The role of three-body H2 formation in the fragmentation of primordial gas

• Verfasst von: Dutta, Jayanta [VerfasserIn]
• Verfasst von: Nath, Biman B. [VerfasserIn]
• Verfasst von: Clark, Paul C. [VerfasserIn]
• Verfasst von: Klessen, Ralf S. [VerfasserIn]
• Titel: The role of three-body H2 formation in the fragmentation of primordial gas
• Verf.angabe: Jayanta Dutta, Biman B. Nath, Paul C. Clark and Ralf S. Klessen
• E-Jahr: 2015
• Jahr: 15 April 2015
• Umfang: 7 S.
• Fussnoten: Die Ziffer 2 ist im Titel tiefgestellt ; Gesehen am 02.07.2020
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2015
• Band/Heft Quelle: 450(2015), 1, Seite 202-208
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stv664
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 1703313895

Abstract

It has been shown that the behaviour of primordial gas collapsing in a dark matter minihalo can depend on the adopted choice of three-body H2 formation rate. The uncertainties in this rate span two orders of magnitude in the current literature, and so it remains a source of uncertainty in our knowledge of Population III star formation. Here, we investigate how the amount of fragmentation in primordial gas depends on the adopted three-body rate. We present the results of calculations that follow the chemical and thermal evolution of primordial gas as it collapses in two dark matter minihaloes. Our results on the effect of three-body rate on the evolution until the first protostar forms agree well with previous studies. However, our modified version of gadget-2 smoothed particle hydrodynamics also includes sink particles, which allows us to follow the initial evolution of the accretion disc that builds up on the centre of each halo, and capture the fragmentation in gas as well as its dependence on the adopted three-body H2 formation rate. We find that the fragmentation behaviour of the gas is only marginally affected by the choice of three-body rate co-efficient, and that halo-to-halo differences are of equal importance in affecting the final mass distribution of stars.