%0 Journal Article
%T The Mechanism of Interacting Stellar Winds beyond Red Giant Branch
%A Sundus A. Abdullah Albakri
%A Sinan H. Ali
%J International Journal of Astronomy and Astrophysics
%P 367-371
%@ 2161-4725
%D 2013
%I Scientific Research Publishing
%R 10.4236/ijaa.2013.34041
%X <p class=\"MsoNormal\">
	<span lang=\"EN-US\" style=\"font-family:Verdana;\">The dynamical processes of the interaction of slow wind
beyond Red Giant phase with fast wind of central star of nebula are evaluated.
The mechanism of interaction stellar wind model (ISW) </span><span lang=\"EN-US\" style=\"font-family:Verdana;\">is </span><span lang=\"EN-US\" style=\"font-family:Verdana;\">found to be
responsible </span><span lang=\"EN-US\" style=\"font-family:Verdana;\">for</span><span lang=\"EN-US\"><span style=\"font-family:Verdana;\"> producing a relatively dense shell of gas which increases in mass
and radius at a constant rate. Both slow wind and superwind are assumed to be
time independent and radial density is calculated at initial time </span><i><span style=\"font-family:Verdana;\">t</span><sub><span style=\"font-family:Verdana;\">o</span></sub></i></span><span lang=\"EN-US\"> </span><span lang=\"EN-US\" style=\"font-family:Verdana;\">~ 60 yrs with the
fast wind velocity </span><span lang=\"EN-US\" style=\"font-family:Verdana;\">(</span><i><span lang=\"EN-US\" style=\"font-family:Verdana;\">v</span></i><span lang=\"EN-US\"> </span><span lang=\"EN-US\" style=\"font-family:Verdana;\">¡Ö</span><span lang=\"EN-US\"> </span><span lang=\"EN-US\" style=\"font-family:Verdana;\">1000
km/s</span><span lang=\"EN-US\" style=\"font-family:Verdana;\">)</span><span lang=\"EN-US\" style=\"font-family:Verdana;\">. The results showed that, at the outer rim of super wind region, a
small density hump appears due to the relative velocity between slow winds and
central star winds, in a good agreement with the previous models. The dynamical
requirements of the observed expansion of planetary nebulae can be satisfied by
the mechanism of interacting stellar wind model with reasonable mass loss rate
from central star.</span> 
</p>
%K Nebulae
%K Stars
%K Evolution
%K Mass Loss
%U http://www.scirp.org/journal/PaperInformation.aspx?PaperID=37624