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Resolving the stellar activity of the Mira AB binary with ALMA

Wouter Vlemmings (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; S. Ramstedt ; Eamon O'Gorman (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik) ; E. M. L. Humphreys ; M. Wittkowski ; A. Baudry ; M. Karovska
Astronomy and Astrophysics (0004-6361). Vol. 577 (2015),
[Artikel, refereegranskad vetenskaplig]

Aims. We present the size, shape, and flux densities at millimeter continuum wavelengths, based on ALMA science verification observations in Band 3 (similar to 94.6 GHz) and Band 6 (similar to 228.7 GHz), from the binary Mira A (o Ceti) and Mira B. Methods. The Mira AB system was observed with ALMA at a spatial resolution down to similar to 25 mas. The extended atmosphere of Mira A and the wind around Mira B sources were resolved, and we derived the sizes of Mira A and of the ionized region around Mira B. The spectral indices within Band 3 (between 89-100 GHz) and between Bands 3 and 6 were also derived. Results. The spectral index of Mira A is found to change from 1.71 +/- 0.05 within Band 3 to 1.54 +/- 0.04 between Bands 3 and 6. The spectral index of Mira B is 1.3 +/- 0.2 in Band 3, in good agreement with measurements at longer wavelengths; however, it rises to 1.72 +/- 0.11 between the bands. For the first time, the extended atmosphere of a star is resolved at these frequencies, and for Mira A the diameter is similar to 3.8 x 3.2 AU in Band 3 (with brightness temperature T-b similar to 5300 K) and similar to 4.0 x 3.6 AU in Band 6 (T-b similar to 2500 K). Additionally, a bright hotspot similar to 0.4 AU, with T-b similar to 10 000 K, is found on the stellar disk of Mira A. The size of the ionized region around the accretion disk of Mira B is found to be similar to 2.4 AU. Conclusions. The emission around Mira B is consistent with emission from a partially ionized wind of gravitationally bound material from Mira A close to the accretion disk of Mira B. The Mira A atmosphere does not fully match predictions with brightness temperatures in Band 3 significantly higher than expected, potentially owing to shock heating. The hotspot is very likely due to magnetic activity and could be related to the previously observed X-ray flare of Mira A.

Nyckelord: stars: AGB and post-AGB, stars: atmospheres, binaries: close, stars: individual: Mira AB



Denna post skapades 2015-08-07. Senast ändrad 2016-02-04.
CPL Pubid: 220363

 

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Projekt

Denna publikation är ett resultat av följande projekt:


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