Transcript cxc.harvard.edu

High Resolution Spectra of Accretion Disk Winds
John Raymond
What parameters can you derive?
Mass
.
M accretion
.
M wind
Router
Mukai et al. 2003
Rinner
Spin
Inclination
Magnetic geometry
Mauche 2004 SS Cyg
DIAGNOSTICS
Emission or Absorption Lines
Ionization Parameter or Temperature
Recombination
Collisional Ionization
Time-Dependent Ionization
Column Density
Density O V K
Line Profiles
Velocity
Velocity Width EX Hya?
P Cygni
Abundances
Kaastra et al. 2005
DIAGNOSTICS II
Emission or Absorption Lines
Ionization Parameter or Temperature
Recombination
Collisional Ionization
Time-Dependent Ionization
Liedahl et al.
Paerels et al
Cyg X-3
What Physics can you investigate?
Heating (dissipation)
Turbulence
Boundary Layer
Disk
ADAF or ADIOS
Photoionization
Winds (Warm Absorbers)
Radiation Pressure
Thermal Pressure
Magnetic driving
(Blandford & Payne or
small scale fields)
.
.
Significance of M and E
Jimenez-Garate et al
Accretion Disk Winds
.
High M CVs
-- ~ 3000 km/s
-- low. ionization state:
<QNe>~5
.
-- Mwind ~ 0.1 Macc
-- modest collimation
-- from or near boundary layer
AGN
-- ~ 1000 km/s
-- Range of ionization states: QFe = 7-24
.
.
-- Mwind
. = 0.02 to 0.05 Macc .
-- originate 0.01 to 1 pc from BH, ~103 to 104 Rs -- clumpy, multiphase
LMXBs
-- 1000 km/s
-- high ionization QFe ~ 22 - 27
-- Mwind
up to Macc.
. 10
-- ~ 10 cm 103 Rs
--- narrow range of ionization parameter
Jimenez-Garate et al. 2005
Her X-1 Low State
Illuminated accretion disk
Lines washed out when
central source is visible
Agrees with reprocessing
domination in optical
Evaporation or Condensation
Jimenez-Garate et al. 2001
Lines From Winds
OY Car Outburst; Mauche & Raymond
1000s of km/s
Biconical Flows
P Cygni profiles
Pure scattering lines
(Only resonance lines seen)
Cir X-1; Schulz & Brandt
Cal 87; Greiner et al.
AGN Absorption Lines
Range of Ionization States
O III = O VIII
Fe M and L shell Ions
(Unlike most X-ray binaries)
Very good agreement between
model and observations
(Instrumental artifacts
Limitations of atomic data)
Unresolved Transition Arrays
Chelouche & Netzer 2005: NGC 3783
AGN Absorption Lines
Strong 1000 km/s Wind
Finite radial extent
Moderate Ionization
Radiation Pressure,
Thermal Pressure
Adiabatic Cooling
Multiphase Medium
Chelouche & Netzer
Krongold et al. 2007: NGC 4151
GRO1655-40
April 1, 2005
90 Absorption Lines!
(2 is typical)
Constant for 64 ksec
Lines of Na, Al, P, Cl, K,
Ti, Cr, Mn, Co
Fe XXII – XXVI
Fe XXIV 2-3 to 2-10
Density sensitive ratios
300-1600 km/s Blue-shifts
WIND
3x1037 erg/s
Very Soft
Miller et al. 2006
Miller et al.
VERY Highly Ionized compared to AGN
Need to use Voigt profiles to model EW (saturation)
High A values mean little flat part to curve of growth
Double Abundances of O, Ne and Ca-Ni to match
(Does not agree with optical abundances of Israelian et al. or
González Hernández et al. enhancement of Si and S)
Low Covering Factor: > 6° (no eclipse) < 12° (no Fe XXIV 3s-2p)
Fe XXII
ne determines fine structure populations of 2p level (Mauche et al.)
2s2p4p 2P
2s2 4d 2D 3/2 , 2D 5/2
2s2p3p 2P
2s2 3d 2D 3/2 , 2D 5/2
2s2 2p 2P 1/2, 2P 3/2
11.77 and 11.92 Å lines
Radiation Negligible
Not Saturated
Radiative Driving?
Opacity in UV Lines
O stars, CVs?, AGN
NO: Add up force in lines
High Ionization-no UV Lines
Force Multiplier=1.6
Thermal Driving
Compton Heating
Photoionization heating
Begelman et al.
Magnetic Processes
Magneto-centifugal
Poynting Flux from MRI
Blandford/Payne; Miller/Stone
Thermally Driven Wind?
Woods et al.
Begelman, McKee & Shields
TIC = 1.4x107 K
RIC= 10 11.7 cm (cs=vesc)
Wind at r > 0.1 to 0.2 RIC
r > 10 10.7 cm
Woods et al.
Full heating, cooling and hydro
Illuminating spectrum very similar to
GRO1655-40
Proga & Kallman
Disk UV can help launch wind, but
density still low
Where is the gas in GRO1655-40?
ξ = L/nr2
N = nr = L/ξr
r < L/Nξ
(L from continuum, N and ξ from lines)
OR
r = (L/nξ)1/2
(n from Fe XXII)
Miller et al. 2006: r < 10 9.5 cm < 0.01 RIC
Netzer 2006
: r0 = 10 10.7 cm
Miller et al. 2007: r0 < 10 10 cm < 0.02 RIC
Slab vs 1/r2
: Not Thermally Driven
: Maybe Thermally Driven
: Not Thermally Driven
(allows somewhat lower )
Fe XXII density ( 11.77Å line cannot be saturated given 2p-4d lines)
Woods et al
Mass Loss Rate
.
M = vA
Woods et al predict
a peak mass loss rate
of 6x10–6 g/(cm2 s)
(scaled with BH mass)
Divide by v=500 km/s
(Vertical wind makes it
worse.)
nmax = 1011 cm-3
vs observed 1014.6 cm -3
THERMAL WIND PREDICTS A DENSITY TOO LOW BY
ORDERS OF MAGNITUDE
equatorial
Magnetic Disk Wind Model
Proga 2003
Equatorial
Matches modest solid angle
v = few*10^(2-3) km/s
Few hundred km/s
Matches observed Doppler shift
high m-dot
High M-dot
Matches High density
Thermally driven wind may explain
more typical high , low ne when only
Fe XXV and Fe XXVI are detected?
Conclusions
Disks and Winds give rich absorption and emission spectra
with lots of diagnostic possibilities.
Emission lines are visible when central continuum is obscured.
Disk emission from LMXRBs is consistent with a photoionization
dominated corona.
Winds are ubiquitous is CVs, AGN and XRBs.
Mass loss rates are significant compared to accretion rates.
Radiation pressure is not sufficient.
Thermal pressure may be sufficient for AGNs and some XRB
spectra, but not for the GRO1655-40 low soft state or for CVs
in the high state.
Therefore, magnetic forces are important in some cases.
Extra Slides
Netzer argued Fe XXII 11.77Å line is saturated, but patchy to
allow n2/n1 ~ 0.1
Identified 11.54Å and 11.42Å as weaker Fe XXII lines, but
Separation is wrong and 11.42 is too strong.
2p – 4d
2s – 4p?
Predicts 8.97 Å 2p 2P1/2 - 4d line stronger than 11.92Å
2p 2P3/2 – 3d line. Fails by more than a factor of 4.
Nearly optically thin ratio matches prediction. 2.6mÅ : 16 mÅ
Model Ingredients/Constraints
Photoionized gas
Ionizing spectrum
Density structure (Slab, wind, hydrostatic)
Velocity structure
Abundances
Radiative Transfer
Lots of Atomic Physics
CLOUDY, XSTAR, ION
Hot Plasma
Temperature structure (ADAF, BOUNDARY LAYER)
Density structure
Velocity Structure
Abundances
Lots of Atomic Physics
APEC, MEKAL, CHIANTI