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Incidence of stellar rotation on the explosion mechanism of massive stars

Published online by Cambridge University Press:  17 October 2017

Rémi Kazeroni ,
Jérôme Guilet  and
Thierry Foglizzo
Rémi Kazeroni
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany email: [email protected] 2 Laboratoire AIM, CEA/DRF-CNRS-Université Paris Diderot, IRFU/Département d’Astrophysique, CEA-Saclay, F-91191, France
Jérôme Guilet
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany email: [email protected] 2
Thierry Foglizzo
Affiliation:
Laboratoire AIM, CEA/DRF-CNRS-Université Paris Diderot, IRFU/Département d’Astrophysique, CEA-Saclay, F-91191, France
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Abstract

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Hydrodynamical instabilities may either spin-up or down the pulsar formed in the collapse of a rotating massive star. Using numerical simulations of an idealized setup, we investigate the impact of progenitor rotation on the shock dynamics. The amplitude of the spiral mode of the Standing Accretion Shock Instability (SASI) increases with rotation only if the shock to the neutron star radii ratio is large enough. At large rotation rates, a corotation instability, also known as low-T/W, develops and leads to a more vigorous spiral mode. We estimate the range of stellar rotation rates for which pulsars are spun up or down by SASI. In the presence of a corotation instability, the spin-down efficiency is less than 30%. Given observational data, these results suggest that rapid progenitor rotation might not play a significant hydrodynamical role in the majority of core-collapse supernovae.

Keywords

hydrodynamicsinstabilitiesshock wavesstars: neutronstars: rotationsupernovae: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S331: Supernova 1987A:30 years later - Cosmic Rays and Nuclei from Supernovae and their aftermaths , February 2017 , pp. 113 - 118
Copyright
Copyright © International Astronomical Union 2017 

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