On the possible existence of short-period g-mode instabilities powered by nuclear-burning shells in post-asymptotic giant branch h-deficient (PG1159-TYPE) stars
dc.contributor.author | Córsico, Alejandro Hugo | pt_BR |
dc.contributor.author | Althaus, Leandro Gabriel | pt_BR |
dc.contributor.author | Bertolami, Marcelo Miguel Miller | pt_BR |
dc.contributor.author | Gonzalez Perez, Jose Miguel | pt_BR |
dc.contributor.author | Kepler, Souza Oliveira | pt_BR |
dc.date.accessioned | 2015-01-15T02:15:13Z | pt_BR |
dc.date.issued | 2009 | pt_BR |
dc.identifier.issn | 0004-637X | pt_BR |
dc.identifier.uri | http://hdl.handle.net/10183/108979 | pt_BR |
dc.description.abstract | We present a pulsational stability analysis of hot post-asymptotic giant branch (AGB) H-deficient pre-white dwarf stars with active He-burning shells. The stellar models employed are state-of-the-art equilibrium structures representative of PG1159 stars derived from the complete evolution of the progenitor stars, through the thermally pulsing AGB phase and born-again episode. On the basis of fully nonadiabatic pulsation computations, we confirmed theoretical evidence for the existence of a separate PG1159 instability strip in the log Teff–log g diagram characterized by short-period g-modes excited by the -mechanism. This instability strip partially overlaps the already known GW Vir instability strip of intermediate/long-period g-modes destabilized by the classical κ-mechanism acting on the partial ionization of C and/or O in the envelope of PG1159 stars. We found that PG1159 stars characterized by thick He-rich envelopes and located inside this overlapping region could exhibit both short and intermediate/ long periods simultaneously. As a natural application of our results, we study the particular case of VV 47, a pulsating planetary nebula nucleus (PG1159 type) that is particularly interesting because it has been reported to exhibit a rich and complex pulsation spectrum including a series of unusually short pulsation periods.We found that the long periods exhibited byVV47 can be readily explained by the classical κ-mechanism,while the observed shortperiod branch below ≈300 s could correspond to modes triggered by the He-burning shell through the ε-mechanism, although more observational work is needed to confirm the reality of these short-period modes. Were the existence of short-period g-modes in this star convincingly confirmed by future observations, VV 47 could be the first known pulsating star in which both the κ-mechanism and the ε-mechanism of mode driving are simultaneously operating. | en |
dc.format.mimetype | application/pdf | |
dc.language.iso | eng | pt_BR |
dc.relation.ispartof | The astrophysical journal. Bristol. Vol. 701, no. 2 (Aug. 2009), p. 1008-1014 | pt_BR |
dc.rights | Open Access | en |
dc.subject | Stars: evolution | en |
dc.subject | Evolucao estelar | pt_BR |
dc.subject | Pulsacoes estelares | pt_BR |
dc.subject | Stars: individual (VV 47) | en |
dc.subject | Stars: interiors | en |
dc.subject | Nebulosas planetarias | pt_BR |
dc.subject | Estrelas supergigantes | pt_BR |
dc.subject | Stars: oscillations | en |
dc.subject | White dwarfs | en |
dc.title | On the possible existence of short-period g-mode instabilities powered by nuclear-burning shells in post-asymptotic giant branch h-deficient (PG1159-TYPE) stars | pt_BR |
dc.type | Artigo de periódico | pt_BR |
dc.identifier.nrb | 000766130 | pt_BR |
dc.type.origin | Estrangeiro | pt_BR |
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