Dynamical and ionization structure of planetary nebulae in three dimensions. A simulation for NGC3132

Details Dynamical and ionization structure of planetary nebulae in three dimensions. A simulation for NGC3132 Dynamical and ionization structure of planetary nebulae in three dimensions. A simulation for NGC3132

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003ap%26ss.288..465k&link_type=abstract

Astrophysics and Space Science, v. 288, Issue 4, p. 465-482 (2003).

Astronomy and Astrophysics

Astrophysics

Scientific paper

Using a numerically accurate radiation-gasdynamical method we investigate the winds scenario for aspherical planetary nebulae (PNe). Our model includes the interaction of two winds: a slow high mass-loss rate wind (a `super wind'); and a fast wind; low mass-loss rate wind. Our model also includes the evolution of the UV spectrum of the PNe centeral star. As stated in the section 3 of Paper I (Ganbari and Khesali, 2001), we consider a three dimensional density distribution ρ(r,θφ for the super wind,in this way we enter the effects of cooling and heating mechanisms in our model. Taking into account the above assumptions,we introduce the code (DIS3D) and numerically we study the dynamical and ionization properties of the planetary nebula NGC3132. We show that it is possible by simulations to reproduce the shape of PNe in three dimensions, and calculating the physical quantities throughout the entire nebula.

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