The role of outflows in black-hole X-ray binaries | Astronomy & Astrophysics (A&A)

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Table A.1.

Parameters of the model.

Symbol	Value	Units	Parameter
β	0.5^a	–	Index of the radial dependence with height of the outflow
τ_∥	1 − 6	–	Optical depth to electron scattering along the axis of the outflow
R₀	50 − 1500	$R_{g}^{b}$ $R_{\mathit{g}}^{\,b}$	Radius of the outflow at its base
γ₀^c	1.10–1.15	–	Lorentz factor of the electrons, when the flow is coasting
kT_BB	0.2	keV	Characteristic energy of the input soft photons
z₀	5	R_g	Distance of the bottom of the outflow from the black hole
H	10⁵	R_g	Height of the outflow
z₁	50	R_g	Height of the acceleration zone
a	0.5	–	Exponent of the velocity profile in the acceleration zone
R_disk	10³	$R_{ISCO}^{d}$ $R_{\mathrm{ISCO}}^{\,d}$	Outer radius of the accretion disk
cos θ^e	–1 to 1	–	θ is the viewing angle
m	10	M_⊙	Mass of the black hole
N_phot	10⁷ − 10⁸	–	Number of simulated photon beams
p^f	3	–	Index of the Lorentz factor power-law distribution
$γ_{\min}^{f}$ $\gamma_{\mathrm{min}}^{\,f}$	1	–	Lower limit of the Lorentz factor power-law distribution
$γ_{\max}^{f}$ $\gamma_{\mathrm{max}}^{\,f}$	500	–	Upper limit of the Lorentz factor power-law distribution

Notes. ^a: β = 0.5 assumes a parabolic outflow^b: Gravitational radius R_g = Gm/c². R_g ≈ 1.48 × 10⁶ cm for a m = 10 M_⊙ black hole^c: $γ_{0} = 1 / \sqrt{1 - (v_{0}^{2} + v_{⊥}^{2}) / c^{2}}$ $\gamma_0 = 1/\sqrt{1-(\mathit{v}_0^2+\mathit{v}_\perp^2)/c^2}$ ^d: Radius of the inner-most stable circular orbit.^e: θ is the angle between the observer and the outflow axis. The code records the escaping direction of the photon in bins of 0.1 in w = cos θ, from w = −1 to w = 1. Negative values indicate back scattering.^f: For the computation of the radio emission.

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