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The wonderful complexity of the Mira AB system

S. Ramstedt ; S. Mohamed ; Wouter Vlemmings (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; Matthias Maercker (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; R. Montez ; A. Baudry ; Elvire De Beck (Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium) ; Michael Lindqvist (Institutionen för rymd- och geovetenskap, Onsala rymdobservatorium) ; Hans Olofsson (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; E. M. L. Humphreys ; A. Jorissen ; F. Kerschbaum ; A. Mayer ; M. Wittkowski ; N. L. J. Cox ; E. Lagadec ; M. L. Leal-Ferreira ; C. Paladini ; A. Perez-Sanchez ; S. Sacuto
Astronomy and Astrophysics (0004-6361). Vol. 570 (2014), p. Art. no. L14.
[Artikel, refereegranskad vetenskaplig]

We have mapped the (CO)-C-12(3-2) line emission around the Mira AB system at 0 ''.5 resolution using the Atacama Large Millimeter/submillimeter Array (ALMA). The CO map shows amazing complexity. The circumstellar gas has been shaped by different dynamical actors during the evolution of the system, and several morphological components can be identified. The companion is marginally resolved in continuum emission and is currently at 0 ''.487 +/- 0 ''.006 separation. In the main line component, centered on the stellar velocity, spiral arcs around Mira A are found. The spiral appears to be relatively flat and oriented in the orbital plane. An accretion wake behind the companion is clearly visible, and the projected arc separation is about 5 ''. In the blue wing of the line emission, offset from the main line, several large (similar to 5-10 '') opposing arcs are found. We tentatively suggest that this structure is created by the wind of Mira B blowing a bubble in the expanding envelope of Mira A.

Nyckelord: stars: AGB and post-AGB, binaries: symbiotic, circumstellar matter, submillimeter: stars



Denna post skapades 2014-12-08. Senast ändrad 2016-11-09.
CPL Pubid: 207680

 

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Magnetic fields and the outflows during the formation and evolution of stars (OUTFLOWMAGN) (EC/FP7/614264)