2018/09/06 by J. Isern, E. Bravo, Isern, J. +2
Physics and Astronomy · #Astro and Planetary Science #Astronomy and Astrophysical Research #FOS: Physical sciences #Gamma-ray bursts and supernovae #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1809.01825
Accepted for publication in RNAAS (3 pages, 1 figure)
arxiv created 2018/09/06 · openalex publication_date 2018/09/06 · arxiv updated 2018/09/07 · openalex created_date 2019/06/27 · openalex updated_date 2026/07/28
It is commonly accepted that collisions between white dwarfs (WD) are rare events that only occur in the dense interior of globular clusters or in the dense outskirts around the central galactic black holes, and are therefore disregarded as an important source of Type Ia supernovae (SNIa). Although the majority of these encounters will not result in a SNIa event, many of them will produce mass ejections. Under the appropriate circumstances, this material can become part of a protostar nebula, including the pre-solar one, in the form of stardust leading to the existence of chemical anomalies in meteorites. We describe a WD-WD collision scenario that potentially might explain the so called Ne-E anomaly found in some primitive meteorites like Orgueil and Murchison.