Journal
ASTROPHYSICAL JOURNAL
Volume 782, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/782/2/108
Keywords
early universe; H II regions; magnetic fields; radiative transfer
Categories
Funding
- Ministry of Education, Science, Sports, and Culture [22540295]
- Grants-in-Aid for Scientific Research [22540295, 25800102] Funding Source: KAKEN
Ask authors/readers for more resources
The generation process of a magnetic field around a proto-first-star is studied. Utilizing the recent numerical results of proto-first-star formation based on radiation hydrodynamics simulations, we assess the magnetic field strength generated by the radiative force and the Biermann battery effect. We find that a magnetic field of similar to 10(-9) G is generated on the surface of the accretion disk around the proto-first-star. The field strength on the accretion disk is smaller by two orders of magnitude than the critical value, above which the gravitational fragmentation of the disk is suppressed. Thus, the generated seed magnetic field hardly affect the dynamics of on-site first star formation directly, unless an efficient amplification process is taken into consideration. We also find that the generated magnetic field is continuously blown out from the disk on the outflows to the poles, that are driven by the thermal pressure of photoheated gas. The strength of the diffused magnetic field in low-density regions is similar to 10(-14)-10(-13) G at n(H) = 10(3) cm(-3), which could play an important role in the next generation star formation, as well as the seeds of the magnetic field in the present-day universe.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available