Outline Quasar Outflows Doron Chelouche (IAS and TAU) Introduction Model NGC 3783 Conclusions Quasar...
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Transcript of Outline Quasar Outflows Doron Chelouche (IAS and TAU) Introduction Model NGC 3783 Conclusions Quasar...
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Quasar Outflows Doron Chelouche (IAS and TAU)
•Introduction
•Model
•NGC 3783
•Conclusions
Quasar Outflows: The X-ray perspective
Doron Chelouche
Institute for Advanced Study, Princeton NJ
(currently at: Tel-Aviv University, Israel)
Proga et al. 2000
Intro
duct
ion
Quasar Outflows Doron Chelouche (IAS and TAU)
Phenomenology:
•blueshifted absorption lines
•common in type-I quasars
•velocity range: 102-105 km s-1
BAL flows
Relevant to:
•Accretion-ejection processes
•Quasar structure (unification)
•Galaxy and cluster formation
Kaspi et al. 2002
NAL flows
Elvis M.
Determining the flow properties is essential for investigating these issues
Mod
elQuasar Outflows Doron Chelouche (IAS and TAU)
Aim: to determine the flow properties
Mean: by comparing model predictions to observations
Kaspi et al. 2002
Flow properties are poorly constrained
predictionsmethod
Spectral features(line, continuum)
Flow properties(v, )
photoionization
dynamics
•
M
Mod
elSolution: Combine detailed photoionization and dynamical calculations
Quasar Outflows Doron Chelouche (IAS and TAU)
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Next step: Comparing to observations
Quasar Outflows Doron Chelouche (IAS and TAU)
NG
C 3
783
•>100 absorption lines
•Continuum absorption
•Continuum variability
Rest wavelength (A)
Pure photoionization models
George et al. 98
Krongold et al. 03
Netzer et al. 03
?????
What is the physics characterizing the multiphase flow?
Kaspi et al. 2002
Arav 1996
Quasar Outflows Doron Chelouche (IAS and TAU)
Ionization potential
Kaspi et al. 2002NG
C 3
783The dynamical viewpoint
de Kool et al. 2002
Calculating…mixed phases reminiscent
of a turbulent medium
],[ ; maxmin ρρξρ β∝
Reeves et al. 2003
Summary of X-ray results for NGC3783
•The flow is energy driven (radiative acceleration is negligible)
•The flow is launched beyond the accretion disk (torus association?)
•The mass loss rate is similar to/smaller than the mass accretion rate (much smaller than previous estimates)
•The flow density structure is reminiscent of a turbulent ISM (triggered by the central star cluster?)N
GC
378
3Quasar Outflows Doron Chelouche (IAS and TAU)
Crenshaw et al. 1999
conc
lusi
ons
Quasar Outflows Doron Chelouche (IAS and TAU)
•Studying quasar outflows is important for understanding accretion phenomena, quasar structure, and galaxy/cluster formation
•High resolution and S/N X-ray grating spectra provide a unique view of such flows
•Realistic spectral fits accounting for hundreds of line and continuum features are feasible
•Combined dynamical, photoionization, and spectral modeling can reveal the physical properties of the ouflowing gas
•Similar models can be used to study gas dynamics in other systems (e.g., X-ray binaries)Th
ank
you!