Magnetohy drodynamics of Population III star formation

Masahiro N. Machida, Kazuyuki Omukai, Tomoaki Matsumoto

Research output: Chapter in Book/Report/Conference proceedingConference contributionpeer-review


The evolution of collapsing primordial clouds and the formation of Population III (Pop III) protostars are investigated with three-dimensional ideal MHD simulations. We follow the collapse of parsec-sized primordial clouds down to the formation of protostars on sub-AU scales. Pop III protostar formation is characterized by the ratio of rotational to magnetic energy of the natal cloud. When the rotational energy is larger than the magnetic energy, fragmentation occurs prior to the formation of the protostar, and a binary or multiple system appears. When the magnetic energy is greater than the rotational energy, a strong (> 100 km s-1) jet is driven by the circumstellar disk around the protostar, which does not fragment. Thus, even in the early universe, magnetic fields play an important role in the star formation process.

Original languageEnglish
Title of host publicationFirst Stars and Galaxies
Subtitle of host publicationChallenges for the Next Decade
Number of pages6
Publication statusPublished - 2010
Event1st Stars and Galaxies: Challenges for the Next Decade - Austin, TX, United States
Duration: 2010 Mar 82010 Mar 11

Publication series

NameAIP Conference Proceedings
ISSN (Print)0094-243X
ISSN (Electronic)1551-7616


Conference1st Stars and Galaxies: Challenges for the Next Decade
Country/TerritoryUnited States
CityAustin, TX


  • Binaries:general
  • Cosmology:theory
  • Early universe
  • ISM
  • Jets and outflows


Dive into the research topics of 'Magnetohy drodynamics of Population III star formation'. Together they form a unique fingerprint.

Cite this