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The evolution of red supergiants to supernovae

Published online by Cambridge University Press:  28 July 2017

Emma R. Beasor  and
Ben Davies
Emma R. Beasor
Affiliation:
Astrophysics Research Institute, Liverpool John Moores University, Liverpool, L3 5RF, UK email: [email protected]
Ben Davies
Affiliation:
Astrophysics Research Institute, Liverpool John Moores University, Liverpool, L3 5RF, UK email: [email protected]
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Abstract

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With red supergiants (RSGs) predicted to end their lives as Type IIP core collapse supernova (CCSN), their behaviour before explosion needs to be fully understood. Mass loss rates govern RSG evolution towards SN and have strong implications on the appearance of the resulting explosion. To study how the mass-loss rates change with the evolution of the star, we have measured the amount of circumstellar material around 19 RSGs in a coeval cluster. Our study has shown that mass loss rates ramp up throughout the lifetime of an RSG, with more evolved stars having mass loss rates a factor of 40 higher than early stage RSGs. Interestingly, we have also found evidence for an increase in circumstellar extinction throughout the RSG lifetime, meaning the most evolved stars are most severely affected. We find that, were the most evolved RSGs in NGC2100 to go SN, this extra extinction would cause the progenitor’s initial mass to be underestimated by up to 9M⊙.

Keywords

circumstellar matterstars: supergiantsstars: evolutionstars: mass-loss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 59 - 63
Copyright
Copyright © International Astronomical Union 2017 

References

Beasor, E. R. & Davies, B., 2016, MNRAS, 463, 1269 Google Scholar
de Jager, C., Nieuwenhuijzen, H., & der Hucht, KA, 1988, Astron. & Astrophys. Suppl. Series, 72, 259 Google Scholar
Fraser, M., et al. 2016, MNRAS, 456, L16 Google Scholar
Ekström, S., Georgy, C., Meynet, G., et al. 2012, Astron. & Astrophys., 537, A146 Google Scholar
Georgy, C., 2012, Astron. and Astrophys., 538, L8 Google Scholar
Georgy, C., Ekström, S., Eggenberger, P., et al. 2013, Astron. and Astrophys., 558, AI03 Google Scholar
Kochanek, C. S., 2015, MNRAS, 446, 1213 Google Scholar
Meynet, G. & Maeder, A., 2003, Astron. and Astrophys., 404, 975 Google Scholar
Meynet, G., et al. 2015, Astron. and Astrophys., 575, A60 Google Scholar
Reynolds, T., Fraser, M., & Gilmore, G, 2015, MNRAS, 453, 2885 Google Scholar
Smartt, S., Eldridge, J., Crockett, R., et al. 2009, MNRAS, 395, 1409 Google Scholar
Smartt, S., et al., 2015, Publ. of the Astron. Soc. of Australia, 32, e016 Google Scholar
Smith, N., Li, W., Filippenko, A., et al. 2011, MNRAS, 412, 1522 Google Scholar
Walmswell, & Eldridge, 2012, MNRAS, 419, 2054 Google Scholar
de Wit, W., et al. 2008, The Astrophys. J. Lett., 419, 2054 Google Scholar