Silicate crystallinities of O-rich evolved stars : J/MNRAS/466/1963

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Authors : Liu J. orcid , Jiang B.W., Li A. (hide) , Jiang B.W., Li A. et..al

VizieR DOI : https://doi.org/10.26093/cds/vizier.74661963
Bibcode : 2017MNRAS.466.1963L (ADS) (Simbad) (Objects)
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Data origin :

CDS Keywords : Stars, giant; Mass loss; Photometry, UBVRI; Photometry, infrared
UAT : Giant stars, Stellar mass loss, Infrared photometry, Optical astronomy, Broad band photometry, Infrared photometry

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Inserted into VizieR : 21-Apr-2020
Last modification : 17-Aug-2024

On the silicate crystallinities of oxygen-rich evolved stars and their mass-loss rates. (2017)

Keywords : stars AGB and post-AGB - circumstellar matter - stars: evolution - stars: mass-loss - dust, extinction

Abstract:For decades ever since the early detection in the 1990s of the emission spectral features of crystalline silicates in oxygen-rich evolved stars, there is a long-standing debate on whether the crystallinity of the silicate dust correlates with the stellar mass-loss rate. To investigate the relation between the silicate crystallinities and the mass-loss rates of evolved stars, we carry out a detailed analysis of 28 nearby oxygen-rich stars. We derive the mass-loss rates of these sources by modelling their spectral energy distributions from the optical to the far-infrared. Unlike previous studies in which the silicate crystallinity was often measured in terms of the crystalline-to-amorphous silicate mass ratio, we ...(more)
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We select a sample of 28 O-rich evolved stars (see Table 1) based on the following criteria: (i) the ISO/SWS spectra of most of these sources exhibit prominent crystalline silicate emission features; (ii) they exhibit distinguished 10 and 18{mu}m amorphous silicate emission features; (iii) they are relatively 'local' with a distance of less than 5kpc to remove the influence of extinction and metallicity. The ISO/SWS spectra are taken from the archive and the ~2.4-45{mu}m wavelength range covers 6 out of 7 of the crystalline silicate feature complexes summarized by Molster et al. (2002A&A...382..222M), i.e. the 10, 18, 23, 28, 33.6 and 40{mu}m complexes except the 69{mu}m complex. These archival data have already been processed by Sloan et al. (2003ApJS..147..379S) in a uniform manner. 


                


                

                    

                


                

                    

                


                

                    
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