Angular momentum transport in astrophysical disks

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Abstract

The evolution of astrophysical disks is dominated by instabilities of gravity perturbations (e.g., those produced by a spontaneous disturbance). We develop a hydrodynamic theory of nonresonant Jeans instability in a dynamically cold subsystem (identified as the gaseous component) of a disk. We show analytically that gravitationally unstable systems, such as disks of rotationally supported galaxies, protoplanetary disks, and, finally, the solar nebula are efficient at transporting mass and angular momentum: already on a timescale of on the order of 2-3 rotational periods an unstable disk sees a large portion of its angular momentum transferred outward, and mass transferred both inward and outward.

Original languageEnglish
Pages (from-to)L127-L130
JournalAstrophysical Journal
Volume672
Issue number2 PART 2
DOIs
StatePublished - 1 Jan 2008

Keywords

  • Formation
  • Formation - Solar system
  • Galaxies
  • Kinematics and dynamics-planetary systems

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