2008/12/10 by Biwei Jiang, B. W. Jiang, Ke Zhang +1 · 1 citation
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Asymptotic giant branch #Circumstellar dust #Feature (linguistics) #Galaxy #Large Magellanic Cloud #Metallicity #Physics #Planetary nebula #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.5047/eps.2008.12.004
published as Earth Planets Space 62:105-110,2010 · 7 pages, 1 figure, uses eps.cls. Accepted for publication in "Earth, Planets and Space" (special issue on Cosmic Dust)
arxiv created 2008/12/10 · openalex publication_date 2010/01/01 · arxiv updated 2014/11/18 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
The 21-μm and 30-μm bands are the strongest dust emission features detected in evolved low- and intermediate-mass C-rich stars (i.e. asymptotic giant branch (AGB) stars, proto-planetary nebulae (PPNe), and planetary nebulae (PNe)). While the 21-μm feature is rare and exists only in the transient PPN phase, the 30-μm feature is more common and seen in the entire late stage of stellar evolution, from AGB to PPN and PN phases, as well as in the low-metallicity galaxies: the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC). The carriers of these features remain unidentified. All the 21-μm sources also emit in the 30-μm band, suggesting that their carriers may be somewhat related.