|AHELP for CIAO 4.3 Sherpa v1||
Self-irradiated funnel. XSpec model.
The multi-blackbody "Self-IrRadiated Funnel" model is designed to model optically-thick outflow-dominated accretion. The basic idea is simple: you just assume a lot of matter, angular momentum and energy emerges in a limited volume. Momentum conservation leads to non-sphericity of the flow that has subsequently conical (funnel-like) shape. The model calculates temperature distribution at the funnel walls (taking into account irradiation by iterative process) and the outer photosphere. We also assume that inside the cone there is a deep pseudo-photosphere. Relativistic boosts are taken into account for high velocities. For a comprehensive description of the physical model, see: Abolmasov, P., Karpov, S. and Kotani, T. PASJ, 61, 2, 213.
This is an additive model component.
|1||tin||inner temperature (at the inner, inside-the-funnel photosphere)|
|2||rin||inner (inside-the-funnel photosphere) radius in "spherisation radius" units (the latter is defined as 3 K Mdot / Omega_f c).|
|3||rout||outer photosphere radius in "spherisation radius" units.|
|4||theta||half-opening angle of the cone|
|5||incl||inclination angle of the funnel. Affects mainly self-occultation and relativistic boost effects.|
|6||valpha||velocity law exponent, v goes as r^valpha|
|7||gamma||adiabatic index. It affects the inner, hotter parts of the flow, therefore it is set to 4/3 by default.|
|8||mdot||mass ejection rate in Eddington (critical) units|
|9||irrad||number of iterations for irradiation|
This information is taken from the XSpec User's Guide. Version 12.6.0l of the XSpec models is supplied with CIAO 4.3.
For a list of known bugs and issues with the XSPEC models, please visit the XSPEC bugs page.
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