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Scientific paper
Nov 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1294...52c&link_type=abstract
THE FIRST STARS AND GALAXIES: CHALLENGES FOR THE NEXT DECADE. AIP Conference Proceedings, Volume 1294, pp. 52-55 (2010).
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Protostellar Clouds, Cosmology, Population Iii Stars, Hydrodynamics, Accretion Disks, Pre-Main Sequence Objects, Young Stellar Objects And Protostars, Origin And Formation Of The Universe, Population Iii Stars, Hydrodynamics, Infall, Accretion, And Accretion Disks
Scientific paper
We study the formation and evolution of the protostellar discs that form around the first stars in the Universe. Using sink particles, we replace the gravitationally bound gas at densities higher than 1015 cm-3 and radii greater than 3 AU from the central protostellar core, with an accreting point mass that is able to gravitationally interact with the surrounding gas. We find the disc is gravitationally (or `Toomre') unstable, and is dominated by a strong m = 2 spiral mode. Although the angular momentum transport is dominated by a combination of gravitational torques and Reynolds stresses, which are extremely efficient mechanisms, the disc is unable to process the infalling material and grows increasingly gravitationally unstable. During the build-up of the disc, the temperature in the gas is regulated by a combination of H2 line cooling, collision-induced emission and H2 dissociation, which together help to offset heating from the gravitational collapse and feedback from the protostar. Once the disc starts to fragment, H2 dissociation keeps the gas almost isothermal as the collapse of the fragment progresses. The fragmentation occurs when the protostar/disc system is only 230 yr old and at a distance of ~20 AU from its sibling, by which point the central protostar has a mass of ~1 Msolar. Given the angular momentum of the new protostellar system, it is likely that the protostars will grow to become a massive binary system.
Bromm Volker
Clark Paul C.
Glover Simon C. O.
Greif Thomas H.
Klessen Ralf S.
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