The Imprint of Nova Nucleosynthesis in Presolar Grains
By J. José, M. Hernanz, S. Amari, K. Lodders, E. Zinner. 2002
159 citations recorded by the source corpus.
Infrared and ultraviolet observations of nova light curves have confirmed grain formation in their expanding shells that are ejected into the interstellar medium by a thermonuclear runaway. In this paper we present isotopic ratios of intermediate-mass elements up to silicon for the ejecta of CO and ONe novae, based on 20 hydrodynamic models of nova explosions. These theoretical estimates will help to properly identify nova grains in primitive meteorites. In addition, equilibrium condensation calculations are used to predict the types of grains that can be expected in the nova ejecta, providing some hints on the puzzling formation of C-rich dust in O > C environments. These results show that SiC grains can condense in ONe novae, in concert with an inferred (ONe) nova origin for several presolar SiC grains.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/3622d26592ddb604a56bdd82f99afe89daa3e6be
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In Astronomy and Astrophysics
Citations in the corpus
- Aluminum-, Calcium- and Titanium-rich Oxide Stardust in Ordinary Chondrite Meteorites (2008, unknown): “For example, Nittler & Hoppe (2005) recently proposed that the most 17O-rich grain (T54; Nittler et al. 1997) might have formed in a nova explosion, since its composition matches that predicted by some recent nova models (José et al. 2004).”
- Astrophysics with Extraterrestrial Materials (2016, background): “Thus, putative nova SiC and graphite grains were identified on the basis of very low 12C/13C and 14N/15N ratios (Figure 5) as well as associated 30Si excesses in some grains, also predicted by nova nucleosynthesis models ( José et al. 2004).”