Qwind 2

Improvements respect to Qwind

1. Model for initial conditions
2. Better radiative transfer
3. Self-consistent mass accretion rate
4. Physical SED

1. Initial conditions

• Locally, solve the 1-D line-driven wind problem.
• Analogous to O-stars but:
  • Different gravity (disc) z / r^3
  • Different radiation (constant)
• Solve momentum equation to compute mass-loss rate
• Start Qwind at the sonic point (very close to the disc)

2. Radiative transfer

3. Self-consistent mass accretion rate

• Initial conditions depend on local Mdot through the local temperature
• Initial density and velocity are adjusted after every iteration

4. Physical SED

We launch a wind everywhere with Mdot > 0 (starting at 6Rg)

Local flux profile follows QSOSED