Spitzer observations of the post-eruption evolution of novae

Details Spitzer observations of the post-eruption evolution of novae Spitzer observations of the post-eruption evolution of novae

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007sptz.prop40060e&link_type=abstract

Spitzer Proposal ID #40060

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Scientific paper

A classical nova (CN) eruption arises following a thermonuclear runaway on the surface of a white dwarf in a semi-detached binary system, following which some 10^-4 Msun of material, enriched in metals, is explosively ejected at ~1000km/s. CNe enable us to observe many astrophysical processes (such as dust formation and processing, shaping of nebulae, gas cooling by IR fine structure lines) in real time. Following the eruption, CNe vary rapidly, on a timescale ~months, and this necessitates continuous monitoring. Several novae have now been observed with Spitzer as targets-of-opportunity (ToO) and this proposal seeks further Spitzer time to continue monitoring ToO novae, and to continue monitoring the evolution of novae that erupted in the previous 20 years but before the Spitzer era. In particular, Spitzer ToO observations in previous cycles have enabled us to observe extremely dusty CNe in the mid-far for the first time. We will use the Spitzer IRS to observe novae that have erupted during the past 20 years, providing us with a well-populated parameter space. We aim to determine (i) the ejecta masses, (ii) abundances in the ejected material, (iii) evolution and processing of the CN dust. We will also continue to monitor the recurrent nova RS Oph following its 2006 eruption, and observe other recurrents during quiescence.

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