Theory and Simulations of Radiation-Driven Disk Winds Daniel Proga - - PowerPoint PPT Presentation

Daniel Proga UNLV & Princeton University

Theory and Simulations of Radiation-Driven Disk Winds

Collaborators

§ J. Stone, T. Kallman, J. Raymond, M. Begelman,

• J. Ostriker, R. Kurosawa, J. Drew, A. Janiuk,
• M. Moscibrodzka, B. Czerny, A. Siemiginowska,
• A. Dorodnityn, S. Sim, S. Luketic, T. Waters, K.

Nagamine, P. Barai, and many more

OUTLINE

• 1. Introduction
• 2. Multidimensional, time-dependent simulations of disk

winds driven by:

• radiation pressure

and

• radiation pressure with thermal expansion
• 3. Conclusions

What can drive an outflow?

n Thermal expansion (e.g., evaporation and

hydrodynamical escape)

n Radiation pressure (gas, dust) n Magnetic fields

In most cases, rotation plays a key role (directly or indirectly) especially in AD.

Miller et al. (2006, 2008), Neilsen & Lee (2009) and others

BHBs

(fig. from DP’s 2009)

Radiation-Driven Winds

The equations of hydrodynamics

Dρ Dt + ρ∇ ⋅ v = 0 ρ Dv Dt = −∇P + ρg + ρ

rad

f

ρ D Dt e ρ ⎛ ⎝ ⎜ ⎞ ⎠ ⎟ = −P∇ ⋅ v + ρL P = (γ −1)e

Proga, Stone & Drew (1998)

D

L =1

S

L =0

D

L = 3

S

L =0

1

D

L = 3

S

L = 3

3

D

L = 3

S

L =9

HD simulations and their line profiles

HD simulations and observations

D

L =23.4

SUN

L

,

WD

L

=0.25

D

L ,

a

˙ M =

−8

3×10

SUN

M

−1

yr

CIV 1549 for IX Vel (Hartley et al. 2001); models Proga (2003b)

a

˙ M =

−8

1×10

Sun

M

−1

yr

WD

M

=1

Sun

M

Drew & Proga (1999)

A big picture

DP (2002)

FU Ori (MS S) AGN (SMBH) CV (WD) LMXB (NS) GBH (LM BH)

1/(TOTAL UV LINE OPACITY)

LEdd = 4πcGMa σ L = M ˙ M

aG

2r

a

Γ = L LEdd = ˙ M

aσ

8πcr

a

Γ

UV = LUV

LEdd

Thermal and Radiation- Driven Winds

The equations of hydrodynamics

Dρ Dt + ρ∇ ⋅ v = 0 ρ Dv Dt = −∇P + ρg + ρ

rad

f

ρ D Dt e ρ ⎛ ⎝ ⎜ ⎞ ⎠ ⎟ = −P∇ ⋅ v + ρL P = (γ −1)e

BH

M

=

8

10 Msun Γ = 0.6

Proga, Stone, & Kallman (2004) Proga & Kallman (2000)

Broad band spectra for various l.o.s.

Sim et al. (2010)

Quasar Irradiation

?

An outflow from an inflow

DP (2007)

BH

M

=

8

10

SUN

M

D

˙ M =

26

10 g/s =1.6

SUN

M /yr

X

T

=8 x

7

10 K ρ( o r )=

−21

10 g/

3

cm

UV

f

=

X

f

=0.5

DP (2007)

BH

M

=

8

10

SUN

M

D

˙ M =

26

10 g/s =1.6

SUN

M /yr

X

T

=8 x

7

10 K ρ( o r )=

−21

10 g/

3

cm

UV

f

=0.95

X

f

=0.05

Effects of gas rotation, optical depth and X-ray background radiation

DP, Ostriker, Kurosawa (2007)

no rotation rotation rotation and opt. thick no X-ray background X-ray background

3-diminesional simulations

Kurosawa & DP (2009a) stay tuned ... e..g., Sim et al. (in preparation)

density map temperature map

Kurosawa & DP (2009a) see also Barai et al. 2011a,b)

Clouds properties

Conclusions

n Simulations of accretion flows and their outflows provide important

insights into the dynamics and geometry of the material that produces

• radiation. In particular, we can use the simulations to assess the

effects of radiation on the flow properties. We can also explore coupling between accretion flows and they outflows as well as mass supply (e.g., various forms of feedback).

n The simulations can be and are used to compute synthetic spectra for

direct comparison with the observations. As such, the simulations are useful in explaining specific spectral features as well as overall shape

• f the SED.

Multi-component flow

torus wind torus corona torus low l inflow

• utflow/jet

Proga (2005)

Does it have to be so complex?

Answer: No, it does not.