SIMBAD references

2013ApJ...778..146O - Astrophys. J., 778, 146 (2013/December-1)

Chemical abundances in the extremely carbon-rich and xenon-rich halo planetary nebula H4-1.

OTSUKA M. and TAJITSU A.

Abstract (from CDS):

We performed detailed chemical abundance analysis of the extremely metal-poor ([Ar/H] ∼ -2) halo planetary nebula (PN) H4-1 based on the multi-wavelength spectra from Subaru/HDS, GALEX, SDSS, and Spitzer/IRS and determined the abundances of 10 elements. The C and O abundances were derived from collisionally excited lines (CELs) and are almost consistent with abundances from recombination lines (RLs). We demonstrated that the large discrepancy in the C abundance between CEL and RL in H4-1 can be solved using the temperature fluctuation model. We reported the first detection of the [Xe III] λ5846 line in H4-1 and determination of its elemental abundance ([Xe/H] > +0.48). H4-1 is the most Xe-rich PN among the Xe-detected PNe. The observed abundances are close to the theoretical prediction by a 2.0 M single star model with an initially element rich ([r/Fe] = +2.0 dex) rapid neutron-capture process (r-process). The observed Xe abundance would be a product of the r-process in primordial supernovae. The [C/O]-[Ba/(Eu or Xe)] diagram suggests that the progenitor of H4-1 shares the evolution with carbon-enhanced metal-poor (CEMP)-r/s and CEMP-no stars. The progenitor of H4-1 is presumably a binary formed in an r-process-rich environment.

Abstract Copyright:

Journal keyword(s): ISM: abundances - planetary nebulae: individual: H4-1

Status at CDS:  

Simbad objects: 14

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2020.05.26-22:56:26

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