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Pulsation of AGB stars in the Small Magellanic Cloud cluster NGC 419

Kamath, Devika; Wood, Peter R; Soszyński, Igor; Lebzelter, Thomas

Description

The intermediate-age Magellanic Cloud clusters NGC 1978 and 419 are each found to contain substantial numbers of pulsating asymptotic giant branch (AGB) stars, both oxygen rich and carbon rich. Each cluster also contains two pulsating AGB stars which are infrared sources with a large mass-loss rate. Pulsation masses have been derived for the AGB variables, from the lowest luminosity O-rich variables to the most evolved infrared sources. It is found that the stars in NGC 1978 have a mass of 1.55...[Show more]

dc.contributor.authorKamath, Devika
dc.contributor.authorWood, Peter R
dc.contributor.authorSoszyński, Igor
dc.contributor.authorLebzelter, Thomas
dc.date.accessioned2015-12-08T22:48:06Z
dc.identifier.issn0037-8720
dc.identifier.urihttp://hdl.handle.net/1885/38207
dc.description.abstractThe intermediate-age Magellanic Cloud clusters NGC 1978 and 419 are each found to contain substantial numbers of pulsating asymptotic giant branch (AGB) stars, both oxygen rich and carbon rich. Each cluster also contains two pulsating AGB stars which are infrared sources with a large mass-loss rate. Pulsation masses have been derived for the AGB variables, from the lowest luminosity O-rich variables to the most evolved infrared sources. It is found that the stars in NGC 1978 have a mass of 1.55 M. early on the AGB while the NGC 419 stars have a mass of 1.87 M. early on the AGB. These masses are in good agreement with those expected from the cluster ages determined by main-sequence turn-off fitting. Non-linear pulsation models fitted to the highly evolved AGB stars show that a substantial amount of mass-loss has occurred during the AGB evolution of these stars. An examination of the observed mass-loss on the AGB, and the AGB tip luminosities, shows that in both clusters the mass-loss rates computed from the formula of Vassiliadis & Wood reproduce the observations reasonably well. The mass-loss rates computed from the formula of Bl�cker terminate the AGB in both clusters at a luminosity which is much too low. � 2010 The Authors. Journal compilation � 2010 RAS.
dc.publisherSocieta Astronomica Italiana
dc.sourceMemorie Della Societa Astronomica Italiana
dc.titlePulsation of AGB stars in the Small Magellanic Cloud cluster NGC 419
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume81
dc.date.issued2010
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.ariespublicationu3356449xPUB159
local.type.statusPublished Version
local.contributor.affiliationKamath, Devika, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationWood, Peter R, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationSoszyński, Igor, Warsaw University Observatory
local.contributor.affiliationLebzelter, Thomas, University of Vienna
local.description.embargo2037-12-31
local.bibliographicCitation.startpage1078
local.bibliographicCitation.lastpage1082
dc.date.updated2015-12-08T11:03:34Z
CollectionsANU Research Publications

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