Further Criteria for the Existence of Steady Line-Driven Winds

Abstract

In Paper I, we showed that steady line-driven disk wind solutions can exist by using "simple" models that mimic the disk environment. Here I extend the concepts introduced in Paper I and discuss many details of the analysis of the steady/unsteady nature of 1D line-driven winds. This work confirms the results and conclusions of Paper I, and is thus consistent with the steady nature of the 1D streamline line-driven disk wind models of Murray and collaborators and the 2.5D line-driven disk wind models of Pereyra and collaborators. When including gas pressures effects, as is routinely done in time-dependent numerical models, I find that the spatial dependence of the nozzle function continues to play a key role in determining the steady/unsteady nature of supersonic line-driven wind solutions. I show here that the existence/nonexistence of local wind solutions can be proved through the nozzle function without integrating the equation of motion. This work sets a detailed framework with which we will analyze, in a following paper, more realistic models than the "simple" models of Paper I.

arXiv comment30 pages, 5 figures, accepted for publication by The Astrophysical Journal

References in corpus (4)

• Reverberation Mapping and the Disk Wind Model of the Broad Line Region
• Hydrodynamic Models of Line-Driven Accretion Disk Winds II: Adiabatic Winds from Nonisothermal Disks
• On the Steady Nature of Line-Driven Disk Winds
• Hydrodynamic Models of Line-Driven Accretion Disk Winds III: Local Ionization Equilibrium

Cited by in corpus (2)

• A Method for the Study of Accretion Disk Emission in Cataclysmic Variables I: The Model
• On the Steady Nature of Line-Driven Disk Winds: Application to Cataclysmic Variables