TY - JOUR
T1 - The effects of convection criteria on the evolution of Population III stars and the detectability of their supernovae
AU - Lawlor, T. M.
AU - Young, T. R.
AU - Teffs, J.
AU - MacDonald, J.
N1 - Publisher Copyright:
© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2015/4/10
Y1 - 2015/4/10
N2 - The first stars continue to elude modern telescopes, but much has been accomplished in observing the glow of the first galaxies. As detection capabilities improve we will eventually resolve these galaxies, but hopes of observing an individual star remains dim for the foreseeable future. However, our first view of an individual first star may be possible due to its explosion. In this work, we present evolution calculations for Population III (Pop III) stars and their subsequent supernovae explosions. Our evolution models include a mass range of 15-100M⊙, each with initial heavy element abundance Z = 10-14. Our models are evolved from pre-main sequence through formation of an iron core, and thus near to core collapse. We find that modelling the evolution of these stars is very sensitive to the choice of convection criterion; here we provide evolution results using both the Schwarzschild and Ledoux criteria. We also use the final structure from our models for numerical simulation of their supernovae light curves using a radiation hydrodynamics code. In doing so, we estimate a lower bound of initial model mass that may be possible to observe in near future. We also find that our 40M⊙ Schwarzschild evolution model produces the brightest supernova peak and statistically should be themost frequently observed. At our highest redshift z=15, only the 60M⊙ Schwarzschild model at peak magnitude starts to rival the 40M⊙ model in brightness.
AB - The first stars continue to elude modern telescopes, but much has been accomplished in observing the glow of the first galaxies. As detection capabilities improve we will eventually resolve these galaxies, but hopes of observing an individual star remains dim for the foreseeable future. However, our first view of an individual first star may be possible due to its explosion. In this work, we present evolution calculations for Population III (Pop III) stars and their subsequent supernovae explosions. Our evolution models include a mass range of 15-100M⊙, each with initial heavy element abundance Z = 10-14. Our models are evolved from pre-main sequence through formation of an iron core, and thus near to core collapse. We find that modelling the evolution of these stars is very sensitive to the choice of convection criterion; here we provide evolution results using both the Schwarzschild and Ledoux criteria. We also use the final structure from our models for numerical simulation of their supernovae light curves using a radiation hydrodynamics code. In doing so, we estimate a lower bound of initial model mass that may be possible to observe in near future. We also find that our 40M⊙ Schwarzschild evolution model produces the brightest supernova peak and statistically should be themost frequently observed. At our highest redshift z=15, only the 60M⊙ Schwarzschild model at peak magnitude starts to rival the 40M⊙ model in brightness.
UR - http://www.scopus.com/inward/record.url?scp=84938117724&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84938117724&partnerID=8YFLogxK
U2 - 10.1093/mnras/stv628
DO - 10.1093/mnras/stv628
M3 - Article
AN - SCOPUS:84938117724
SN - 0035-8711
VL - 450
SP - 1618
EP - 1630
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -