Add to ORKGUsing two-dimensional hydrodynamical simulations, we investigate the interaction of a collimated fast wind (CFW) interacting with a spherical asymptotic giant branch (AGB) wind as the mechanism for shaping proto-planetary nebulae and young planetary nebulae. In particular, we compare our simulations to the observations of an evolved PPN with multiple, highly collimated lobes, CRL 618
Proceedings of the International Astronomical Union, 2008, v. 4 n. S252, p. 197-203Planetary nebulae...
Abstract. Proto-planetary nebulae (pPN) and planetary nebulae (PN) seem to be formed by interacting ...
We present results of a series of magnetohydrodynamic (MHD) and hydrodynamic (HD) 2.5 dimensional si...
(abridged) The interaction of a fast wind with a spherical Asymptotic Giant Branch (AGB) wind is tho...
We calculate the X-ray emission from both constant and time evolving shocked fast winds blown by the...
We present hydrodynamical models of planetary nebulae with detached binary cores. The models are obt...
To understand how the circumstellar environments of post-Active Giant Branch (AGB) stars develop int...
The morphologies of planetary nebula have long been believed to be due to wind shaping processes in ...
In this paper we present optical long-slit spectroscopy and imaging of the proto-planetary nebula CR...
Interaction with the Interstellar Medium (ISM) cannot be ignored in understanding planetary nebula (...
The stellar winds of the central stars of planetary nebulae play an essential role in the shaping of...
Context. Massive stars shape their surrounding medium through the force of their stellar winds, whic...
We discuss the interaction of the slow wind blown by an asymptotic giant branch (AGB) star with a co...
Sh 2-188 is an example of strong interaction between a planetary nebula (PN) and the interstellar me...
In this paper we explore the dynamics of ionization bounded planetary nebulae after the termination ...
Proceedings of the International Astronomical Union, 2008, v. 4 n. S252, p. 197-203Planetary nebulae...
Abstract. Proto-planetary nebulae (pPN) and planetary nebulae (PN) seem to be formed by interacting ...
We present results of a series of magnetohydrodynamic (MHD) and hydrodynamic (HD) 2.5 dimensional si...
(abridged) The interaction of a fast wind with a spherical Asymptotic Giant Branch (AGB) wind is tho...
We calculate the X-ray emission from both constant and time evolving shocked fast winds blown by the...
We present hydrodynamical models of planetary nebulae with detached binary cores. The models are obt...
To understand how the circumstellar environments of post-Active Giant Branch (AGB) stars develop int...
The morphologies of planetary nebula have long been believed to be due to wind shaping processes in ...
In this paper we present optical long-slit spectroscopy and imaging of the proto-planetary nebula CR...
Interaction with the Interstellar Medium (ISM) cannot be ignored in understanding planetary nebula (...
The stellar winds of the central stars of planetary nebulae play an essential role in the shaping of...
Context. Massive stars shape their surrounding medium through the force of their stellar winds, whic...
We discuss the interaction of the slow wind blown by an asymptotic giant branch (AGB) star with a co...
Sh 2-188 is an example of strong interaction between a planetary nebula (PN) and the interstellar me...
In this paper we explore the dynamics of ionization bounded planetary nebulae after the termination ...
Proceedings of the International Astronomical Union, 2008, v. 4 n. S252, p. 197-203Planetary nebulae...
Abstract. Proto-planetary nebulae (pPN) and planetary nebulae (PN) seem to be formed by interacting ...
We present results of a series of magnetohydrodynamic (MHD) and hydrodynamic (HD) 2.5 dimensional si...