Ambipolar diffusion and star formation: Formation and contraction of axisymmetric cloud cores. II. Results

Robert A. Fiedler, Telemachos Ch Mouschovias

Research output: Contribution to journalArticle

Abstract

The problem of the formation and contraction of fragments (or cores) in magnetically supported parent molecular clouds was formulated in a previous paper. Three dimensionless free parameters appear in the evolution equations: the initial ratio of the free-fall and neutral-ion collision times (in the uniform reference state), vff.0, the exponent k in the relation between the ion and neutral densities ni ∝ nkn, and the initial ratio of the magnetic and thermal pressures, α0. The initial central mass-to-flux ratio in units of the critical value for gravitational collapse, μ0, enters through the initial conditions. We follow both the quasistatic and dynamic phases of contraction and demonstrate that ambipolar diffusion leads to self-initiated protostar formation ("quasistatic" meaning motion with negligible acceleration). A typical cloud core forms and contracts quasistatically on the flux-loss time scale until the central mass-to-flux ratio (dM/dΦB)c exceeds the critical value. During quasistatic contraction, the magnetic field lines are essentially "held in place" as the neutrals contract through them, and the field strength increases by less than a factor of 2. Despite subsequent dynamic contraction perpendicular to magnetic field lines, thermal pressure continues to balance gravity along field lines, hereby enforcing quasistatic contraction in this direction. We follow the contraction until the central density nc increases by a factor of 106 (typically from 3 × 102 to 3 × 108 cm-3). The envelope remains magnetically supported. The results from our parameter study show that decreasing vff.0 speeds up ambipolar diffusion shortens the quasistatic phase of contraction, and causes (dM/dΦB)c to increase by a greater amount above the critical value. The enhancement of the central magnetic field Bc, however, is not sensitive to the value of vff.0. A smaller k leads to progressively more rapid ambipolar diffusion as nc increases. Reducing μ0 lengthens the duration of the quasistatic phase and results in a larger reduction of a core's magnetic flux, but the dynamic phase of contraction is independent of μ0. The value of (dM/dΦB)c in our models is initially 1.9-16.3 times smaller than the critical value, but increases (because of ambipolar diffusion) by a factor of 10-50 by the time nc has increased by a factor ≈106. The value of α0 mainly affects the relaxation of clouds from their initial states into the corresponding equilibrium states under flux-freezing, in which α is related to μ0 by αc,eqμ20 ≈ constant.

Original languageEnglish (US)
Pages (from-to)680-700
Number of pages21
JournalAstrophysical Journal
Volume415
Issue number2
DOIs
StatePublished - Oct 1 1993

Fingerprint

ambipolar diffusion
contraction
star formation
magnetic field
magnetic fields
free fall
ion
protostars
gravitational collapse
molecular clouds
freezing
magnetic flux
field strength
envelopes
collision
fragments
exponents
gravity
gravitation
timescale

Keywords

  • Diffusion
  • Hydromagnetics
  • ISM: clouds
  • ISM: magnetic fields
  • Plasmas
  • Stars: formation

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Ambipolar diffusion and star formation : Formation and contraction of axisymmetric cloud cores. II. Results. / Fiedler, Robert A.; Mouschovias, Telemachos Ch.

In: Astrophysical Journal, Vol. 415, No. 2, 01.10.1993, p. 680-700.

Research output: Contribution to journalArticle

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