Super Massive Dark Stars Douglas Spolyar Fermi lab and The University of Chicago ApJ 705.1031S (2009) arXiv:0903.1724 D. Spolyar, P. Bodenheimer, K Freese, and P Gondolo Phys. Rev. Lett. 98, 010001 (2008) arXiv:0705.0521 D. Spolyar , K .Freese, and P. Gondolo JCAP,11,014F (2008) arXiv:0802.1724 K. Freese, D. Spolyar, and A. Aguirre arXiv:1002.2233 K. Freese, C. Ilie, D. Spolyar, M. Valluri, and P. Bodenhe Super Massive
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Super Massive Dark Stars Douglas Spolyar Fermi lab and The University of Chicago ApJ 705.1031S (2009) arXiv:0903.1724 D. Spolyar, P. Bodenheimer, K Freese,
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Super Massive Dark Stars
Douglas Spolyar
Fermi lab and The University of Chicago
ApJ 705.1031S (2009) arXiv:0903.1724D. Spolyar, P. Bodenheimer, K Freese, and P Gondolo
Phys. Rev. Lett. 98, 010001 (2008) arXiv:0705.0521
D. Spolyar , K .Freese, and P. Gondolo
JCAP,11,014F (2008) arXiv:0802.1724K. Freese, D. Spolyar, and A. Aguirre
arXiv:1002.2233K. Freese, C. Ilie, D. Spolyar, M. Valluri, and P. Bodenheimer
Super
Massive
Primordial Dark Star Basics
• Dark Matter (DM) in haloes can dramatically alter the formation of the first stars leading to a new stellar phase driven by DM annihilation.– Change: Re-ionization, Early Stellar Enrichment,
Formation of early Big Black Holes.– Discover DM.
• Properties– Very luminous up to ~ 1011 L – Relatively cool ~ 104 K– Can be very long lived ~ 108 years– Super Massive up to ~ 107 M – The more massive DS can be detectable with JWST
• Potentially this could be even larger due to additional orbits becoming chaotic as found in the Valluri et al. 2010– This effect will be further studied by (Freese and Valluri
2010)
• Hence DM is not annihilated away.• Dark Stars can become Super Massive
JWST limits
JWST Extended AC
As one example
Tentative Hints
• Eventually DS runs out of DM or Displaced from DM reservoir (star goes onto the main sequence and eventually collapses to a BHs – Progenitors of super massive black holes
• Get the metallicity right for low metallicity stars, IGM, ICM and M82– Depending upon spin of star