Dust Ejecta

The data here presented are the outputs of the computations of dust formation in CSEs of TP-AGB stars published in Nanni et al. 2013 and Nanni et al. 2014. These calculations are based on the new TP-AGB tracks obtained by the COLIBRI code (Marigo et al. 2013) in which the characteristic quantities at the first thermal pulse are taken from the PARSEC database of full stellar models (Bressan et al. 2012).

The following files provide the total dust ejecta produced during the entire duration of the TP-AGB phase at varying metallicities (Z=0.001, 0.008, 0.02, 0.04, 0.06) and for different initial stellar masses. The calculations at solar and sub-solar metallicities are based on Nanni et al. 2013, while, for super-solar metallities, the reader can refer to Nanni et al. 2014 for all the details.

Solar and sub-solar metallicities (Z=0.001, 0.008, 0.02)

These files contain the output of two different dust condensation schemes named "low-" and the "high-" condensation temperature models (LCT and HCT models) respectively. As fully discussed in Nanni et al. 2013, these two models primarily differ for the dust condensation temperature of the main dust species produced in the CSEs of TP-AGB stars (silicates, in M-giants and carbon, in C-stars).

Super-solar metallicities (Z=0.04, 0.06)

The dust ejecta here provided are based on our preferred dust condensation scheme (HCT model, for M-giants, and LCT model, for C-stars) already presented in Nanni et al. 2013. An additional dust heating term due to the collisions between H2 molecules and dust grains is included in the computation of the dust temperature along the CSE structure.

New updated dust ejecta

New updated dust ejecta obtained from the latest calibration of the mass-loss rate (Rosenfield et al. 2014) applied to the TP-AGB track by Marigo et al. 2013. See again Nanni et al. 2013 and Nanni et al. 2014 for further details.
Contact: ananni@sissa.it or a.nanni@keele.ac.uk - Last modified: 12/08/2014