Supernova Dust Evolution Probed by Deep-sea 60Fe Time History
There is a wealth of data on live, undecayed ^60 Fe ( t _1/2 = 2.6 Myr) in deep-sea deposits, the lunar regolith, cosmic rays, and Antarctic snow, which is interpreted as originating from the recent explosions of at least two near-Earth supernovae. We use the ^60 Fe profiles in deep-sea sediments to...
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ftdoajarticles:oai:doaj.org/article:ab41f387300f4d1eb74ed1292cf6a041 2023-10-09T21:47:02+02:00 Supernova Dust Evolution Probed by Deep-sea 60Fe Time History Adrienne F. Ertel Brian J. Fry Brian D. Fields John Ellis 2023-01-01T00:00:00Z https://doi.org/10.3847/1538-4357/acb699 https://doaj.org/article/ab41f387300f4d1eb74ed1292cf6a041 EN eng IOP Publishing https://doi.org/10.3847/1538-4357/acb699 https://doaj.org/toc/1538-4357 doi:10.3847/1538-4357/acb699 1538-4357 https://doaj.org/article/ab41f387300f4d1eb74ed1292cf6a041 The Astrophysical Journal, Vol 947, Iss 2, p 58 (2023) Supernovae Nucleosynthesis Mass spectrometry Astrophysical dust processes Astrophysics QB460-466 article 2023 ftdoajarticles https://doi.org/10.3847/1538-4357/acb699 2023-09-10T00:44:45Z There is a wealth of data on live, undecayed ^60 Fe ( t _1/2 = 2.6 Myr) in deep-sea deposits, the lunar regolith, cosmic rays, and Antarctic snow, which is interpreted as originating from the recent explosions of at least two near-Earth supernovae. We use the ^60 Fe profiles in deep-sea sediments to estimate the timescale of supernova debris deposition beginning ∼3 Myr ago. The available data admits a variety of different profile functions, but in all cases the best-fit ^60 Fe pulse durations are >1.6 Myr when all the data is combined. This timescale far exceeds the ≲0.1 Myr pulse that would be expected if ^60 Fe was entrained in the supernova blast wave plasma. We interpret the long signal duration as evidence that ^60 Fe arrives in the form of supernova dust, whose dynamics are separate from but coupled to the evolution of the blast plasma. In this framework, the >1.6 Myr is that for dust stopping due to drag forces. This scenario is consistent with the simulations in Fry et al. (2020), where the dust is magnetically trapped in supernova remnants and thereby confined around regions of the remnant dominated by supernova ejects, where magnetic fields are low. This picture fits naturally with models of cosmic-ray injection of refractory elements as sputtered supernova dust grains and implies that the recent ^60 Fe detections in cosmic rays complement the fragments of grains that survived to arrive on the Earth and Moon. Finally, we present possible tests for this scenario. Article in Journal/Newspaper Antarc* Antarctic Directory of Open Access Journals: DOAJ Articles Antarctic The Astrophysical Journal 947 2 58 |
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Open Polar |
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Directory of Open Access Journals: DOAJ Articles |
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ftdoajarticles |
language |
English |
topic |
Supernovae Nucleosynthesis Mass spectrometry Astrophysical dust processes Astrophysics QB460-466 |
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Supernovae Nucleosynthesis Mass spectrometry Astrophysical dust processes Astrophysics QB460-466 Adrienne F. Ertel Brian J. Fry Brian D. Fields John Ellis Supernova Dust Evolution Probed by Deep-sea 60Fe Time History |
topic_facet |
Supernovae Nucleosynthesis Mass spectrometry Astrophysical dust processes Astrophysics QB460-466 |
description |
There is a wealth of data on live, undecayed ^60 Fe ( t _1/2 = 2.6 Myr) in deep-sea deposits, the lunar regolith, cosmic rays, and Antarctic snow, which is interpreted as originating from the recent explosions of at least two near-Earth supernovae. We use the ^60 Fe profiles in deep-sea sediments to estimate the timescale of supernova debris deposition beginning ∼3 Myr ago. The available data admits a variety of different profile functions, but in all cases the best-fit ^60 Fe pulse durations are >1.6 Myr when all the data is combined. This timescale far exceeds the ≲0.1 Myr pulse that would be expected if ^60 Fe was entrained in the supernova blast wave plasma. We interpret the long signal duration as evidence that ^60 Fe arrives in the form of supernova dust, whose dynamics are separate from but coupled to the evolution of the blast plasma. In this framework, the >1.6 Myr is that for dust stopping due to drag forces. This scenario is consistent with the simulations in Fry et al. (2020), where the dust is magnetically trapped in supernova remnants and thereby confined around regions of the remnant dominated by supernova ejects, where magnetic fields are low. This picture fits naturally with models of cosmic-ray injection of refractory elements as sputtered supernova dust grains and implies that the recent ^60 Fe detections in cosmic rays complement the fragments of grains that survived to arrive on the Earth and Moon. Finally, we present possible tests for this scenario. |
format |
Article in Journal/Newspaper |
author |
Adrienne F. Ertel Brian J. Fry Brian D. Fields John Ellis |
author_facet |
Adrienne F. Ertel Brian J. Fry Brian D. Fields John Ellis |
author_sort |
Adrienne F. Ertel |
title |
Supernova Dust Evolution Probed by Deep-sea 60Fe Time History |
title_short |
Supernova Dust Evolution Probed by Deep-sea 60Fe Time History |
title_full |
Supernova Dust Evolution Probed by Deep-sea 60Fe Time History |
title_fullStr |
Supernova Dust Evolution Probed by Deep-sea 60Fe Time History |
title_full_unstemmed |
Supernova Dust Evolution Probed by Deep-sea 60Fe Time History |
title_sort |
supernova dust evolution probed by deep-sea 60fe time history |
publisher |
IOP Publishing |
publishDate |
2023 |
url |
https://doi.org/10.3847/1538-4357/acb699 https://doaj.org/article/ab41f387300f4d1eb74ed1292cf6a041 |
geographic |
Antarctic |
geographic_facet |
Antarctic |
genre |
Antarc* Antarctic |
genre_facet |
Antarc* Antarctic |
op_source |
The Astrophysical Journal, Vol 947, Iss 2, p 58 (2023) |
op_relation |
https://doi.org/10.3847/1538-4357/acb699 https://doaj.org/toc/1538-4357 doi:10.3847/1538-4357/acb699 1538-4357 https://doaj.org/article/ab41f387300f4d1eb74ed1292cf6a041 |
op_doi |
https://doi.org/10.3847/1538-4357/acb699 |
container_title |
The Astrophysical Journal |
container_volume |
947 |
container_issue |
2 |
container_start_page |
58 |
_version_ |
1779309735099498496 |