Classical Novae Evolution Revealed by the NASA Spitzer Telescope

Details Classical Novae Evolution Revealed by the NASA Spitzer Telescope Classical Novae Evolution Revealed by the NASA Spitzer Telescope

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.2805w&link_type=abstract

American Astronomical Society, HEAD meeting #11, #28.05; Bulletin of the American Astronomical Society, Vol. 41, p.699

Astronomy and Astrophysics

Astrophysics

Scientific paper

Many facets of astrophysics are captured in classical novae (CNe) eruptions, making these systems unique laboratories in which several poorly understood processes (e.g., variable super-soft X-ray emission, mass transfer, thermonuclear runaway, optically thick winds, common envelope evolution, molecule and grain formation, coronal emission) may be observed, many in real time. CNe are also thought to be related to the super-soft sources, the likely progenitors of SN Ia explosions. CNe spectra are remarkable for their changing elemental and ion content and the temporal development of line profiles are critical to understanding the dynamics of ejection. Low-energy permitted lines of CNO and Fe II give way to He II, as well as high ionization lines, e.g., [Fe VII] 6087 Angstrom, and ultimately to infrared (IR) "coronal” lines as the ejecta evolve. The latter lines are sources for abundance information as a wide range of isoelectronic sequences and adjacent ionization states of metals are observable. Often, as the ejecta cool and evolve molecules (e.g., CO) and dust form; the spectrophotometric signature best revealed in the IR. CNe originating on CO White Dwarfs (WDs) are often dust-formers and, while C is a major grain component, silicates, PAHs, and SiC are often present, occasionally in the same nova. At higher energies, X-ray and UV emission in CNe comes from nuclear burning of residual accreted material on the WD surface after the initial outburst, directly probing processes powering the post outburst evolution and affecting ejecta grain growth and destruction. Thus panchromatic observations are necessary to develop a coherent data set to properly model and interpret CNe evolution. Here we highlight IR observations of select CNe studied with the NASA Spitzer telescope and contemporaneously with SWIFT, Chandra, and XMM-Newton. We discuss new paradigms derived from photoionization models and synoptic monitoring efforts.

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