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) is found to be
responsible for 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 to ~ 60 yrs with the
fast wind velocity (v ≈ 1000
km/s). 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.
Cite this paper
S. Albakri and S. Ali, "The Mechanism of Interacting Stellar Winds beyond Red Giant Branch," International Journal of Astronomy and Astrophysics
, Vol. 3 No. 4, 2013, pp. 367-371. doi: 10.4236/ijaa.2013.34041
 B. A. Sargent, et al., “The Mass Loss Return from Evolved Stars to Large Magellanc Cloud II. Dust Properties for Oxygen-Rich Asymptotic Giant Branch Stars,” Astrophysical Journal, Vol. 716, No. 1, 2010, pp. 878-881.
 K. Werner and T. Rauch, “Late Helium Flashes and Hydrogen-Poor Stars,” Kepler Center for Astro and Particle Physics, University of Tübingen, Tübingen, 2009.
 S. Kwok, “On the Origin of Planetary Nebulae,” Astrophysical Journal, Vol. 219, 1978, pp. L125-L127.
 S. De Ruyter, H. Van Winckel, C. Domind, et al., “Strong Dust Processing in Circum Stellar Disk around RV Tauri Stars,” Astronomy and Astrophysics Journal, Vol. 435, 2005, pp. 161-166.
 E. Vassiliadis and P. R. Wood, “Evolution of Lowand Intermediate-Mass Stars to the End of the Asymptotic Giant Branch with Mass Loss,” Astrophysical Journal, Vol. 413, No. 2, 1993, pp. 641-657.
 M. Jura, “RV Tauri Stars as Post Asymptotic Giant Branch Objects,” Astrophysical Journal, Vol. 309, 1986, pp. 732-736.
 M. Morris, “The IRC+10216 Molecular Envelope,” Astrophysical Journal, Vol. 197, No. 3, 1975, pp. 603-610.
 P. Marigo, “Asymptotic Giant Branch Evolution of Varying Surface C/Oration Effects of Changes in Molecular Opacities,” Astronomy and Astrophysics Journal, Vol. 387, 2002, pp. 507-519.
 S. Kwok, “Stellar Evolution from AGB to Planetary Nebulae,” In: The Art of Modelling Stars in 21st Century Proceeding IAU Symposium No. 252, International Astronomical Union, Paris, 2008, pp. 197-203.
 O. DeMarico, “The Origin and Shaping of Planetary Nebulae Putting the Binary Hypothesis to the Test,” Publication of the Astronomical Society of the Pacific, Vol. 121, No. 878, 2009, pp. 316-342.
 H. Umeda, T. Yoshida and K. Takashi, “Massive Star Evolution and Nucleosynthesis: Lower End of Fe-CoreCollapse Supernova Progenitors and Remnant Nutron Star Mass Distribution,” Progress of Theoretical and Experimental Physics, 2012, Article ID: 01A302.
 P. Marigo and L. Girardi, “Evolution of Asymptotic Giant Branch Stars,” Astronomy and Astrophysics Journal, Vol. 482, 2008, pp. 883-905.
 F. Kahn, “Models of Planetary Nebulae Generalization of Multiple Winds Model,” Planetary Nebulae, Vol. 131, 1989, pp. 411-424.
 H. Marten and D. Schonberner, “On the Dynamical Evolution of Planetary Nebulae,” Astronomy and. Astrophysics Journal, Vol. 248, 1991, pp. 590-598.
 N. Socker and M. Livio, “Interacting Winds and Shaping of Planetary Nebulae,” Astrophysical Journal, Vol. 339, 1989, pp. 268-278.
 A. Sundus, “Synthetic Model for Evolution of Plantary Nebulae (PN),” Ph.D. Thesis, University of Baghdad, Baghdad, 2012.
 S. Kwok, “From Red Giants to Planetary Nebulae,” Astrophysical Journal, Vol. 258, 1982, pp. 280-288.
 S. Kwok, “The Origin and Evolution of Planetary Nebulae,” Cambridge University Press, New York, 2000.