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Triggered Star Formation inside the Shell of a Wolf-Rayet Bubble as the Origin of the Solar System

Published online by Cambridge University Press:  13 January 2020

Vikram V. Dwarkadas Open the ORCID record for Vikram V. Dwarkadas [Opens in a new window] ,
Nicolas Dauphas ,
Bradley Meyer ,
Peter Boyajian  and
Michael Bojazi
Vikram V. Dwarkadas
Affiliation:
University of Chicago, Chicago, IL, 60637 email: vikram@astro.uchicago.edu
Nicolas Dauphas
Affiliation:
University of Chicago, Chicago, IL, 60637 email: vikram@astro.uchicago.edu
Bradley Meyer
Affiliation:
Clemson University
Peter Boyajian
Affiliation:
University of Chicago, Chicago, IL, 60637 email: vikram@astro.uchicago.edu
Michael Bojazi
Affiliation:
Clemson University
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Abstract

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A constraint on Solar System formation is the high 26Al/27Al abundance ratio, 17 times higher than the average Galactic ratio, while the 60Fe/56Fe value was lower than the Galactic value. This challenges the assumption that a nearby supernova was responsible for the injection of these short-lived radionuclides into the early Solar System. We suggest that the Solar System was formed by triggered star formation at the edge of a Wolf-Rayet (W-R) bubble. We discuss the details of various processes within the model using numerical simulations, and analytic and semi-analytic calculations, and conclude that it is a viable model that can explain the initial abundances of 26Al and 60Fe. We estimate that 1%-16% of all Sun-like stars could have formed in such a setting.

Keywords

methods: analyticalmethods: numericalSolar System: formationstars: mass lossstars: windsoutflowsstars: Wolf-RayetISM: bubbles
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. 78 - 82
Copyright
© International Astronomical Union 2020 

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