Raghvendra Sahai, Christopher K. Chronopoulos
Published 2010-01-27Version 1
We have discovered a very extended shock structure (i.e., with a diameter of about 24 arcmin) surrounding the well-known carbon star IRC+10216 in ultraviolet images taken with the GALEX satellite. We conclude that this structure results from the interaction of IRC+10216's molecular wind with the interstellar medium (ISM), as it moves through the latter. All important structural features expected from theoretical models of such interactions are identified: the termination shock, the astrosheath, the astropause, the bowshock, and an astrotail (with vortices). The extent of the astropause provides new lower limits to the envelope age (69,000 years) and mass (1.4 solar masses, for a mass-loss rate of 2 x 10^(-5) solar masses/year). From the termination-shock standoff distance, we find that IRC+10216 is moving at a speed of about > 91 km/s [1 cm^(-3)/n_(ISM)]^1/2 through the local ISM.
Comments: 4 pages, 3 color figures; accepted for Astrophysical Journal (Letters)
The extended molecular envelope of the asymptotic giant branch star $π^{1}$ Gruis as seen by ALMA I. Large-scale kinematic structure and CO excitation properties
The extended molecular envelope of the asymptotic giant branch star $π^{1}$ Gruis as seen by ALMA II. The spiral-outflow observed at high-angular resolution
Spectroscopic and Photometric Study of the Asymptotic Giant Branch Star T Cephei
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