Is Mira a magneto-dusty rotator?
Abstract
We investigate the possibility that a magnetic field may be present in the star o-Ceti (hereafter Mira) and that the field plays a role in the star's mass loss. The model presented here is an application of an earlier derived theory that has been successfully applied for modelling the wind of a generic intermediate-mass asymptotic giant branch (AGB) star and that of the red supergiant star Betelgeuse, and is now extended to the low-mass end AGB stars, Mira. The modelling shows that it is possible to obtain a hybrid magnetohydrodynamic-dust-driven wind scenario for Mira, in which the magnetic field in the equatorial plane of the star is dynamically important for producing a stellar wind. The wind velocity and the temperatures obtained from the model appear consistent with observational findings elsewhere.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- April 2013
- DOI:
- 10.1093/mnras/sts716
- arXiv:
- arXiv:1206.0044
- Bibcode:
- 2013MNRAS.430.1359T
- Keywords:
-
- MHD;
- stars: AGB and post-AGB;
- stars: individual: Mira (o-Ceti);
- stars: winds;
- outflows;
- Astrophysics - Solar and Stellar Astrophysics
- E-Print:
- 5 pages, 2 figures