Dust Formation in Very Massive Primordial Supernovae

Details Dust Formation in Very Massive Primordial Supernovae Dust Formation in Very Massive Primordial Supernovae

2003-07-04

arxiv.org/abs/astro-ph/0307087v2

Mon.Not.Roy.Astron.Soc.351:1379,2004

Astronomy and Astrophysics

Astrophysics

10 pages, 8 figures, accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2004.07876.x

At redshift z>5 Type II supernovae (SNII) are the only known dust sources with evolutionary timescales shorter than the Hubble time. We extend the model of dust formation in the ejecta of SNII by Todini & Ferrara (2001) to investigate the same process in pair-instability supernovae (PISN), which are though to arise from the explosion of the first, metal free, very massive (140-260 Msun) cosmic stars. We find that 15%-30% of the PISN progenitor mass is converted into dust, a value >10 times higher than for SNII; PISN dust depletion factors (fraction of produced metals locked into dust grains) range between 0.3 and 0.7. These conclusions depend very weakly on the mass of the PISN stellar progenitor, which instead affects considerably the composition and size distribution. For the assumed temperature evolution, grain condensation starts 150-200 days after the explosion; the dominant compounds for all progenitor masses are SiO2 and Mg2SiO4 while the contribution of amorphous carbon and magnetite grains grows with progenitor mass; typical grain sizes range between 0.001 and a few 0.1 micron and are always smaller than 1 micron. We give a brief discussion of the implications of dust formation for the IMF evolution of the first stars, cosmic reionization and the intergalactic medium.

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