/ftp/cats/A+A/556/A38



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J/A+A/556/A38    Period-mass-loss rate relation of Miras    (Uttenthaler, 2013)
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	table1.dat
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Beginning of ReadMe : J/A+A/556/A38 Period-mass-loss rate relation of Miras (Uttenthaler, 2013) ================================================================================ Period-mass-loss rate relation of Miras with and without technetium. Uttenthaler S. <Astron. Astrophys. 556, A38 (2013)> =2013A&A...556A..38U ================================================================================ ADC_Keywords: Stars, variable ; Photometry, infrared Keywords: stars: AGB and post-AGB - stars: late-type - stars: evolution - stars: mass-loss - stars: oscillations Abstract: We report the discovery that Mira variables with and without absorption lines of the element technetium (Tc) occupy two different regions in a diagram of near- to mid-IR colour versus pulsation period. Tc is an indicator of a recent or ongoing mixing event called the third dredge-up (3DUP), and the near- to mid-IR colour, such as the (K-[22]) colour where [22] is the the 22um band of the WISE space observatory, is an indicator of the dust mass-loss rate of a star. We collected data from the literature about the Tc content, pulsation period, and near- and mid-IR magnitudes of more than 190 variable stars on the asymptotic giant branch (AGB) to which Miras belong. The sample is naturally biased towards optical AGB stars, which have low to intermediate (dust) mass-loss rates. Description: Table 1 is a collection of information on the technetium (Tc) content, pulsation period, and IR photometry of AGB variables, without claim of completeness, in particular for the semi-regular variables (SRVs). Up to three references on the Tc content are given. The pulsation period is the most up-to-date value possible, for many objects based on an analysis of AAVSO data with the Period04 program (Lenz & Breger, 2005CoAst.146...53L). The spectral (or chemical) type of the star is taken from the same literature as the information on Tc. A mean K magnitude and J-K colour is computed from all available literature, as listed in Sect. 2 of the paper; they are meant to be as close as possible to cycle-averaged values, to average out the variability of the objects. Finally, magnitudes are given in the IRAS 12, 25, and 60 micron bands, Akari 9 and 18 micron bands, and WISE 22 micron bands are given, where fluxes have been converted to magnitudes given the zero-magnitude fluxes as given in the Note to Table 1.