Modeling The Structure Of Shocked Ejecta In Tycho's Snr

Astronomy and Astrophysics – Astronomy

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Scientific paper

SN 1572 is a famous, and nearby, example of a type Ia supernova; its remnant, Tycho's SNR, has been studied extensively by the Chandra X-ray observatory. Chandra's images show the fluffy structure of the ejecta, potentially due to Rayleigh-Taylor fluid instabilities. The absence of a sharp cutoff in limb brightening suggests that either the reverse shock has been disrupted by these instabilities or that only the Rayleigh-Taylor fingers are radiating in the X-ray band. This project attempts to model these features of Tycho's SNR, using the exponential ejecta profile of Dwarkadas and Chevalier (1998); the hydrodynamics code was augmented by incorporating ionization timescale. The simulation was performed in 3-D, allowing for line-of-sight integration to model the effects Chandra observes and for unfettered instability growth. Further, in order to avoid preferential selection of small angular modes, the simulation was run over all 4π steradians; coordinate singularities at the poles were avoided by using a specialized Yin-Yang grid. We present the results from this simulation, consider the role of ionization timescale in modeling Chandra's observations, and offer suggestions for refinements and changes to the model used.

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