2004/03/20 by Hideki Maki, Hajime Susa · 1 citation
Materials Science · Physics and Astronomy · #Accretion (finance) #Angular momentum #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Chemical and Physical Properties of Materials #Field (mathematics) #Field strength #Magnetic cloud #Magnetic field #Magnetic flux #Magnetic pressure #Magnetohydrodynamics #Turbulence #astro-ph
paper · pdf · doi:10.1086/421103
published as Astrophys.J. 609 (2004) 467-473 · 23 pages, 10 figures, accepted for publication in ApJ
arxiv created 2004/03/20 · openalex publication_date 2004/07/09 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We report on the strength of the seed magnetic flux of the accretion disk surrounding Population III stars. Themagnetic field in accretion disks might play an important role in the transport of angular momentum because of the turbulence induced by magnetorotational instability (MRI). On the other hand, since the primordial star-forming clouds contain no heavy elements or grains, they experience a very different thermal history and magnetic-field-dissipation history in the course of their gravitational contraction from those in the present-day star-forming molecular clouds. In order to assess the magnetic field strength in the accretion disk of Population III stars, we calculate the thermal history of the primordial collapsing clouds and investigate the coupling of the magnetic field with the primordial gas. As a result, we find that the magnetic field strongly couples with the primordial gas cloud throughout the collapse, i.e., the magnetic field is frozen to the gas, as long as the initial field strength satisfies B ≲ 10 -5 ( N H /10 3 cm -3 ) 0.55 G.