Other
Scientific paper
Aug 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009rmxac..36..272m&link_type=abstract
Magnetic Fields in the Universe II: From Laboratory and Stars to the Primordial Universe - Supplementary CD (Eds. A. Esquivel, J
Other
Early-Universe, Ism: Jets And Outflows, Mhd, Stars: Formation
Scientific paper
Outflow and fragmentation processes in collapsing primordial cloud are studied using three-dimensional MHD nested grid simulations. Starting from the number density of n_c ≃ 10^3 cm-3, we follow the evolution of rotating spherical cloud with uniform magnetic field up to the stellar density n_c ≃ 1022 cm-3. We calculate 36 models parameterizing the magnetic γ_0 and rotational β_0 energies. In the collapsing primordial clouds, cloud evolutions are characterized by the ratio of the rotational to magnetic energy, γ_0/β_0. The Lorentz force significantly affects the cloud evolution in the cloud with γ_0 > β_0, while the centrifugal force is more dominant than the Lorentz force in the cloud with β_0 > γ_0. When the cloud rotates rapidly with angular velocity of Ω_0 > 10-17 s-1 and β_0 > γ_0, fragmentation occurs before the protostar formation, but no outflow appears after the protostar formation. On the other hand, strong outflow appears after the protostar formation without fragmentation when the initial cloud has the strong magnetic field of B_0 > 10-9 G and γ_0 > β_0. Our results indicate that proto-Population III stars frequently show fragmentation and protostellar outflow. Thus, as well as the present-day star formation, Population III stars are born as the binary or multiple stellar system, and they can drive strong outflow which significantly disturb the interstellar medium and may induce the formation of next generation stars.
Inutsuka Shu-ichiro
Machida Masahiro N.
Matsumoto Toshio
Omukai Kazuyuki
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