## Line-Driven Winds Revisited in the Context of Be Stars: Ω-slow Solutions with High k Values

**Jessie Silaj(1), Michel Cure(2), Carol E. Jones(1)**

(1) Department of Physics and Astronomy, The University of Western Ontario, Canada

(2) Instituto de Fisica y Astronomıa, Universidad de Valparaıso, Chile

The standard, or fast, solutions of m-CAK line-driven wind theory cannot

account for slowly outflowing disks like the ones that surround Be stars. It

has been previously shown that there exists another family of solutions --- the

$Omega$-slow solutions --- that is characterized by much slower terminal

velocities and higher mass-loss rates. We have solved the one-dimensional m-CAK

hydrodynamical equation of rotating radiation-driven winds for this latter

solution, starting from standard values of the line force parameters ($alpha$,

$k$, and $delta$), and then systematically varying the values of $alpha$ and

$k$. Terminal velocities and mass-loss rates that are in good agreement with

those found in Be stars are obtained from the solutions with lower $alpha$ and

higher $k$ values. Furthermore, the equatorial densities of such solutions are

comparable to those that are typically assumed in ad hoc models. For very high

values of $k$, we find that the wind solutions exhibit a new kind of behavior.

**Reference: **ApJ 795, 78 (2014)

Status: Other

**Weblink: **http://arxiv.org/abs/1411.1465

**Comments: **

**Email: **michel.cure@uv.cl