Circumstellar CO in metal-poor stellar winds: the highly irradiated globular cluster star 47 Tucanae V3. (18th January 2019)

• Record Type: Journal Article
• Authors: McDonald, I; Boyer, M L; Groenewegen, M A T; Lagadec, E; Richards, A M S; Sloan, G C; Zijlstra, A A
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 484:Number 1(2019)
• Page Start: L85
• Page End: L89
• Publication Date: 2019-01-18
• Subjects: stars: AGB and post-AGB -- circumstellar matter -- stars: mass-loss -- stars: winds, outflows -- globular clusters: individual: NGC 104 -- infrared: stars; Astronomy -- Research -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnrasl/slZ009
• Languages: English
• ISSNs: 1745-3933

Abstract

ABSTRACT: We 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 v LSR = –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.