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- W3105404493 abstract "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." @default.
- W3105404493 created "2020-11-23" @default.
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- W3105404493 date "2013-11-12" @default.
- W3105404493 modified "2023-10-14" @default.
- W3105404493 title "CHEMICAL ABUNDANCES IN THE EXTREMELY CARBON-RICH AND XENON-RICH HALO PLANETARY NEBULA H4-1" @default.
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- W3105404493 doi "https://doi.org/10.1088/0004-637x/778/2/146" @default.
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