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The kinematical behavior of ORLs and CELs in PNe with [WC] central star

Published online by Cambridge University Press:  08 August 2017

Miriam Peña ,
Francisco Ruiz-Escobedo ,
Jackeline Rechy-García  and
Jorge García-Rojas
Miriam Peña
Affiliation:
Instituto de Astronomia, UNAM, México email: [email protected], [email protected], [email protected]
Francisco Ruiz-Escobedo
Affiliation:
Instituto de Astronomia, UNAM, México email: [email protected], [email protected], [email protected]
Jackeline Rechy-García
Affiliation:
Instituto de Astrofisica de Canarias, La Laguna, Spain email: [email protected]
Jorge García-Rojas
Affiliation:
Instituto de Astrofisica de Canarias, La Laguna, Spain email: [email protected]
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Abstract

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In Planetary Nebulae (PNe) and HII regions ionic abundances can be derived by using collisionally excited lines (CELs) or recombination lines (ORLs). Such abundances do not coincide for the same ion and usually abundances from ORLs are larger than those from CELs by factors of 2 or larger. The origin of the discrepancy, known as the Abundance Discrepancy Factor is an open problem in astrophysics of gaseous nebulae. It has been attributed to temperature fluctuations in the plasma, tiny metal-rich inclusions embedded in the H-rich plasma, gas inhomogeneities or other processes. In this work we analyze the kinematical behavior of CELs and ORLs in two PNe ionized by [WC] stars, finding that kinematics of ORLS is incompatible with the kinematics of CELs. In particular the expansion velocities from CELs and ORLs for the same ion are different, indicating that ORLs seem to be produced in zones nearer the central star than CELs. This is in agreement with results found by other authors for individual PNe.

Keywords

planetary nebulae: generalkinematics and dynamicsplanetary nebulae: individual: (Cn 1-5, PC 14)
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. 60 - 64
Copyright
Copyright © International Astronomical Union 2017 

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