The coronal structure of Speedy Mic — I. A densely packed prominence system beyond corotation

• Published in: Monthly notices of the Royal Astronomical Society 2006-01, Vol.365 (2), p.530-538
• Main Authors: Dunstone, N. J., Barnes, J. R., Cameron, A. Collier, Jardine, M.
• Format: Article
• Language: English
• Subjects: Astronomy; circumstellar matter; Corona; Earth, ocean, space; Exact sciences and technology; line: profiles; Magnetic fields; methods: data analysis; Star & galaxy formation; stars: activity; stars: individual: Speedy Mic (HD 197890); stars: late-type
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2005.09729.x

We present new observations of the prominence system on the K3 dwarf Speedy Mic (BO Mic, HD 197890). Using an improved technique to track the absorption features in Hα we find a very active prominence system with approximately 10 prominences on the observable hemisphere per rotation. From a total of 25 prominences, we find an average axial distance of (2.85 ± 0.54) R* which is twice the corotation radius above the stellar surface. We discuss the consequences of these observations on the nature of the supporting magnetic structures. Two consecutive nights, with complete phase coverage, combined with a further night after a three-night gap allow us to study the evolution of the prominence system on two different time-scales. Several of the prominences have counterparts at similar phases on consecutive nights. During this interval, many prominences show evidence for evolution in their heights and phases of observation. Five nights (13 rotation cycles) later, we recover many prominences at approximately the same phases. Whilst individual prominences change axial distances or appear/reappear from night-to-night, the underlying prominence supporting structures appear to be stable over as many as 13 stellar rotations.