1. Radiatively Driven Winds and Disks Stan Owocki Bartol Research Institute University of Delaware CAK (1975) line-driven wind theory steady, 1D spherically symmetric applied to hot, luminous, massive, OB-type stars Modern extensions & applications: Small-scale instability Co-rotating Interaction Regions (CIRs) Radiative braking in colliding wind binaries Wind Compressed Disk inhibition Line-driven ablation Accretion disk winds in BAL QSOs Collaborators: David Cohen, Bartol Ken Gayley, U. Iowa Steve Cranmer, Harvard CfA Joachim Puls, Munich

2. Doppler Shifting of Line-Absorption in an Accelerating Stellar Wind

3. 0.00.51.0 0 500 1000 1500 -15 -14 -13 -12 -11 -10 Height (R * ) CAK Steady-State Velocity (km/s) Density (g/cm 3 ) 1D Simulation of small-scale line-driven instability X-ray emitting shock

4. XMonitoring campaigns of P- Cygni lines formed in hot-star winds also often show modulation at periods comparable to the stellar rotation period. XThese may stem from large-scale surface structure that induces spiral wind variation analogous to solar Corotating Interaction Regions. HD64760 Monitored during IUE “Mega” Campaign Rotational Modulation of Hot-Star Winds Radiation hydrodynamics simulation of CIRs in a hot-star wind

5. WCD Inhibition by non-radial line-forces Vrot (km/s) = 200 250 300 350 400 450 Wind Compressed Disks

6. O star * WR star * WR star Radiative braking in colliding wind binaries

7. g lines ~ dv l /dl Line-Driven Ablation Net radiative Flux = 0, but g lines ~ dv l /dl > 0 !

8. Accretion Disk Winds from BAL QSOs

9. local CAK model nonlocal smooth model nonlocal structured model c.  log(Density) b. a. 2D Simulation of large-scale Co-rotating Interaction Regions