Collapse and fragmentation of rotating magnetized clouds - I. Magnetic flux-spin relation

Masahiro N. Machida, Tomoaki Matsumoto, Kohji Tomisaka, Tomoyuki Hanawa

Research output: Contribution to journalArticlepeer-review

94 Citations (Scopus)

Abstract

We discuss the evolution of the magnetic flux density and angular velocity in a molecular cloud core, on the basis of three-dimensional numerical simulations, in which a rotating magnetized cloud fragments and collapses to form a very dense optically thick core of >5 × 1010 cm -3. As the density increases towards the formation of the optically thick core, the magnetic flux density and angular velocity converge towards a single relationship between the two quantities. If the core is magnetically dominated its magnetic flux density approaches 1.5(n/5 × 1010 cm-3)1/2 mG, while if the core is rotationally dominated the angular velocity approaches 2.57 × 10-3 (n/5 × 1010 cm-3)1/2 yr-1, where n is the density of the gas. We also find that the ratio of the angular velocity to the magnetic flux density remains nearly constant until the density exceeds 5 × 1010 cm-3. Fragmentation of the very dense core and emergence of outflows from fragments will be shown in the subsequent paper.

Original languageEnglish
Pages (from-to)369-381
Number of pages13
JournalMonthly Notices of the Royal Astronomical Society
Volume362
Issue number2
DOIs
Publication statusPublished - Sep 11 2005
Externally publishedYes

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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