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The rapid evolution of the born-again giant Sakurai’s object

Asplund, Martin; Lambert, David L; Kipper, T; Pollacco, D; Shetrone, M.D

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The extraordinarily rapid evolution of the born-again giant Sakurai’s object following discovery in 1996 has been investigated. The evolution can be traced both in a continued cooling of the stellar surface and dramatic changes in chemical composition on a timescale of a mere few months. The abundance alterations are the results of the mixing and nuclear reactions which have ensued due to the final He-shell flash which occurred during the descent along the white dwarf cooling track. The...[Show more]

dc.contributor.authorAsplund, Martin
dc.contributor.authorLambert, David L
dc.contributor.authorKipper, T
dc.contributor.authorPollacco, D
dc.contributor.authorShetrone, M.D
dc.date.accessioned2002-12-18
dc.date.accessioned2004-05-19T04:53:17Z
dc.date.accessioned2011-01-05T08:42:13Z
dc.date.available2004-05-19T04:53:17Z
dc.date.available2011-01-05T08:42:13Z
dc.date.created1999
dc.identifier.urihttp://hdl.handle.net/1885/40068
dc.identifier.urihttp://digitalcollections.anu.edu.au/handle/1885/40068
dc.description.abstractThe extraordinarily rapid evolution of the born-again giant Sakurai’s object following discovery in 1996 has been investigated. The evolution can be traced both in a continued cooling of the stellar surface and dramatic changes in chemical composition on a timescale of a mere few months. The abundance alterations are the results of the mixing and nuclear reactions which have ensued due to the final He-shell flash which occurred during the descent along the white dwarf cooling track. The observed changes in the H and Li abundances can be explained by ingestion and burning of the H-rich envelope and Li-production through the Cameron-Fowler mechanism. The rapidly increasing abundances of the light s-elements (including Sc) are consistent with current s-processing by neutrons released from the concomitantly produced 13C. However, the possibility that the s-elements have previously been synthesized during the AGB-phase and only mixed to the surface in connection with the final He-shell flash in the pre-white dwarf cannot be convincingly ruled out either. Since Sakurai’s object shows substantial abundance similarities with the R CrB stars and has recently undergone R CrB-like visual fading events, the “birth” of an R CrB star may have been witnessed for the first time ever. Sakurai’s object thus lends strong support for the suggestion that at least some of the R CrB stars have been formed through a final He-shell flash in a post-AGB star.
dc.format.extent314439 bytes
dc.format.mimetypeapplication/pdf
dc.language.isoen_AU
dc.subjectstars: variables: general
dc.subjectstars: individual: Sakurai's Object
dc.subjectV4334 Sgr
dc.subjectstars: AGB and post-AGB
dc.subjectstars: evolution
dc.subjectstars: abundances
dc.titleThe rapid evolution of the born-again giant Sakurai’s object
dc.typeJournal article
local.description.refereedyes
local.identifier.citationpages507-518
local.identifier.citationpublicationAstronomy and Astrophysics
local.identifier.citationvolume343
local.identifier.citationyear1999
local.identifier.eprintid752
local.rights.ispublishedyes
dc.date.issued1999
CollectionsANU Research Publications

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