Mass-loss History of a 'typical' AGB Star, Mira, Using Far-Infrared Imaging Photometry

Details Mass-loss History of a 'typical' AGB Star, Mira, Using Far-Infrared Imaging Photometry Mass-loss History of a 'typical' AGB Star, Mira, Using Far-Infrared Imaging Photometry

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21943924m&link_type=abstract

American Astronomical Society, AAS Meeting #219, #439.24

Astronomy and Astrophysics

Astronomy

Scientific paper

During the Asymptotic giant branch (AGB) phase intermediate mass stars suffer mass loss which leads to the formation of a circumstellar shell of gas and dust. At the end of the AGB phase, a star develops a superwind that leads to the exhaustion of the outer stellar envelope. Then the star evolves off the AGB and becomes a pre-planetary nebula (PPN) for short time 1000 years.
At this stage the mass loss has significantly decreased or stopped, and the circumstellar shell begins to drift away from the star. When the stellar core evolves to high enough effective temperatures to produce photo-ionizing radiation, the circumstellar dust shell gets ejected (to the interstellar medium) and the star becomes a planetary nebula (PN). If the velocity of the AGB wind has been relatively constant, then dust furthest from the star represents the oldest mass loss, while material closer to the star represents more recent mass loss. Hence, the history of mass loss during the AGB phase is imprinted on the dust shells of AGB and post-AGB envelopes.
We present the results and analysis of linear map scans from far infrared image observations of prototypical AGB star Mira, that were taken using IRAS, ISOPHOT, Spitzer telescopes in order to determine a) the history of mass loss, and b) to measure the total mass of the circumstellar dust from which we can infer the lower limit to the initial mass of the progenitor star. Furthermore, we derived the profile of dust emission spectral index vs. dust temperature that is useful in the study of the distribution of matter within the shells. We discuss the nature of the dust shells in terms of the derived spectral energy distribution implied by the observations.

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