Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.5118h&link_type=abstract
American Astronomical Society, AAS Meeting #211, #51.18; Bulletin of the American Astronomical Society, Vol. 39, p.818
Astronomy and Astrophysics
Astronomy
Scientific paper
Classical novae are thought to be contributors to the chemical evolution of gas in the interstellar medium on local scales, but are they significant contributors to interstellar dust? How much dust do they contribute and on what timescale? Many classical novae have been observed to produce prodigious amounts of dust in their ejecta, but it is often held that this dust should be rapidly destroyed by the high intensity radiation emitted by the underlying white dwarf. We present five epochs of data on the dusty nova V1065 Centauri obtained with the Spitzer Space Telescope Infrared Spectrograph and trace the evolution of the 10 and 20 µm silicate emission features observed in the ejecta. Throughout our observations, the flux of the broad 10 µm feature intensifies by a factor of about four above the continuum while the peak of the underlying black body emission appears to be moving to longer wavelengths indicative of cooling. Comparing these developments with the evolution of hydrogen recombination lines and nebular emission lines of neon and oxygen, we see evidence for a hardening radiation field coincident with cooling of the dust implying substantial structure within the ejecta. We explore the possibility that these clumps of dusty material may survive long enough to be disseminated into the surrounding interstellar medium.
Support for this work also was provided by NASA through contracts 1314757 & 1267992, issued by JPL/Caltech to the University of Minnesota.
Evans Nick
Helton Lorren Andrew
Lynch David K.
Rudy Richard J.
Schwarz Greg J.
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