Splinter Meeting DustEvol
Dust evolution in galaxies - focus on supernovae, AGB stars and the ISM
Time: Thursday September 12, 14:00-15:45
and 16:15-18:00
and Friday September 13, 14:00-15:45
CEST (UTC+2)
Room: S12
Convenor(s): Florian Kirchschlager,
Ilse De Looze,
Nina Sartorio,
Tassilo Scheffler,
Fabian Walter,
Kathryn Kreckel
Ghent University,
MPIA Heidelberg,
Heidelberg University
Cosmic dust, comprising (sub-)microscopic particles, is ubiquitous in the universe and plays a pivotal role in various astronomical phenomena. Originating from stellar processes such as supernova (SN) explosions or low-mass stars at late evolutionary stages, this interstellar component provides crucial insights into the formation of celestial bodies and the evolution of galaxies. Astronomical observations are profoundly impacted by cosmic dust which often obscures distant objects or scatters light to reveal cosmic structures. Cosmic dust thus stands as an omnipresent and indispensable component of the local and early universe.
SNe are cosmic factories that produce most of the known elements. Furthermore, the expanding ejecta of the SN remnants provide perfect conditions for condensing dust from these heavy elements. However, there are several dust destruction processes going on which are related to SN shocks. Internal shock waves in the SN remnant can destroy a significant part of the newly formed dust, while pre-existing ISM dust is hit by the SN blast wave, which can lead to a massive destruction by sputtering and grain-grain collisions. Overall, it is unclear whether SNe are net dust producers or destroyers.
In order to maintain dust masses observed in the universe, further dust formation sites have to be taken into account, like the winds and outer shells of asymptotic giant branch (AGB) stars. However, significant quantities of dust have been observed in galaxies and quasars in the early Universe which has left little room for dust enrichment by AGB stars. The apparent challenge to reconcile dust destruction and formation rates has led to the idea that dust growth in the ISM is important. In the last years, observational and theoretical studies constraining the dust abundances of galaxies have made a leap forward, in particular at high redshift where sub-mm telescopes such as ALMA have shown that the build-up of metals to dust occurs very rapidly. PAH grains, which have a particular relevance for dust evolution in galaxies, have also been detected recently by the JWST.
In this session, we aim to discuss the state-of-the-art models and observations of dust at known formation sites, namely SN remnants, AGB stars, and the ISM. We aim to discuss the dust formation but also the dust destruction by SN shock waves and other processes. Using high-resolution observations and sophisticated simulations, we will bring together theorists and observers to facilitate discussions and make progress on the physical interpretation of recent observations. Understanding the mechanisms and the conditions under which dust is destroyed and formed in SNRs and in the ISM is critical to answering the eminent question of how dust evolves within a galaxy.
Program
Thursday September 12, 14:00-15:45
Dust evolution in galaxies - focus on supernovae, AGB stars and the ISM (S12)
Thursday September 12, 16:15-18:00
Dust evolution in galaxies - focus on supernovae, AGB stars and the ISM (S12)
Friday September 13, 14:00-15:45
Dust evolution in galaxies - focus on supernovae, AGB stars and the ISM (S12)
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