1 code implementation • 22 Apr 2019 • Lluís Galbany, Chris Ashall, Peter Hoeflich, Santiago González-Gaitán, Stefan Taubenberger, Maximilian Stritzinger, Eric Y. Hsiao, Paolo Mazzali, Eddie Baron, Stéphane Blondin, Subhash Bose, Mattia Bulla, Jamison F. Burke, Christopher R. Burns, Régis Cartier, Ping Chen, Massimo Della Valle, Tiara R. Diamond, Claudia P. Gutiérrez, Jussi Harmanen, Daichi Hiramatsu, T. W. -S. Holoien, Griffin Hosseinzadeh, D. Andrew Howell, Yiwen Huang, Cosimo Inserra, Thomas de Jaeger, Saurabh W. Jha, Tuomas Kangas, Markus Kromer, Joseph D. Lyman, Kate Maguire, George Howie Marion, Dan Milisavljevic, Simon J. Prentice, Alessandro Razza, Thomas M. Reynolds, David J. Sand, Benjamin J. Shappee, Rohit Shekhar, Stephen J. Smartt, Keivan G. Stassun, Mark Sullivan, Stefano Valenti, Steven Villanueva, Xiao-Feng Wang, J. Craig Wheeler, Qian Zhai, Jujia Zhang
Our modeling suggests that the narrow [Ca II] features observed in the nebular spectrum are associated with $^{48}$Ca from electron capture during the explosion, which is expected to occur only in white dwarfs that explode near or at the $M_{\rm Ch}$ limit.
Solar and Stellar Astrophysics High Energy Astrophysical Phenomena
