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Summary: Constraints on the Progenitor of Cassiopeia A
Patrick A. Young1,2
, Chris L. Fryer1,3
, Aimee Hungerford1
, David Arnett2
, Gabriel
Rockefeller1,3
, F. X. Timmes1
, Benedict Voit1,4
, Casey Meakin2
, and Kristoffer A. Eriksen1,2
payoung@lanl.gov, fryer@lanl.gov, aimee@lanl.gov, darnett@as.arizona.edu,
gaber@lanl.gov, fxt@lanl.gov, cmeakin@as.arizona.edu,
keriksen@as.arizona.edu
ABSTRACT
We compare a suite of 3D explosion calculations and stellar models incor-
porating advanced physics with observational constraints on the progenitor of
Cassiopeia A. We consider binary and single stars from 16 to 40 M with a range
of explosion energies and geometries. The parameter space allowed by observa-
tions of nitrogen rich high velocity ejecta, ejecta mass, compact remnant mass,
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