• Rin – inner launch radius (units of RG)
  • Rout – maximum launch radius (units of  Rin )  controls thickness of wind
  • d – focus of wind streamline (units of Rin) below the disk plane, which controls the degree of collimation and opening angle of the wind: tan(θin) = Rin/d i.e., θin=45deg

Measurable Physical Parameters:

  • Terminal velocity: v=fv(2GMBH/Rin)1/2
  • Mass outflow rate (in Eddington units): ṁout=Ṁout/ṀEdd
  • X-ray ionizing luminosity (% of Eddington): LX=L2-10keV/LEdd

What is the DISK-WIND model?

The DISK-WIND model is generated through a 2.5D Monte Carlo radiative transfer code which provides a physically-motivated, self-consistent treatment of both absorption and emission from an accretion disk-wind by computing the local ionization state and velocity field within the flow.

An interesting outcome of this model is that the accretion disk-wind itself can give rise to iron K emissions, with line widths up to σ ~ 1000 eV. Such profiles are obtained from the combination of:

(i) velocity shear in the flow,

(ii) its rotation around the polar axis, and

(iii) the Compton scattering of the iron K line photons from the wind.

mtables for XSPEC:

diskwind_fast32rg.zip diskwind_slow64rg.zip (800 Mb each)

See Matzeu et al. 2022, Sim et al. 2008, 2010

for more details.

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