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TEO MUÑOZ DARIASOXFORD ASTROPHYSICS
Fast Variability as a Tracer of
Hysteresis and Accretion States in Low Mass X-ray Binaries
Tomaso Belloni Rob Fender Sara Motta
LOW MASS X-RAY BINARY
Quiescence Outburst (and Persistents)
Credit: R. Hynes Credit: R. Hynes
LX ~ 10-8 to -6 LEDD LX ~ 0.01-1 LEDD
LOW MASS X-RAY BINARY
Quiescence Outburst (and Persistents)
Credit: R. Hynes Credit: R. Hynes
LX ~ 10-8 to -6 LEDD LX ~ 0.01-1 LEDD
BLACK HOLE IN OUTBURST: HYSTERESIS
10
100
1000
PCU
2 co
unt
rate
0.1 11
10
rms
(%)
Hardness
Hardness-Intensity (Homan et al. 2001)
Hardness-rms
Belloni 2010
X-ra
y Lu
mino
sity
How hard the spectrum is
Varia
bility
Daily basis monitoring (RXTE)
1 keV 100 keV
hardcomponent
softcomponent
(disc)
1 keV 100 keV
hardcomponent
softcomponent
(disc)
BLACK HOLE IN OUTBURST: HYSTERESIS
10
100
1000
PCU
2 co
unt
rate
0.1 11
10
rms
(%)
Hardness
Hardness-Intensity (Homan et al. 2001)
Hardness-rms
Belloni 2010
X-ra
y Lu
mino
sity
How hard the spectrum is
Varia
bility
Daily basis monitoring (RXTE)
RMS-INTENSITYVARIABILITY-LUMINOSITY
Muñoz-Darias, Motta & Belloni, 2011X
-ray
Lum
inosit
y
Variability Fast variability traces accretion states and hysteresis
DIAGRAM
COMPTONIZATION FRACTION AND VARIABILITY
disc
con
tribu
tion
Varia
bility
How hard the spectrum is
Remillard & McClintock 2006
Fast variability traces Power-law contribution (Comptonization Fraction)
COMPTONIZATION FRACTION AND VARIABILITY
disc
con
tribu
tion
Varia
bility
How hard the spectrum is
Remillard & McClintock 2006
DISTINCTIVE ACCRETION FLOW PROPERTIES
Comptonization component
dominates
Belloni 2010
X-ra
y Lu
mino
sity
Harder and more variable
Thermal componentdominates
DISTINCTIVE ACCRETION FLOW PROPERTIES
Comptonization component
dominates
Belloni 2010
X-ra
y Lu
mino
sity
Harder and more variable
Thermal componentdominates
Compact jet
•X-ray-Radio correlation(Corbel et al., Gallo et al. 2003)
DISTINCTIVE RADIO PROPERTIES
DISTINCTIVE ACCRETION FLOW PROPERTIES
Comptonization component
dominates
Belloni 2010
X-ra
y Lu
mino
sity
Harder and more variable
Thermal componentdominates
Relativistic ejections(e.g. Mirabel & Rodriguez 1994)
Compact jet
•X-ray-Radio correlation(Corbel et al., Gallo et al. 2003)
DISTINCTIVE RADIO PROPERTIES
DISTINCTIVE ACCRETION FLOW PROPERTIES
Comptonization component
dominates
Belloni 2010
X-ra
y Lu
mino
sity
Harder and more variable
Thermal componentdominates
Relativistic ejections(e.g. Mirabel & Rodriguez 1994)
Compact jet
•X-ray-Radio correlation(Corbel et al., Gallo et al. 2003)
Soft State: NO JET(e.g. Russell et al 2011)
DISTINCTIVE RADIO PROPERTIES
NEUTRON STARS LOOK DIFFERENT Low accretion rate (atolls) High accretion rate (Z)
van der Klis 2006 (Hasinger & van der Klis 1989)
•Spectral fitting (more) degenerate. Extra component from the NS surface•Very similar Timing properties than BHs (Wijnands & van der Klis 1999; Belloni, Psaltis & van der Klis 2002).
•Large data base (~15 years of RXTE): 50 systems, 10000+ observations
•PERSISTENT and TRANSIENT sources accreting in the range 0.01-1 LEDD
•Colour and fast variability as a function of the Luminosity
For the interpretation we use results from Lin, Remillard & Homan 2007, 2009
NEUTRON STARS: A GLOBAL STUDYMuñoz-Darias, Fender, Motta & Belloni 2014
Multi-colour disc component Power-Law (Comptonization)
+BB component (NS)
NEUTRON STARS: A GLOBAL STUDYMuñoz-Darias, Fender, Motta & Belloni 2014
Aql X-1
NEUTRON STARS: A GLOBAL STUDYMuñoz-Darias, Fender, Motta & Belloni 2014
Aql X-1
NEUTRON STARS: A GLOBAL STUDYMuñoz-Darias, Fender, Motta & Belloni 2014
Aql X-1
Variability (rms)
Lx
LEdd
1
0.5
0.01
5% 20%
A
INTERMEDIATESOFT HARDCompton dominatedThermal dominated
1-30% LEDD: Hysteresis
Variability (rms)
Lx
LEdd
1
0.5
0.01
5% 20%
A
INTERMEDIATESOFT HARDCompton dominatedThermal dominated
1-30% LEDD: Hysteresis
Loop duration: 1 month -1 yearTransition duration: < 1 week
very similar to BHs
Variability (rms)
Lx
LEdd
1
0.5
0.01
5% 20%
Z
A
FB
INTERMEDIATESOFT
BA
HARDCompton dominatedThermal dominated
HYSTERESIS
BRIGHT SOFT STATE
30-60% LEDD: Bright Soft State
Variability (rms)
Lx
LEdd
1
0.5
0.01
5% 20%
Z
A
HBNB
FB
INTERMEDIATESOFT
BA
HARDCompton dominated
Thermal dominated
HYSTERESIS
BRIGHT SOFT STATE
STATE TRANSITIONS
~LEDD: State transitions
Variability (rms)
Lx
LEdd
1
0.5
0.01
5% 20%
Z
A
HBNB
FB
INTERMEDIATESOFT
BA
HARDCompton dominated
Thermal dominated
HYSTERESIS
BRIGHT SOFT STATE
STATE TRANSITIONS
~LEDD: State transitions
Variability (rms)
Lx
LEdd
1
0.5
0.01
5% 20%
Z
A
HBNB
FB
INTERMEDIATESOFT
BA
HARDCompton dominated
Thermal dominated
HYSTERESIS
BRIGHT SOFT STATE
STATE TRANSITIONS
~LEDD: State transitions
Comptonization Fraction Increases
Variability (rms)
Lx
LEdd
1
0.5
0.01
5% 20%
Z
A
HBNB
FB
INTERMEDIATESOFT
BA
HARDCompton dominated
Thermal dominated
HYSTERESIS
BRIGHT SOFT STATE
STATE TRANSITIONS
~LEDD: State transitions
Comptonization Fraction Increases
The Radio Picture(based in Migliari & Fender 2006)
Variability (rms)
Lx
LEdd
1
0.5
0.01
5% 20%
Z
A
HBNB
FB
INTERMEDIATESOFT
BA
Radio Flares
Radio Flares
HARDRadio loudRadio quiet
HYSTERESIS
BRIGHT SOFT STATE
STATE TRANSITIONS
Variability (rms)
Lx
LEdd
1
0.5
0.01
5% 20%
Z
INTERMEDIATESOFT
BA
Radio Flares
HARD
GRS 1915 +105
Radio Flares Black Hole Transients
Neutron Stars vs. Black Holes
SUMMARY★Large Neutron Star data base accreting at 0.01-1 LEDD
★(Fast) Variability - Luminosity Diagram: common framework for accretion states in NS and BHs
✦ Fast Variability traces the ratio between thermal and Comptonized emission
✦ (Heavily) supported by multi-wavelength observations
✦Hysteresis is commonly observed below ~30 % LEDD
• (very) comparable to that seen in Black holes