English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present a novel approach to address dust production by low- andintermediate-mass stars. We study the asymptotic giant branch (AGB) phase,during which the formation of dust takes place, from the perspective ofpost-AGB and planetary nebula (PN) evolutionary stage. Using results fromstellar evolution and dust formation modelling, we interpret the spectralenergy distribution of carbon-dust-rich sources currently evolving throughdifferent evolutionary phases, believed to descend from progenitors of similarmass and chemical composition. Comparing the results of different stages alongthe AGB to PNe transition, we can provide distinct insights on the amount ofdust and gas released during the very late AGB phases. While the post-AGBtraces the history of dust production back to the tip of the AGB phase,investigating the PNe is important to reconstruct the mass-loss processexperienced after the last thermal pulse. The dust surrounding the post-AGB wasformed soon after the tip of the AGB. The PNe dust-to-gas ratio is$\sim10^{-3}$, 2.5 times smaller than what expected for the same initial massstar during the last AGB interpulse, possibly suggesting that dust might bedestroyed during the PN phase. Measuring the amount of dust present in thenebula can constrains the capacity of the dust to survive the central starheating.

Dust from evolved stars: a pilot analysis of the AGB to PN transition