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Scientific paper
Sep 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..332..249s&link_type=abstract
The Fate of the Most Massive Stars, ASP Conference Series, Vol. 332, Proceedings of the conference held 23-28 May, 2004 in Grand
Other
Scientific paper
Recent theoretical studies consistently predict that the first (Pop III) stars had characteristic masses of 100-600 M&sun;, i.e. more than 100 times more massive than those observed today. The basis for this claim is that (i) the fragmentation scale of metal-free clouds is typically 103 M&sun; tep{Abel02,Bromm02}; (ii) because of the absence of dust grains the radiative feedback from the forming star is not strong enough to halt the accretion tep{Omukai03}; (iii) since accretion rate is as large as 10-2-10-3 M&sun; /yr, the star grows up to ≫ 100 M&sun; within its lifetime tep{Omukai03}. A number of indirect evidences seem to favor short-lived, very massive Pop III stars, which include the amplitude and anisotropy of the Near-Infrared Background, tep{Salvaterra03,Magliocchetti03} and the failure to find any zero-metallicity star in our Galaxy halo tep{Bond81}. On the other hand, observations in the present-day universe show that (Pop II/I) stars form according to a Salpeter initial mass function (IMF) with a characteristic mass of ˜ 1 M&sun;. This situation stimulates some fundamental questions: Has a transition from the early massive star formation mode characterizing Pop III stars to a ``normal'' one occurred ? When did it happen ? What physical process caused it ?
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