A New Numerical Method for Solving Radiation Driven Winds from Hot Stars

Abstract

We present a general method for solving the non--linear differential equation of monotonically increasing steady--state radiation driven winds. We graphically identify all the singular points before transforming the momentum equation to a system of differential equations with all the gradients explicitly give. This permits a topological classification of all singular points and to calculate the maximum and minimum mass--loss of the wind. We use our method to analyse for the first time the topology of the non--rotating frozen in ionisation m--CAK wind, with the inclusion of the finite disk correction factor and find up to 4 singular points, three of the x--type and one attractor--type. The only singular point (and solution passing through) that satisfies the boundary condition at the stellar surface is the standard m--CAK singular point.

Accepted for publication in Astronomische Nachrichten / Astronomical Notes

References in corpus (3)

• Be-star rotation: how close to critical?
• The influence of rotation in radiation driven wind from hot stars: New solutions and disk formation in Be stars
• The influence of rotation in radiation driven winds from hot stars II. CAK topological analysis

Cited by in corpus (8)

• New hydrodynamic solutions for line-driven winds of hot massive stars using Lambert $W$-function
• Radiation-Driven Wind Hydrodynamics of Massive Stars: A Review
• Evolution of rotating massive stars with new hydrodynamic wind models
• New self-consistent wind parameters fitting optical spectra of O-type stars observed with HERMES spectrograph
• Evolution of rotating massive stars adopting a newer, self-consistent wind prescription at SMC metallicity
• Co-existence and switching between fast and $\Omega$-slow wind solutions in rapidly rotating massive stars
• Revisiting Viscous Transonic Decretion Disks of Be Stars
• Revisiting the Evolutionary Status of Massive Stars at the central parsec of the Milky Way