Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21943618r&link_type=abstract
American Astronomical Society, AAS Meeting #219, #436.18
Astronomy and Astrophysics
Astronomy
Scientific paper
Infrared spectroscopic data are presented for V496 Scuti (Nova Scuti 2009) that include both the carbon monoxide (CO) fundamental and first overtone emission. These data, from 3 weeks after outburst, were obtained from Lick Observatory and the NASA Infrared Telescope Facility. The relative strength of the bandheads within the first overtone indicates that the CO forms in a region whose temperature is about 2500K. More important, however, is the strength of the first overtone to the fundamental. The flux ratio is about a factor of 20 lower than expected if the fundamental were optically thin. The shape of the CO fundamental, which follows the Planck function at the 2500 K temperature, also indicates that the fundamental is optically thick. To be so means that line escape in this region is controlled by the local thermal width of the lines rather than the overall Doppler widths of the nova ejecta. Despite the optical depth, the energy radiated by the CO bands is greater than any other infrared line, and is the dominant cooling source for the region in which it forms.
The first overtone also shows a significant contribution from C13O16, indicating a C13/C12 ratio of about 0.8. C I and O I lines appear in the spectrum along with the CO emission and are also quite strong. While this would suggest that carbon monoxide formation in V496 Scuti did not proceed to saturation (as it does in the outer atmospheres of late-type stars), the comparatively low temperature indicated for the CO molecules suggests that CO formation probably occurs in a different region from that where the C I and O I lines form. The conditions within the CO region should be conducive to dust formation.
Astronomy at The Aerospace Corporation is funded by the Internal Research and Development program.
Bernstein Lawrence
Bjorkman Karen S.
Dimpfl William L.
Perry Raleigh B.
Prater T. R.
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