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Short-lived radioisotopes in meteorites from Galactic-scale correlated star formation

Published online by Cambridge University Press:  13 January 2020

Yusuke Fujimoto Open the ORCID record for Yusuke Fujimoto [Opens in a new window] ,
Mark R. Krumholz  and
Shogo Tachibana
Yusuke Fujimoto
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australian Capital Territory 2611, Australia email: [email protected]
Mark R. Krumholz
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University, Canberra, Australian Capital Territory 2611, Australia email: [email protected]
Shogo Tachibana
Affiliation:
UTokyo Organization for Planetary and Space Science (UTOPS), The University of Tokyo, 7-3-1 Hongo, Tokyo 113-0033, Japan
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Abstract

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Meteoritic evidence shows that the Solar system at birth contained significant quantities of short-lived radioisotopes (SLRs) such as 60Fe and 26Al produced in supernova explosions and in the Wolf-Rayet winds. Explaining how they travelled from these origin sites to the primitive Solar system before decaying is an outstanding problem. In this paper, we present a chemo-hydrodynamical simulation of the entire Milky Way to measure for the distribution of 60Fe/56Fe and 26Al/27Al ratios over all stars in the Galaxy. We show that the Solar abundance ratios are well within the normal range. We find that SLRs are abundant in newborn stars because star formation is correlated on Galactic scales, so that ejecta preferentially enrich atomic gas that will subsequently be accreted onto existing GMCs or will form new ones. Thus new generations of stars preferentially form in patches of the Galaxy contaminated by previous generations of stellar feedback.

Keywords

hydrodynamicsmethods: numericalGalaxy: diskISM: kinematics and dynamicsmeteorsmeteoroids
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S345: Origins: From the Protosun to the First Steps of Life , August 2018 , pp. 83 - 86
Copyright
© International Astronomical Union 2020 

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