Turbulent Entrainment in Mira's Cometary Tail

Details Turbulent Entrainment in Mira's Cometary Tail Turbulent Entrainment in Mira's Cometary Tail

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...685l.141r&link_type=abstract

The Astrophysical Journal, Volume 685, Issue 2, pp. L141-L144.

Astronomy and Astrophysics

Astronomy

12

Stars: Circumstellar Matter, Hydrodynamics, Ism: Jets And Outflows, Stars: Agb And Post-Agb, Stars: Individual (Mira)

Scientific paper

Mira is a red giant star which passes through the Galactic ISM, leaving behind a cometary tail extending over ~2° (seen in the spectacular UV image of Martin and coworkers). H I 21 cm emission from this cometary tail has now also been detected. The 21 cm emission shows a velocity that decreases monotonically with increasing distances from Mira (along the axis of the cometary tail). We present a ``turbulent wake'' model which gives a simple, analytic prediction for the velocity of the material in the wake as a function of distance from the stellar wind source. We fit this predicted velocity versus position law to the velocities deduced from the 21 cm observations, and find that a wake with a half-opening angle of ~11.8° (and a stellar motion and wind velocity/mass-loss rate corresponding to the values determined for Mira) reproduces the observations.

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