The Effect Of Metallicity And C/O On The Low-Contrast Dust Features Of Low-Mass-Loss Rate O-Rich AGB Stars.

Details The Effect Of Metallicity And C/O On The Low-Contrast Dust Features Of Low-Mass-Loss Rate O-Rich AGB Stars. The Effect Of Metallicity And C/O On The Low-Contrast Dust Features Of Low-Mass-Loss Rate O-Rich AGB Stars.

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21934313a&link_type=abstract

American Astronomical Society, AAS Meeting #219, #343.13

Astronomy and Astrophysics

Astronomy

Scientific paper

Asymptotic Giant Branch (AGB) stars are major contributors of material to the interstellar medium. The chemistry of the dust ejected into the ISM is dictated by the ratio of carbon to oxygen atoms. The reason for this division is that carbon monoxide (CO) is very stable, so the most of the carbon and oxygen will be trapped in CO. The excess of the more abundant element, carbon or oxygen, will dominate the dust formation. Consequently AGB stars either are O-rich or carbon-rich (C-rich). Carbon, and possibly some oxygen atoms are made and dredged up to the stellar surface during the AGB phase, and therefore an AGB star has timing varying C/O, starting out with values expected to be close to solar. It has been suggested that even small changes in C/O may affect the precise composition and structure of the O-rich dust forming around these stars. Moreover, metallicity affects the atoms available for dust formation.
The infrared spectra of oxygen-rich (O-rich) asymptotic giant branch (AGB) stars show a broad 9-13 micron feature. Here we present a study of the effect of both C/O and the metallicity on low-intensity broad dust features around O-rich AGB stars, we find that while dust feature parameters do not correlate with C/O, they do correlate with the Fe-group abundances. The implications of this finding are discussed.

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