x-ray time lags modeling with thermal and bulk comptonization
TRANSCRIPT
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X-Ray Time Lags with Thermal and Bulk Comptonization Modeling
Juan C Luna
George Mason University
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Introduction X-Ray Astronomy Models Spectral States Time Lags Our Model
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Variable Sources
AGN (Active Galactic Nucleus) Neutron Star / White Dwarf Black Hole Candidate
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Compact Objects
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Neutron StarAfter a supernova explosion, the central region of the star collapses combining protons and electrons and forcing them to produce neutrons. A pulsar is a rotating neutron star.
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Telescopes
Rossi XTEXMM NewtonChandra
Software: FTOOLS CIAO 3.1 XSPEC Sherpa Xronos
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Xspec Output:Spectrum and Light Curve
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Accretion Disc
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Accretion Models Standard Disk
(Shakura & Sunyaev 1973)optically thick, geometrically thin, energy produced by viscous heating emitted locally as blackbody radiation (“cool disk”)
Two temperature Disks (Shapiro, Lightman & Eardley 1976)
The inner region of the disk is hot geometrically thicker than the cool disk, but optically thin to absorption (gas pressure is dominant “hot disk”)
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Advection Dominated Accretion FlowAccretion flow in which as the gas spirals in and gets very hot, it does not radiate its heat energy efficiently. Instead of radiating and cooling down, the gas remains
hot and spirals in to the center. “The heat energy released by viscous dissipation is not radiated immediately, as in a thin disk, but is stored in the gas as thermal energy and advected with the flow” Narayan ‘’06
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Main spectral states of accreting black holes
unabsorbed spectra
predicted detection by
Z. & Gierliński 2004
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black hole
cold accretion disk
active region soft seedphotons
reflectedphotons
scatteredhard
photons
Spectral States:
A. Zdziarski ‘05
cold outer disk
direct softphotons
scatteredhard photons
reflectedphotons
hot inner disk
variable inner radius
gravity + Coulomb
black hole
outflow/jet emitting radio/IR/...
Soft State
Hard State
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Power Spectra (Powspec & FFT)
QPO: quasiperidodical oscillationsFFT & PSD Statistics Terms:Power Spectral Density (PSD) FFT of the auto-correlation functionCross Spectral Density (CSD) FFT of the Cross-correlation function
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Phase Info (autocorrelation FFT):
Time Lag
Time Lag: Time or Phase Shifts between X-ray Pulses at different energies.
Difference in Photon Arrival times gives us information about source size and propagation speed
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Time Lags
Intrinsic signature of the interaction of the comptonized radiation with the NS and accretion disk plasma.
Energy dependent time lags are a result of downscattering and upscattering in a comptonized medium.
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Justification
Comptonization spectra models cannot provide by themselves information about the size of the scattering plasma neither the dynamics of the accretion of the hot gas onto the compact object
Magnitude of the time lags provides an estimate of the size of the scattering medium. Time Lags in contrast with PSD are not affected by variations in the accretion rate, as a result they probe properties inherent to the scattering cloud. Hua,Kazanas,Cui 1999
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Constraints
a) IGR J00291+5934.b) XTE J1751-305 c) SAX J1808.4-3658,Falanga, Titarchuk 2007
The data corresponds to MSP (millisecond pulsars), while our model had good fits in regular Pulsars (pulse period ~ seconds)
The RXTE-ASM light curve of LMC X-4, in 2–12 keV energy range, folded at the long term period of 30.276 ± 0.009 days. Naik,Paul 2003
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Advection model references
Blandford & Begelman (1999) non-relativistic advection dominated inflow-outflow solution
Becker, Subramanian & Kazanas (2001)pseudo-newtonian process in the event horizon RADIOS (self-similar relativistic advection dominated inflow-outflow solution)
Truong V. Le & Becker (2005)relativistic outflows in advection dominated accretion disks with shocks
Becker & Wolff (2006)Thermal and Bulk Comptonization in accretion powered X-ray pulsars
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Transport Equation
2 2 0 0 0 02 2 2 2
0 0
( ) ( ) ( )1 1v v
3 4
N r r t tf f d f fr r
t r r dr r r r r
First order Fermi energization Diffusion term
42 2
1e Te
e
n cf ff kT
t m c
Kompaneets Equation
Recoillosses
Stochastic energization by thermal electrons
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2 2 0 0 0 02 2 2 2
0 0
( ) ( ) ( )1 1v v
3 4
N r r t tf f d f fr r
t r dr r rr r r
0
9 31/ 21/ 4 2
0 00
3 30 00 0
3 2, , exp
1 18 2 1
x
t
xx x xN eF x w I
xxr xx
0( ) 21( , )
2iw t t
eF t dt observed fluxe
22
2
164 81 9ln
4 2 1
AB
AB
v
v
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5 10 15 20
-2.25
-2
-1.75
-1.5
-1.25
-1
-0.75
-0.5
M. Van Der Klis et Al. 1987
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Future Work
42 2
1e TB e
e
n c ff k T
m c
2 2 40 0 0 02 2 2 2 2 2
0 0
( ) ( ) ( )1 1 1v v
3 4e T
B ee
N r r t t n cf f d f f fr r f k T
t r dr r rr r r m c
•Add stochastic energization by thermal electrons, and the effect of the electrons recoil (Kompaneets equation)•The transport equation has to be solved considering a disc geometry.
Kompaneets equation term
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References Energy Dependent Time Lags as Observational Evidence of Comptonization Effects in The Neutron Star
Plasma Environment. Falanga, Titarchuk-2007 Thermal And Bulk Comptonization In Accretion-Powered X-RayPulsars. Becker,Wolff-2007 Timing and Spectral Studies of LMC X-4 in High and Low States with BeppoSAX: Detection of
pulsations in the soft spectral Component. Naik, Paul-2004 Probing The Structure of Accreting Compact Sources Through X-ray Time Lags and Spectra. Hua,
Kazanas,Cui-1999 Time Lags In Compact Objects: Constraints in the Emission Models.J.Poutanen-2000 X-Ray Spectral Formation In a Converging FluidFlow:Spherical Accretion Into Black Holes.
Titarchuk,Mstichiadis,Kylafis-1997 The Why & How of X-Ray timing
Z. Arzoumanian. 2003 X-Ray Summer School X-Ray Timing Analysis
Michael Novak- Chandra X-Ray Science Center / MIT Chandra X-ray Observatory
http://chandra.harvard.edu/ Dr. Peter Becker- Class Notes, Verbal Communication Dr. Lev Titarchuk- Class Notes, Seminars Dr. Rita M. Sambruna – Class Notes [1] A Catalog of Candidate Intermediate-luminosity X-ray Objects V2. ApJS 2002. E.J.M
Colbert, and A.F. Ptak. Gravity’s Fatal Attraction
Mitchell Begelman