NONUNIFORM EXPANSION OF THE YOUNGEST GALACTIC SUPERNOVA REMNANT G1.9+0.3
- Department of Physics, North Carolina State University, Raleigh, NC 27695-8202 (United States)
- Cavendish Laboratory, 19 J.J. Thomson Avenue, Cambridge CB3 0HE (United Kingdom)
- Department of Astronomy, University of Maryland, College Park, MD 20742 (United States)
- NASA/GSFC, Code 660, Greenbelt, MD 20771 (United States)
- Department of Electrical and Computer Engineering, Duke University, Durham, NC 27708 (United States)
- Department of Electrical and Computing Engineering, University of Wisconsin-Madison, Madison, WI 53706 (United States)
We report measurements of the X-ray expansion of the youngest Galactic supernova remnant, G1.9+0.3, using Chandra observations in 2007, 2009, and 2011. The measured rates strongly deviate from uniform expansion, decreasing radially by about 60% along the X-ray bright SE-NW axis from 0.84% ± 0.06% yr{sup –1} to 0.52% ± 0.03% yr{sup –1}. This corresponds to undecelerated ages of 120-190 yr, confirming the young age of G1.9+0.3 and implying a significant deceleration of the blast wave. The synchrotron-dominated X-ray emission brightens at a rate of 1.9% ± 0.4% yr{sup –1}. We identify bright outer and inner rims with the blast wave and reverse shock, respectively. Sharp density gradients in either the ejecta or ambient medium are required to produce the sudden deceleration of the reverse shock or the blast wave implied by the large spread in expansion ages. The blast wave could have been decelerated recently by an encounter with a modest density discontinuity in the ambient medium, such as may be found at a wind termination shock, requiring strong mass loss in the progenitor. Alternatively, the reverse shock might have encountered an order-of-magnitude density discontinuity within the ejecta, such as may be found in pulsating delayed-detonation Type Ia models. We demonstrate that the blast wave is much more decelerated than the reverse shock in these models for remnants at ages similar to G1.9+0.3. Similar effects may also be produced by dense shells possibly associated with high-velocity features in Type Ia spectra. Accounting for the asymmetry of G1.9+0.3 will require more realistic three-dimensional Type Ia models.
- OSTI ID:
- 22365494
- Journal Information:
- Astrophysical Journal Letters, Vol. 790, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
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