ToO Observations of Galactic and Magellanic Cloud Classical Novae

Details ToO Observations of Galactic and Magellanic Cloud Classical Novae ToO Observations of Galactic and Magellanic Cloud Classical Novae

Sep 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop.2333w&link_type=abstract

Spitzer Proposal ID #2333

Astronomy and Astrophysics

Astronomy

Scientific paper

Stars are the engines of energy production and chemical evolution in our Universe. They deposit radiative and mechanical energy into their environments, and enrich the ambient interstellar medium with elements synthesized in their interiors and dust grains condensed in their atmospheres. Classical novae (CN), a transient phenomenon, contribute to this cycle of chemical enrichment through explosive nucleosynthesis and the violent ejection of material dredged from the white dwarf progenitor and mixed with the accreted surface layers. Using Spitzer (+IRS), we propose a 10.5 hr, no-impact, multi-cycle (2) ToO program to study (in temporal detail) the later evolutionary stages of CN (> 40 days post-outburst) by targeting 4 Galactic and 3 Magellanic Cloud novae. Spitzer is a unique facility that can enable us to investigate aspects of CN phenomenon including: the in situ formation and astromineralogy of dust, the elemental abundances resulting from thermonuclear runaway, the correllation of ejecta masses with progenitor type, the bolometric luminosities of the outburst, and the kinematics and structure of the ejected envelopes. Specifically, our program addresses four research problems in the study of CN evolution: 1)~determination of the grain size distribution and mineral composition of nova dust; 2)~estimation of chemical abundances of nova ejecta from coronal and forbidden emission line spectroscopy; 3)~measurement of the density and masses of the ejecta; and 4)~characterization of the nature of novae in the SMC and LMC at mid- to far-infrared wavelengths.

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