Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.2801s&link_type=abstract
American Astronomical Society, HEAD meeting #11, #28.01; Bulletin of the American Astronomical Society, Vol. 41, p.699
Astronomy and Astrophysics
Astronomy
Scientific paper
Classical and Recurrent Novae (CNe and RNe) outbursts are the most common of the explosions in a galaxy. They have been observed as close as a kpc and as far as M87. In a nova, material is accreted from a Roche-lobe filling star and accumulates on a white dwarf until an explosion occurs. Accreted material is mixed with white dwarf core material at some time during the evolution of the explosion. The mixture is processed through hot hydrogen burning before being ejected into space and analyzing the ejecta allows us to determine the core composition of the white dwarf. CNe are one component in the cycle of Galactic chemical evolution where the ejected metal-enriched gas is a source of nuclei for the ISM. IR observations show that some CNe form multiple types of grains in their ejecta which may have been identified in meteoritic material. Simulations predict, and observations confirm, that there is a phase of X-ray emission from the post-explosion hot white dwarf emitted by the accreted plus core layers that were not initially ejected. The hot photosphere is revealed as the ejection phase ends. We will report on the recent renaissance in studies of RNe and CNe with Swift, Chandra, XMM, RXTE, HST, and Spitzer, as well as recent advances in the theory of the outburst. These new results question some long held beliefs about novae and provided evidence for a possible connection between novae, the Super Soft Binary X-ray sources, and SN Ia.
I acknowledge partial support from Chandra, Swift, Spitzer, NASA Theory and the NSF.
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