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Title:
The Preshock Gas of SN 1006 from Hubble Space Telescope Advanced Camera for Surveys Observations
Authors:
Raymond, J. C.; Korreck, K. E.; Sedlacek, Q. C.; Blair, W. P.; Ghavamian, P.; Sankrit, R.
Affiliation:
AA(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138.), AD(Johns Hopkins University, Baltimore, MD.), AE(Johns Hopkins University, Baltimore, MD.), AF(Space Sciences Laboratory, University of California, Berkeley, CA.)
Publication:
The Astrophysical Journal, Volume 659, Issue 2, pp. 1257-1264. (ApJ Homepage)
Publication Date:
04/2007
Origin:
UCP
ApJ Keywords:
ISM: Individual: Alphanumeric: SN 1006, Shock Waves, ISM: Supernova Remnants
DOI:
10.1086/512483
Bibliographic Code:
2007ApJ...659.1257R

Abstract

We derive the preshock density and scale length along the line of sight for the collisionless shock from a deep HST image that resolves the Hα filament in SN 1006 and updated model calculations. The very deep ACS high-resolution image of the Balmer line filament in the northwest quadrant shows that 0.25 cm-3<=n0<=0.4 cm-3 and that the scale along the line of sight is about 2×1018 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 timescale 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 through 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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