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Modelling dust processing and the evolution of grain sizes in the ISM using the method of moments
KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.ORCID iD: 0000-0002-0105-4102
2016 (English)In: Planetary and Space Science, ISSN 0032-0633, E-ISSN 1873-5088Article in journal (Refereed) Published
Abstract [en]

Interstellar dust grains do not have a single well-defined origin. Stars are demonstrably dust producers, but also efficient destroyers of cosmic dust. Dust destruction in the ISM is believed to be the result of SN shocks hitting the ambient ISM gas (and dust) and lead to an increased rate of ion sputtering, which reduces the dust mass. Grains located in cold molecular clouds can on the other hand grow by condensation, thus providing a replenishment mechanism or even a dominant channel of dust formation. In dense environments grains may coagulate and form large composite grains and aggregates and if grains collide with large enough energies they may be shattered, forming a range of smaller debris grains. The present paper presents a statistical modelling approach using the method of moments, which is computationally very inexpensive and may therefore be an attractive option when combining dust processing with, e.g., detailed simulations of interstellar gas dynamics. A solar-neighbourhood-like toy model of interstellar dust evolution is presented as an example. © 2016.

Place, publisher, year, edition, pages
Elsevier, 2016.
Keyword [en]
Dust, Galaxy evolution, Grain size distribution, Interstellar medium, Milky Way, Cosmology, Galaxies, Gas dynamics, Grain size and shape, Method of moments, Evolution of grain, Interstellar dust, Interstellar mediums, Milky ways, Solar neighbourhood, Statistical modelling
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:kth:diva-196154DOI: 10.1016/j.pss.2016.05.002ISI: 000389284800014ScopusID: 2-s2.0-84971672815OAI: oai:DiVA.org:kth-196154DiVA: diva2:1046987
Note

Correspondence Address: Mattsson, L.email: larsmat@kth.se. QC 20161116

Available from: 2016-11-16 Created: 2016-11-14 Last updated: 2017-01-09Bibliographically approved

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