Hydrodynamical Models of Line-driven Accretion Disk Winds

Details Hydrodynamical Models of Line-driven Accretion Disk Winds Hydrodynamical Models of Line-driven Accretion Disk Winds

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997apj...477..368p&link_type=abstract

Astrophysical Journal v.477, p.368

Astronomy and Astrophysics

Astronomy

37

Accretion, Accretion Disks, Hydrodynamics, Stars: Novae, Cataclysmic Variables, Stars: Mass Loss

Scientific paper

We present here one-dimensional analytic hydrodynamic models and both one-dimensional and two-dimensional numerical hydrodynamic models for line-driven accretion disk winds from cataclysmic variable (CV) systems. Using the one-dimensional analytic models we explore the physical conditions necessary for the existence of a disk wind and study the dependence of wind speed and mass-loss rate on radius. The results of our two-dimensional model are consistent with the spectrum observed from CVs in the polar nature of the wind, the maximum absorption at roughly half the terminal speed of the P Cygni profiles, and the order of magnitude of the terminal speeds. For disk luminosity Ldisk = L&sun;, white dwarf mass Mwd = 0.6 M&sun;, disk radius Rdisk = R&sun;, and sound speed a = 10 km s-1 we obtain a wind mass-loss rate of M dot _{{wind}}=2{x10}^{-14} Msolar yr-1 and a terminal velocity of ~3000 km s-1. The two-dimensional models show that centrifugal forces produce shocks in the disk wind. If these shocks were absent, the mass-loss rates obtained would be too low to produce the optical depths required to explain the P Cygni profile of CVs. The two-dimensional models demonstrate the importance of centrifugal forces in winds from accretion disks and thus the necessity of models where these forces may be represented.

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