broad iron lines from accretion disks
DESCRIPTION
Broad iron lines from accretion disks. K. Iwasawa University of Cambridge. Accreting black hole systems Most energy dissipates at inner radii of the accretion disk. In the accretion disk + corona model. An X-ray source illuminates the disk to give rise reflection - PowerPoint PPT PresentationTRANSCRIPT
Broad iron lines from accretion disks
K. IwasawaUniversity of Cambridge
Accreting black hole systems
Most energy dissipates at inner radii of the accretion disk
In the accretion disk + corona model
An X-ray source illuminates the disk to give rise reflection
The most prominent spectral feature is Fe K line
Effects of strong gravity
Because of the proximity to a black hole, relativistic effects are important
Doppler shift
Gravitational redshift
ASCA observation of MCG-6-30-15
Tanaka et al 1995
Other examples of broad iron emission
Seyfert nucleus
IRAS 18325-5926
Galactic black hole binary
XTE J1650-500
Iwasawa et al 2003
Miniutti et al 2003
XMM-Newton observations of MCG-6-30-15
Vaughan & Fabian 2003 MNRAS submitted
See also Wilms et al 2002; Fabian et al 2002; Vaughan et al 2002; Fabian & Vaughan 2002; Ballantyne et al 2003; Reynolds et al 2003
Overall spectral shape of MCG-6-30-15
MCG-6-30-15
/ 3C273
Fluxed spectrum
Fe K line profile after correcting for warm absorption (modelled by Turner et al 2003 based on RGS data analysis)
RMS variability spectra for the 2001 data
Whole observation
Neighbouring bins
(See also Matsumoto et al 2003)
Spectral changes seen in 10 flux slices
Spectrum of the variable component
Difference spectrum: (High flux)-(Low flux)
Presence of a stable componentIn MCG-6-30-15
Offset
Spectrum of the constant component fraction
Variable power-law
Stable reflection-dominated component
Schematic picture of the two-component model
Variability of Fe K line in MCG-6-30-15
ASCA 1994 ASCA 1997
Iwasawa et al 1996 Iwasawa et al 1999
Excess emission above a fitted absorbed power-law continuum
Line-Flux correlations from the 2000 + 2001 observations
Line-Flux correlations from a simulation for the 2000+2001 data
Comparison between real-data and simulations
Simulation for the 2000 observation
Line-Flux correlations from the 2000 observation
Simulation-Realdata comparison for the 2000 observation
Rapid variation of the line core during the 2000 observation
See also M Cappi’s poster
Simulation-Realdata comparison for the 2nd orbit of the 2001 observation (high-flux state)
Summary of the Fe K line properties in MCG-6-30-15
• Presence of red wing appears to be robust• Spectral variability can be explained by the
two-component model: variable power-law + (semi)-stable reflection dominated emission.
• There are occasional variability. • The line emission is most likely to originate
from the relativistic region close to a black hole.
Broad Fe lines from Accretion Disks
Giovanni MiniuttiInstitute of Astronomy - Cambridge
In collaboration with Andy Fabian and with
Russell Goyder, and Anthony Lasenby
Summary of MCG-6-30-15 observations:
A broad Fe line is present in all flux states
Fe line red wing suggests a rotating Kerr black hole
1. The broad Fe line
Fabian et al 02
Tanaka et al ’95 – Iwasawa et al ’96 - Guainazzi et al ’99 – Wilms et al 01 – Fabian et al 02 …
Summary of MCG-6-30-15 observations:
A broad Fe line is present in all flux states
Fe line red wing suggests a rotating Kerr black hole
1. The broad Fe line
A steep emissivity profile is implied ( > 3 ) possibly in the form of a broken power-law
The emissivity suggests the presence of a centrally concentrated primary source of hard X-rays
Tanaka et al ’95 – Iwasawa et al ’96 - Guainazzi et al ’99 – Wilms et al 01 – Fabian et al 02 …
Summary of MCG-6-30-15 observations:
The Fe line generally appears to be
The Fe line-continuum correlation is puzzling
2. The variability properties (> 10ks)
1. Fe line almost constant in “normal” flux states while the continuum varies by a factor 3-4
broader in low flux states narrower in high flux states
2. Fe line is correlated with continuum in low flux states
Iwasawa et al ’96 – Iwasawa et al ’99 – Wilms et al 01 – Lee at al 02 ...
Shih et al 02 - Fabian & Vaughan 03 – Vaughan & Fabian 03 (submitted)
Reynolds et al 03 (submitted)
A light bending model in the Kerr BH spacetimePrimary source of X-
rays• isotropic emission• position specified by h
Photons lost into the BH
RDC reaches the disc and then the observer
PLC reaches the observer
The source is linked to the disc
The orbital timescale << 10ks
corotatingring-like source
GM et al 03, MNRAS, 344, L22 – GM & Fabian 03, astro-ph/0309064 (submitted)
The variability of the PLC is induced by light bending
The variability is due to changes in the height of the primary source at constant intrinsic luminosity
(i.e. at constant mass accretion rate)
1. If the height of the source is small
most of the emitted photons are bent towards the disc and only a small fraction can escape at infinit so that the observed PLC is small (low flux states)
2. if the height is increased
light bending is less effective and more photons are able to reach infinity so that the observed PLC
increasesThe main idea is thus that changes in the height of
the source induce the observed variability via gravitational light bending
PLC
Disk
Disk + lost photons
Primary source emission: where do photons land ?
the PLC drops as the source height (x-axis) gets smaller
averaged (ring-like) non averaged (point-like) present X-ray missions future X-ray missions
Disk emissivity
We present results for averaged emissivity
Emissivity dependence on the primary source height (decreasing clockwise)
The emissivity has the form of a broken power law
steeper in the inner disk region and flatter in the outer
Flat profile at large heights and steep at low heights
= 6
= 3
hs = 1 rg
hs = 20 rg
PLC
Fe line
PLC and Fe line variability induced by light bending
The Fe line varies with much smaller amplitude
hs
Small h = low PLC fluxLarge h = high PLC flux
PLC
Fe line
Fe line EW
The Fe line EW is anti-correlated with the PLC
The Fe line EW tends to constant at very low PLC flux
hs
Regime III: large source height and anti-correlationRegime II: intermediate source height and constant Fe line
Regime I: small source height and correlation
IIIIII
Fe line – PLC correlation
III
II III
I IIIII
Variability timescales
Assuming the primary source is moving with v = 0.1 c and that the BH has a mass of 10 solar
masses the PLC can vary by a factor 4 in about 2ks (or by a factor 20 in 10ks)
7
this may help to explain the extreme variability in some systems (such as e.g IRAS 13224-3809)
most extreme variation is a factor 3-4 in 10ks
XTE J1650-500 during outburstFe lin
e fl
ux
9-100 keV PLC flux
Rossi et al 03
GM & Fabian 03
I/II
III
I II III
?
Conclusions Some predictions of the light bending model
1. The Fe line flux is correlated with the continuum
during low flux states and anti-correlated during high flux states2. The Fe line flux is constant during intermediate
flux states while the continuum varies by a factor 4
correlated
constant
anti-correlated
Conclusions Some predictions of the light bending model
1. The Fe line flux is correlated with the continuum
during low flux states and anti-correlated during high flux states2. The Fe line flux is constant during intermediate
flux states while the continuum varies by a factor 4
3. The Fe line EW is generally anti-correlated with the continuum and almost constant only during
very low flux states4. The hard spectrum is more and more reflection
dominated as the PLC flux drops
Thank you