strong><br />
YSOs<br />
Ubiquitous
“<strong>Jets</strong> are possibly the most spectacular and powerful<br />
phenomena in astrophysics; they are ubiquitous in the universe,<br />
common to a number of different accreting systems”<br />
“However, the mechanism(s) of jet production is still poorly<br />
understood”
Meier et al. 2001
Which<br />
parameters<br />
are involved in<br />
jet formation?<br />
⋅<br />
M<br />
Accreting<br />
Object
M87: 1 yr<br />
Walker et al.
X-<strong>ray</strong> binary: 42 days
outburst: accretion disc variability<br />
BH X-<strong>ray</strong> binary<br />
Migliari et al. 2007
X-<strong>ray</strong> binary<br />
Radio<br />
opt<br />
IR<br />
IR<br />
opt<br />
Υ-<strong>ray</strong>s<br />
X-<strong>ray</strong>s<br />
opt<br />
IR
BH X-<strong>ray</strong> <strong>binaries</strong>
transient<br />
Two types of jets<br />
Fender 2000
Two types of jets<br />
transient<br />
compact<br />
Starling et al. ‘01<br />
Fender 2000
Two types of jets<br />
transient<br />
compact<br />
Starling et al. ‘01<br />
Flux<br />
Radio IR ?<br />
Fender 2000
X-<strong>ray</strong> Intensity<br />
few 100s<br />
accretion disc variability<br />
few months<br />
Time
X-<strong>ray</strong> Intensity<br />
few 100s<br />
accretion disc variability<br />
few months<br />
Time<br />
X-<strong>ray</strong> Intensity<br />
full cycle of an outburst<br />
X-<strong>ray</strong> hardness
X-<strong>ray</strong> Intensity<br />
few 100s<br />
accretion disc variability<br />
few months<br />
Time<br />
X-<strong>ray</strong> Intensity<br />
full cycle of an outburst<br />
X-<strong>ray</strong> hardness
X-<strong>ray</strong> Intensity<br />
few 100s<br />
accretion disc variability<br />
few months<br />
Time<br />
X-<strong>ray</strong> Intensity<br />
full cycle of an outburst<br />
X-<strong>ray</strong> hardness
X-<strong>ray</strong> Intensity<br />
few 100s<br />
Migliari et al. 2007<br />
few months<br />
Time<br />
X-<strong>ray</strong> Intensity<br />
X-<strong>ray</strong> hardness<br />
Homan et al. 200
X-<strong>ray</strong> Intensity<br />
few 100s<br />
few months<br />
X-<strong>ray</strong> Intensity<br />
Time<br />
X-<strong>ray</strong> hardness<br />
Gallo et al. 2002
X-<strong>ray</strong> Intensity<br />
few 100s<br />
few months<br />
X-<strong>ray</strong> Intensity<br />
Time<br />
X-<strong>ray</strong> hardness<br />
Gallo et al. 2002
X-<strong>ray</strong> Intensity<br />
few 100s<br />
few months<br />
X-<strong>ray</strong> Intensity<br />
Time<br />
X-<strong>ray</strong> hardness<br />
Gallo et al. 2002
Miller-Jones et al.: JACPOT collaboration<br />
http://www.astro.virginia.edu/xrb_jets/
compact<br />
Miller-Jones et al.: JACPOT collaboration<br />
http://www.astro.virginia.edu/xrb_jets/
transient<br />
compact<br />
Miller-Jones et al.: JACPOT collaboration<br />
http://www.astro.virginia.edu/xrb_jets/
jet line<br />
transient<br />
compact<br />
Miller-Jones et al.: JACPOT collaboration<br />
http://www.astro.virginia.edu/xrb_jets/
proposed Unified Scenario<br />
Fender et al. 2004<br />
Text
proposed Unified Scenario<br />
Fender et al. 2004<br />
Text<br />
- does the disk radius vary?<br />
- correlation slope?<br />
- Lorentz factor?<br />
- does the jet speed increases as increases potential well.<br />
- is there a jet line? is it vertical?
proposed Unified Scenario<br />
Fender et al. 2004<br />
Text<br />
- does the disk radius vary?<br />
- correlation slope?<br />
- Lorentz factor?<br />
- does the jet speed increases as increases potential well.<br />
- is there a jet line? is it vertical?<br />
- is the ejection, an ejection of the corona?<br />
- does the core jet quench? when exactly during the outburst?<br />
- at what hardness/the core jet reforms back?<br />
- do subsequent ejecta vary speed?<br />
- and what about QPOs and jets?<br />
- ...
AGN<br />
X-<strong>ray</strong> <strong>binaries</strong><br />
WD <strong>binaries</strong><br />
YSOs
stellar-mass/super-massive BH connection<br />
Merloni et al. 2003<br />
The search for the grand unification scheme
NS X-<strong>ray</strong> <strong>binaries</strong>
Which<br />
parameters<br />
are involved in<br />
jet formation?<br />
⋅<br />
M<br />
Spin<br />
Magn. field
Nomenclature: NS classes<br />
Atoll sources<br />
Z sources<br />
HB<br />
.<br />
m<br />
IS<br />
??<br />
?? ṁ<br />
NB<br />
LB<br />
UB<br />
FB<br />
~0.01 ~0.1<br />
’Hard’ atoll sources ’Soft’ atoll sources<br />
Luminosity / Eddington<br />
’Z’ sources<br />
van der Klis 2006<br />
Migliari & Fender 2006
X-<strong>ray</strong> binary<br />
population<br />
sample: 264 XRBs (Liu et al. 01/06)
X-<strong>ray</strong> binary<br />
population<br />
sample: 264 XRBs (Liu et al. 01/06)<br />
Atolls<br />
143
X-<strong>ray</strong> binary<br />
population<br />
sample: 264 XRBs (Liu et al. 01/06)<br />
Atolls<br />
X-<strong>ray</strong> pulsars<br />
143<br />
80
X-<strong>ray</strong> binary<br />
population<br />
sample: 264 XRBs (Liu et al. 01/06)<br />
Atolls<br />
X-<strong>ray</strong> pulsars<br />
AMXPs<br />
143 80<br />
13
X-<strong>ray</strong> binary<br />
population<br />
sample: 264 XRBs (Liu et al. 01/06)<br />
Atolls<br />
X-<strong>ray</strong> pulsars<br />
Z<br />
8<br />
AMXPs<br />
13<br />
143<br />
80
X-<strong>ray</strong> binary<br />
population<br />
sample: 264 XRBs (Liu et al. 01/06)<br />
Atolls<br />
X-<strong>ray</strong> pulsars<br />
Z<br />
8<br />
AMXPs<br />
13<br />
Black<br />
Holes<br />
143 80<br />
20
X-<strong>ray</strong> binary<br />
population<br />
Radio detection/jet<br />
sample: 264 XRBs (Liu et al. 01/06)<br />
Atolls<br />
X-<strong>ray</strong> pulsars<br />
Z<br />
8<br />
Black<br />
AMXPs<br />
Holes<br />
143<br />
80<br />
13<br />
20
Nomenclature: NS classes<br />
Atoll sources<br />
Z sources<br />
HB<br />
.<br />
m<br />
IS<br />
??<br />
??<br />
.<br />
m<br />
NB<br />
LB<br />
UB<br />
FB<br />
~0.01 ~0.1<br />
’Hard’ atoll sources ’Soft’ atoll sources<br />
Luminosity / Eddington<br />
’Z’ sources<br />
van der Klis 2006<br />
Migliari & Fender 2006
XTE J1701-462: the Rosetta Stone<br />
Atoll Z-Sco Z-Cyg<br />
Homan et al. 2010
Z-Cyg<br />
Z-Sco<br />
X-<strong>ray</strong> intensity<br />
Atoll-GX<br />
Atoll-S<br />
⋅M<br />
Atoll-H<br />
Migliari<br />
Hard X-<strong>ray</strong> color
Z-Cyg<br />
GX5-1<br />
4U1701-462<br />
CygX-2<br />
CygX-2<br />
Z-Sco<br />
4U1701-462<br />
ScoX-1<br />
GX17+2<br />
X-<strong>ray</strong> intensity<br />
⋅M<br />
Atoll-GX<br />
Atoll-S<br />
GX9+9...<br />
MXB1730-33<br />
4U1820-30<br />
SerX-1<br />
AqlX-1<br />
Migliari<br />
Atoll-H<br />
AqlX-1<br />
4U1728-34<br />
4U0614+091<br />
Hard X-<strong>ray</strong> color
Atoll-H<br />
0.2<br />
Flux density (mJy)<br />
4U0614+09<br />
0.1<br />
4U1728-34<br />
5<br />
Frequency (GHz)<br />
10<br />
Migliari et al.<br />
2003,2006,2010
Atoll-H-S transitions<br />
Miller-Jones et al. 2010: JACPOT collaboration<br />
http://www.astro.virginia.edu/xrb_jets/
Atoll-GX<br />
quenching at ~10% Eddington?<br />
Radio Luminosity<br />
BHs<br />
NSs<br />
AMXPs<br />
Atolls hard<br />
L 8.5 GHz<br />
(x10 26 erg/s)<br />
100 1000 10 4<br />
Atolls<br />
soft<br />
Z<br />
0.1 1 10 100 1000<br />
L 2!10 keV<br />
(x10 36 erg/s)<br />
10% Eddington<br />
X-<strong>ray</strong> Luminosity<br />
Migliari & Fender 2006<br />
Migliari et al. in prep.
Atoll-GX<br />
quenching at ~10% Eddington?<br />
Radio Luminosity<br />
BHs<br />
NSs<br />
AMXPs<br />
Atolls hard<br />
L 8.5 GHz<br />
(x10 26 erg/s)<br />
100 1000 10 4<br />
Atolls<br />
soft<br />
Z<br />
0.1 1 10 100 1000<br />
L 2!10 keV<br />
(x10 36 erg/s)<br />
10% Eddington<br />
X-<strong>ray</strong> Luminosity<br />
Migliari & Fender 2006<br />
Migliari et al. in prep.
Atoll-GX<br />
quenching at ~10% Eddington?<br />
Radio Luminosity<br />
BHs<br />
NSs<br />
AMXPs<br />
Atolls hard<br />
L 8.5 GHz<br />
(x10 26 erg/s)<br />
100 1000 10 4<br />
Atolls<br />
soft<br />
Z<br />
GX3+1<br />
GX9+9<br />
0.1 1 10 100 1000<br />
L 2!10 keV<br />
(x10 36 erg/s)<br />
10% Eddington<br />
X-<strong>ray</strong> Luminosity<br />
Migliari & Fender 2006<br />
Migliari et al. in prep.
Atolls<br />
Z-Cyg<br />
Detection:<br />
all X-<strong>ray</strong> states<br />
Z-Sco<br />
Brightest:<br />
transitions<br />
X-<strong>ray</strong> intensity<br />
⋅M<br />
Atoll-GX<br />
Atoll-S<br />
Type of Jet:<br />
always compact<br />
Quenching:<br />
possibly ~10% Edd<br />
Atoll-H<br />
Migliari<br />
Hard X-<strong>ray</strong> color
Z<br />
GX17+2<br />
Migliari et al. 2007<br />
GX17+2<br />
CygX-2<br />
Hjellming et al. 1990<br />
Jy
Z<br />
GX17+2<br />
Migliari et al. 2007<br />
GX17+2<br />
CygX-2<br />
Jy<br />
0 2×10 !4 4×10 !4<br />
jet off: FB<br />
jet on: NB<br />
Hjellming et al. 1990<br />
days
Z<br />
Fomalont et al. 2001<br />
ScoX-1<br />
CygX-2<br />
Hjellming et al. 1990<br />
GX340+0
Z-Cyg<br />
Z-Sco<br />
X-<strong>ray</strong> intensity<br />
Atoll-GX<br />
Atoll-S<br />
⋅M<br />
Atoll-H<br />
Migliari<br />
Hard X-<strong>ray</strong> color
Z-Cyg<br />
Z-Sco<br />
Z<br />
Transient<br />
jet<br />
&<br />
X-<strong>ray</strong> intensity<br />
Atoll-GX<br />
Atoll-S<br />
Compact<br />
jet<br />
Atoll~10%Edd<br />
Quenching<br />
⋅M<br />
Atoll-H<br />
Atoll<br />
Compact<br />
jet<br />
Migliari<br />
Hard X-<strong>ray</strong> color
Role of the NS magnetic field?
X-<strong>ray</strong> pulsars<br />
B> 10 12 G<br />
L 8.5 GHz<br />
(x10 26 erg/s)<br />
10 100 1000 10 4<br />
NO quantitative proof yet<br />
0.01 0.1 1 10 100 1000<br />
L 2!10 keV<br />
(x10 36 erg/s)<br />
Migliari 2010
X-<strong>ray</strong> pulsars<br />
B> 10 12 G<br />
L 8.5 GHz<br />
(x10 26 erg/s)<br />
10 100 1000 10 4<br />
NO quantitative proof yet<br />
0.01 0.1 1 10 100 1000<br />
L 2!10 keV<br />
(x10 36 erg/s)<br />
Migliari 2010
Role of the NS Spin?
Role of the NS Spin?
Role of the NS Spin?
Role of the NS Spin?
spin vs jet power<br />
L R<br />
/L X<br />
!<br />
normalization (!=1.4)<br />
10 100 1000 10 4<br />
200 500<br />
Spin (Hz)<br />
Migliari 2010<br />
Migliari, Miller-Jones & Russell in prep.
Models for jets in NSs: what are we looking for?<br />
_when liberated, the average jet power is correlated with average Mdot<br />
_within a sub-class, the jet activity depends on a second parameter which regulates<br />
the output channel (jet, wind?) and is related to state transitions: instantaneous<br />
Mdot? disk instabilities? ...?<br />
_transient jets observed only > ~10% Eddington<br />
_parameters of the NS involved? magn. field/spin? NO quantitative proof yet.<br />
hints: 1) high mag field - quenched jet?<br />
2) higher spin - stronger jet?<br />
(growing)<br />
(weak)
AGN<br />
X-<strong>ray</strong> <strong>binaries</strong><br />
WD <strong>binaries</strong><br />
YSOs
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