The pre-shock gas of SN1006 from HST/ACS observations

Details The pre-shock gas of SN1006 from HST/ACS observations The pre-shock gas of SN1006 from HST/ACS observations

2007-01-10

arxiv.org/abs/astro-ph/0701311v1

Astrophys.J.659:1257-1264,2007

Astronomy and Astrophysics

Astrophysics

16 pages, 6 figures, to appear in ApJ

Scientific paper

10.1086/512483

We derive the pre-shock density and scale length along the line of sight for the collisionless shock from a deep HST image that resolves the H alpha filament in SN1006 and updated model calculations. The very deep ACS high-resolution image of the Balmer line filament in the northwest (NW) quadrant shows that 0.25 < n_0 < le$ 0.4 cm-3 and that the scale along the line of sight is about 2 x 10^{18} cm, while bright features within the filament correspond to ripples with radii of curvature less than 1/10 that size. The derived densities are within the broad range of earlier density estimates, and they agree well with the ionization time scale derived from the Chandra X-ray spectrum of a region just behind the optical filament. This provides a test for widely used models of the X-ray emission from SNR shocks. The scale and amplitude of the ripples are consistent with expectations for a shock propagating though interstellar gas with ~ 20% density fluctuations on parsec scales as expected from studies of interstellar turbulence. One bulge in the filament corresponds to a knot of ejecta overtaking the blast wave, however. The interaction results from the rapid deceleration of the blast wave as it encounters an interstellar cloud.

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