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Article: Circumstellar CO in metal-poor stellar winds: the highly irradiated globular cluster star 47 Tucanae V3

TitleCircumstellar CO in metal-poor stellar winds: the highly irradiated globular cluster star 47 Tucanae V3
Authors
Keywordsstars: AGB and post-AGB
circumstellar matter
stars: mass-loss
stars: winds
outflows
Issue Date2019
PublisherOxford University Press. The Journal's web site is located at https://academic.oup.com/mnrasl/
Citation
Monthly Notices of the Royal Astronomical Society: Letters, 2019, v. 484 n. 1, p. L85-L89 How to Cite?
AbstractWe report the first detection of circumstellar CO in a globular cluster. Observations with ALMA have detected the CO J = 3–2 and SiO v = 1 J = 8 − 7 transitions at 345 and 344 GHz, respectively, around V3 in 47 Tucanae (NGC 104; [Fe/H] = –0.72 dex), a star on the asymptotic giant branch. The CO line is detected at 7σ at a rest velocity vLSR = –40.6 km s−1 and expansion velocity of 3.2 ± ∼0.4 km s−1. The brighter, asymmetric SiO line may indicate a circumstellar maser. The stellar wind is slow compared to similar Galactic stars, but the dust opacity remains similar to Galactic comparisons. We suggest that the mass-loss rate is set by the levitation of material into the circumstellar environment by pulsations, but that the terminal wind-expansion velocity is determined by radiation pressure on the dust: a pulsation-enhanced dust-driven wind. We suggest the metal-poor nature of the star decreases the grain size, slowing the wind and increasing its density and opacity. Metallic alloys at high altitudes above the photosphere could also provide an opacity increase. The CO line is weaker than expected from Galactic AGB stars, but its strength confirms a model that includes CO dissociation by the strong interstellar radiation field present inside globular clusters.
Persistent Identifierhttp://hdl.handle.net/10722/278607
ISSN
2023 SCImago Journal Rankings: 1.521
ISI Accession Number ID

 

DC FieldValueLanguage
dc.contributor.authorMcDonald, I-
dc.contributor.authorBoyer, ML-
dc.contributor.authorGroenewegen, MAT-
dc.contributor.authorLagadec, E-
dc.contributor.authorRichards, AMS-
dc.contributor.authorSloan, GC-
dc.contributor.authorZijlstra, AA-
dc.date.accessioned2019-10-21T02:10:40Z-
dc.date.available2019-10-21T02:10:40Z-
dc.date.issued2019-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society: Letters, 2019, v. 484 n. 1, p. L85-L89-
dc.identifier.issn1745-3925-
dc.identifier.urihttp://hdl.handle.net/10722/278607-
dc.description.abstractWe report the first detection of circumstellar CO in a globular cluster. Observations with ALMA have detected the CO J = 3–2 and SiO v = 1 J = 8 − 7 transitions at 345 and 344 GHz, respectively, around V3 in 47 Tucanae (NGC 104; [Fe/H] = –0.72 dex), a star on the asymptotic giant branch. The CO line is detected at 7σ at a rest velocity vLSR = –40.6 km s−1 and expansion velocity of 3.2 ± ∼0.4 km s−1. The brighter, asymmetric SiO line may indicate a circumstellar maser. The stellar wind is slow compared to similar Galactic stars, but the dust opacity remains similar to Galactic comparisons. We suggest that the mass-loss rate is set by the levitation of material into the circumstellar environment by pulsations, but that the terminal wind-expansion velocity is determined by radiation pressure on the dust: a pulsation-enhanced dust-driven wind. We suggest the metal-poor nature of the star decreases the grain size, slowing the wind and increasing its density and opacity. Metallic alloys at high altitudes above the photosphere could also provide an opacity increase. The CO line is weaker than expected from Galactic AGB stars, but its strength confirms a model that includes CO dissociation by the strong interstellar radiation field present inside globular clusters.-
dc.languageeng-
dc.publisherOxford University Press. The Journal's web site is located at https://academic.oup.com/mnrasl/-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society: Letters-
dc.rightsPre-print: Journal Title] ©: [year] [owner as specified on the article] Published by Oxford University Press [on behalf of xxxxxx]. All rights reserved. Pre-print (Once an article is published, preprint notice should be amended to): This is an electronic version of an article published in [include the complete citation information for the final version of the Article as published in the print edition of the Journal.] Post-print: This is a pre-copy-editing, author-produced PDF of an article accepted for publication in [insert journal title] following peer review. The definitive publisher-authenticated version [insert complete citation information here] is available online at: xxxxxxx [insert URL that the author will receive upon publication here].-
dc.subjectstars: AGB and post-AGB-
dc.subjectcircumstellar matter-
dc.subjectstars: mass-loss-
dc.subjectstars: winds-
dc.subjectoutflows-
dc.titleCircumstellar CO in metal-poor stellar winds: the highly irradiated globular cluster star 47 Tucanae V3-
dc.typeArticle-
dc.identifier.emailZijlstra, AA: zijlstra@hku.hk-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1093/mnrasl/slZ009-
dc.identifier.scopuseid_2-s2.0-85062194597-
dc.identifier.hkuros307434-
dc.identifier.volume484-
dc.identifier.issue1-
dc.identifier.spageL85-
dc.identifier.epageL89-
dc.identifier.isiWOS:000482180300018-
dc.publisher.placeUnited Kingdom-

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