High velocity dust grains produced by a supernova explosion
Abstract
Motivated by the discovery of a meteor with velocity more than 300~km/s (Afanasiev et al. 2007) we study how dust grains formed in the supernova (SN) ejecta at its free-expansion phase can keep their high velocity obtained from the gas, where these grains were born. Using a one-dimensional spherically symmetric Lagrangian approach we follow the dynamics of grains during the interaction of a SN ejecta with the ambient interstellar gas. We found that grains larger ∼ 0.3 μm can cross the SN forward shock front and reach the ambient interstellar medium. They are destroyed inefficiently, thus, their sizes remain close to the initial ones. In a diffuse interstellar gas of density ≲ 1 cm−3 grains larger as ≳ 1 μm move with velocity around 1−2 thousand km/s and spread over distances exceeding ∼ 40−90 pc from the SN origin within tens of kiloyears. In dense environment the propagation of grains is significantly suppressed: even large grains do not spread over distances greater than 50% of the current SN remnant size. Grains born close to the edge of the SN ejecta core in less-massive ejecta reach greater distances. Thus, high-velocity grains are expected to be formed in this part of the ejecta with mass lower than ∼ 3 M⊙ of the SN remnant evolving in a diffuse gas with density ≲ 1 cm−3. We discuss possible consequences for dust transport out from galactic disks.
Related
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BibTeX
@misc{vasiliev2026high,
title = {{High velocity dust grains produced by a supernova explosion}},
author = {Evgenii O. Vasiliev},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.39759},
eprint = {2609.39759},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.39759},
}
RIS
TY - UNPB
TI - High velocity dust grains produced by a supernova explosion
AU - Evgenii O. Vasiliev
PY - 2026
DA - 2026/09/30
PB - arXiv
DO - 10.48550/arxiv.2609.39759
UR - https://arxiv.org/abs/2609.39759
AB - Motivated by the discovery of a meteor with velocity more than 300~km/s (Afanasiev et al. 2007) we study how dust grains formed in the supernova (SN) ejecta at its free-expansion phase can keep their high velocity obtained from the gas, where these grains were born. Using a one-dimensional spherically symmetric Lagrangian approach we follow the dynamics of grains during the interaction of a SN ejecta with the ambient interstellar gas. We found that grains larger ∼ 0.3 μm can cross the SN forward shock front and reach the ambient interstellar medium. They are destroyed inefficiently, thus, their sizes remain close to the initial ones. In a diffuse interstellar gas of density ≲ 1 cm^−3 grains larger as ≳ 1 μm move with velocity around 1−2 thousand km/s and spread over distances exceeding ∼ 40−90 pc from the SN origin within tens of kiloyears. In dense environment the propagation of grains is significantly suppressed: even large grains do not spread over distances greater than 50% of the current SN remnant size. Grains born close to the edge of the SN ejecta core in less-massive ejecta reach greater distances. Thus, high-velocity grains are expected to be formed in this part of the ejecta with mass lower than ∼ 3 M_⊙ of the SN remnant evolving in a diffuse gas with density ≲ 1 cm^−3. We discuss possible consequences for dust transport out from galactic disks.
ER -