We report on studies of classical nova (CN) explosions where we follow the evolution of thermonuclear runaways (TNRs) on carbon oxygen (CO) and oxygen-neon (ONe) white dwarfs (WDs). Our simulations are guided by the results of multi-dimensional studies of TNRs in WDs which find that sufficient mixing with WD core material occurs after the TNR is well underway, reaching levels of enrichment that agree with observations of CN ejecta abundances. Our results show large enrichments of7Be in the ejected gases implying that CNe may be responsible for a significant fraction (∼ 100 M) of the7Li in the galaxy (∼1000 M). In addition, the WDs in these simulations are ejecting less material than they accrete. We, therefore, predict that the WDs can grow in mass as a consequence of the TNR and CNe may be an important channel of Supernova Ia progenitors.
|Original language||English (US)|
|Number of pages||5|
|Journal||Memorie della Societa Astronomica Italiana - Journal of the Italian Astronomical Society|
|State||Published - 2020|
|Event||2019 Lithium in the Universe: to Be or not to Be? - Monte Porzio Catone, Italy|
Duration: Nov 18 2019 → Nov 22 2019
Bibliographical noteFunding Information:
Acknowledgements. We acknowledge useful discussion and encouragement from C. Deliyannis, J. José, M. Hernanz, L. Izzo, P. Molaro, and M. della Valle. This work was supported in part by NASA under the Astrophysics Theory Program grant 14-ATP14-0007 and the U.S. DOE under Contract No. DE-FG02-97ER41041. SS acknowledges partial support from NASA, NSF and HST grants to ASU, WRH is supported by the U.S. Department of Energy, Office of Nuclear Physics, and CEW acknowledges support from NASA and NSF.
© SAIt 2020.
- Stars: Classical novae
- Stars: abundances
- Stars: lithium