Journal
ASTROPHYSICAL JOURNAL
Volume 810, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/810/1/39
Keywords
dust, extinction; galaxies: evolution; galaxies: ISM; Magellanic Clouds
Categories
Funding
- Ministry of Science and Technology (MoST) [102-2119-M-001 -006-MY3]
- Grants-in-Aid for Scientific Research [15K05033] Funding Source: KAKEN
Ask authors/readers for more resources
The Large and Small Magellanic Clouds (LMC and SMC, respectively) are observed to have characteristic dust extinction curves that are quite different from those of the Galaxy (e.g., strength of the 2175 angstrom bump). Although the dust composition and size distribution of the Magellanic Clouds (MCs), which can self-consistently explain their observed extinction curves, have already been proposed, it remains unclear whether and how the required dust properties can be achieved in the formation histories of the MCs. We therefore investigate the time evolution of the dust properties of the MCs and thereby derive their extinction curves using one-zone chemical evolution models with formation and evolution of small and large silicate and carbonaceous dust grains and dusty winds associated with starburst (SB) events. We find that the observed SMC extinction curve without a conspicuous 2175 angstrom bump can be reproduced well by our SMC model if the small carbon grains can be selectively lost through the dust wind during the latest SB, about 0.2 Gyr ago. We also find that the LMC extinction curve with a weak 2175 angstrom bump can be reproduced by our LMC model with less efficient removal of dust through dust wind. We discuss possible physical reasons for different dust wind efficiencies between silicate and graphite and among galaxies.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available