Radiatively Driven Winds and Disks Stan Owocki Bartol Research Institute University of Delaware CAK (1975) line-driven wind theory steady, 1D spherically.

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Presentation transcript:

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

Doppler Shifting of Line-Absorption in an Accelerating Stellar Wind

Height (R * ) CAK Steady-State Velocity (km/s) Density (g/cm 3 ) 1D Simulation of small-scale line-driven instability X-ray emitting shock

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

WCD Inhibition by non-radial line-forces Vrot (km/s) = Wind Compressed Disks

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

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

Accretion Disk Winds from BAL QSOs

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