Evolution and nucleosynthesis of helium-rich asymptotic giant branch models
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Shingles, Luke; Doherty, Carolyn L; Karakas, Amanda; Stancliffe, R J; Lattanzio, John; Lugaro, Maria
Description
There is now strong evidence that some stars have been born with He mass fractions as high as Y≈0.40 (e.g. in ω Centauri). However, the advanced evolution, chemical yields, and final fates of He-rich stars are largely unexplored. We investigate the consequences of He-enhancement on the evolution and nucleosynthesis of intermediate-mass asymptotic giant branch (AGB) models of 3, 4, 5, and 6 M⊙ with a metallicity of Z = 0.0006 ([Fe/H] ≈-1.4). We compare models with He-enhanced compositions (Y =...[Show more]
dc.contributor.author | Shingles, Luke | |
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dc.contributor.author | Doherty, Carolyn L | |
dc.contributor.author | Karakas, Amanda | |
dc.contributor.author | Stancliffe, R J | |
dc.contributor.author | Lattanzio, John | |
dc.contributor.author | Lugaro, Maria | |
dc.date.accessioned | 2016-06-14T23:20:23Z | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.uri | http://hdl.handle.net/1885/103358 | |
dc.description.abstract | There is now strong evidence that some stars have been born with He mass fractions as high as Y≈0.40 (e.g. in ω Centauri). However, the advanced evolution, chemical yields, and final fates of He-rich stars are largely unexplored. We investigate the consequences of He-enhancement on the evolution and nucleosynthesis of intermediate-mass asymptotic giant branch (AGB) models of 3, 4, 5, and 6 M⊙ with a metallicity of Z = 0.0006 ([Fe/H] ≈-1.4). We compare models with He-enhanced compositions (Y = 0.30, 0.35, 0.40) to those with primordial-He (Y = 0.24). We find that the minimum initial mass for C burning and super-AGB stars with CO(Ne) or ONe cores decreases from above our highest mass of 6 to ~4-5M⊙ with Y = 0.40. We also model the production of trans-Fe elements via the slow neutron-capture process (sprocess). He-enhancement substantially reduces the third dredge-up efficiency and the stellar yields of s-process elements (e.g. 90 per cent less Ba for 6 M⊙, Y = 0.40). An exception occurs for 3 M⊙, where the near-doubling in the number of thermal pulses with Y = 0.40 leads to ~50 per cent higher yields of Ba-peak elements and Pb if the 13C neutron source is included. However, the thinner intershell and increased temperatures at the base of the convective envelope with Y = 0.40 probably inhibit the 13C neutron source at this mass. Future chemical evolution models with our yields might explain the evolution of s-process elements among He-rich stars in ω Centauri. | |
dc.publisher | Blackwell Publishing Ltd | |
dc.source | Monthly Notices of the Royal Astronomical Society | |
dc.title | Evolution and nucleosynthesis of helium-rich asymptotic giant branch models | |
dc.type | Journal article | |
local.description.notes | Imported from ARIES | |
local.identifier.citationvolume | 452 | |
dc.date.issued | 2015 | |
local.identifier.absfor | 020100 - ASTRONOMICAL AND SPACE SCIENCES | |
local.identifier.absfor | 020110 - Stellar Astronomy and Planetary Systems | |
local.identifier.ariespublication | U3488905xPUB6611 | |
local.type.status | Published Version | |
local.contributor.affiliation | Shingles, Luke, College of Physical and Mathematical Sciences, ANU | |
local.contributor.affiliation | Doherty, Carolyn L, Monash University | |
local.contributor.affiliation | Karakas, Amanda, College of Physical and Mathematical Sciences, ANU | |
local.contributor.affiliation | Stancliffe, R J, Universitat Bonn | |
local.contributor.affiliation | Lattanzio, John, Monash University | |
local.contributor.affiliation | Lugaro, Maria, Hungarian Academy of Sciences | |
local.description.embargo | 2037-12-31 | |
local.bibliographicCitation.issue | 3 | |
local.bibliographicCitation.startpage | 2804 | |
local.bibliographicCitation.lastpage | 2821 | |
local.identifier.doi | 10.1093/mnras/stv1489 | |
dc.date.updated | 2016-06-14T08:48:42Z | |
local.identifier.scopusID | 2-s2.0-84945299182 | |
Collections | ANU Research Publications |
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