Kazimierz J. Borkowski et al 2006 ApJ 642 L141 doi:10.1086/504472
Dust Destruction in Type Ia Supernova Remnants in the Large Magellanic Cloud
FREEKazimierz J. Borkowski1, Brian J. Williams1, Stephen P. Reynolds1, William P. Blair2, Parviz Ghavamian2, Ravi Sankrit2, Sean P. Hendrick3, Knox S. Long4, John C. Raymond5, R. Chris Smith6, Sean Points6 and P. Frank Winkler7
Show affiliationsWe present first results from an extensive survey of Magellanic Cloud supernova remnants (SNRs) with the Spitzer Space Telescope. We describe IRAC and MIPS imaging observations at 3.6, 4.5, 5.8, 8, 24, and 70 μm of four Balmer-dominated Type Ia SNRs in the Large Magellanic Cloud (LMC): DEM L71 (0505-67.9), 0509-67.5, 0519-69.0, and 0548-70.4. None was detected in the four short-wavelength IRAC bands, but all four were clearly imaged at 24 μm, and two at 70 μm. A comparison of these images with Chandra broadband X-ray images shows a clear association with the blast wave, and not with internal X-ray emission associated with ejecta. Our observations are well described by one-dimensional shock models of collisionally heated dust emission, including grain size distributions appropriate for the LMC, grain heating by collisions with both ions and electrons, and sputtering of small grains. Model parameters are constrained by X-ray, optical, and far-ultraviolet observations. Our models can reproduce observed 70/24 μm flux ratios only by including sputtering, destroying most grains smaller than 0.03-0.04 μm in radius. We infer total dust masses swept up by the SNR blast waves, before sputtering, on the order of 10-2 M
, several times less than those implied by a dust-to-gas mass ratio of 0.3% as often assumed for the LMC. Substantial dust destruction has implications for gas-phase abundances.
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Issue 2 (2006 May 10)
Received 2006 February 10, accepted for publication 2006 March 23
Published 2006 April 20
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Dust Destruction in Type Ia Supernova Remnants in the Large Magellanic Cloud
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