Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...345l..39s&link_type=abstract
Astronomy and Astrophysics, v.345, p.L39-L42 (1999)
Astronomy and Astrophysics
Astrophysics
26
Stars: Agb And Post-Agb, Stars: Circumstellar Matter, Stars: Individual: Iras 04296+3429, Stars: Individual: Iras 22272+5435, Radiative Transfer
Scientific paper
We report the detection of the 30 mu m emission feature from the C-rich post-Asymptotic Giant Branch (post-AGB) star IRAS 04296+3429 based on ISO SWS observations. ISO data show that there is a clear substructure in the 30 mu m feature in the form of a plateau which extends from 26 to 27 mu m. This is confirmed by the ISO SWS data for another post-AGB object IRAS 22272+5435, which has the strongest known 30 mu m band accounting for about 24% of its total infrared (IR) emission or 12% of the bolometric luminosity. In the case of IRAS 04296+3429 we estimate that about 85% of the total energy is emitted in the infrared of which about 15-22% (depending on the estimated continuum level) is contributed by the 30 mu m band. The total energy emitted in the band is at least comparable for both sources, while the energy emitted in the 21 mu m band seems to be about 3 times larger in the case of IRAS 04296+3429, if they have the same bolometric luminosity. Grains of pure MgS could be responsible for the observed 30 mu m feature provided they have a broad distribution of shapes, but they cannot account for the observed plateau emission. Small graphite grains with relatively thick MgS coating could be responsible for the observed substructure, but we were not able to definitively solve the question of their contribution to the 30 mu m band. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with participation of ISAS and NASA
Cox Pierre
Henning Th
Kwok Sun
Szczerba Ryszard
Volk Kathryn
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