A model of Mira's cometary head/tail entering the Local Bubble

Details A model of Mira's cometary head/tail entering the Local Bubble A model of Mira's cometary head/tail entering the Local Bubble

2010-10-15

arxiv.org/abs/1010.3167v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

12 pages, 8 figures (4 in color). Accepted for publication in The Astrophysical Journal

Scientific paper

We model the cometary structure around Mira as the interaction of an AGB wind from Mira A, and a streaming environment. Our simulations introduce the following new element: we assume that after 200 kyr of evolution in a dense environment Mira entered the Local Bubble (low density coronal gas). As Mira enters the bubble, the head of the comet expands quite rapidly, while the tail remains well collimated for a 100 kyr timescale. The result is a broad-head/narrow-tail structure that resembles the observed morphology of Mira's comet. The simulations were carried out with our new adaptive grid code WALICXE, which is described in detail.

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