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Study of protoplanetary nebulae

Published online by Cambridge University Press:  08 August 2017

D. Estrella ,
L. Hernández-Martínez ,
P. F. Velázquez ,
A. Esquivel  and
C. A. Raga
D. Estrella
Affiliation:
Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México Circuito Exterior S/N – Ciudad Universitaria, Ciudad de México, Distrito Federal – México email: [email protected], [email protected], [email protected], [email protected], [email protected]
L. Hernández-Martínez
Affiliation:
Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México Circuito Exterior S/N – Ciudad Universitaria, Ciudad de México, Distrito Federal – México email: [email protected], [email protected], [email protected], [email protected], [email protected]
P. F. Velázquez
Affiliation:
Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México Circuito Exterior S/N – Ciudad Universitaria, Ciudad de México, Distrito Federal – México email: [email protected], [email protected], [email protected], [email protected], [email protected]
A. Esquivel
Affiliation:
Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México Circuito Exterior S/N – Ciudad Universitaria, Ciudad de México, Distrito Federal – México email: [email protected], [email protected], [email protected], [email protected], [email protected]
C. A. Raga
Affiliation:
Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México Circuito Exterior S/N – Ciudad Universitaria, Ciudad de México, Distrito Federal – México email: [email protected], [email protected], [email protected], [email protected], [email protected]
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Abstract

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We have performed 3D hydrodynamic simulations of a symmetrical jet ejection following previous works (Raga et al. 2009, Riera et al. 2014, Velázquez et al. 2014). The jet is emitted from a binary system in elliptical orbit, and its direction changes describing a precession cone. We have considered that the jet has a time-dependence density ejection or a time-dependence velocity ejection, in order to propose an alternative model to explain the morphology of PPNe’s. Also in our description we have included the effect of the photoionization of the central source. From numerical results, synthetic Hα maps were obtained, and a proper motion study were carried out. We found that the photoionization has an important effect on the case with variation density resulting in a increse in the Hα emission.

Keywords

ISMjets and outflowsnumerical methodsplanetary nebulaeradiation mechanisms
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 373 - 375
Copyright
Copyright © International Astronomical Union 2017 

References

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