Matthew R. Bate and Ian A. Bonnell
This was the second large-scale calculation to be performed. The initial conditions were identical to those in the original calculation, except that the cloud's radius was reduced so that the gas was 9 times denser. This reduced the mean thermal Jeans mass of the cloud from 1 solar mass to 1/3 of a solar mass. The result was that the typical masses of the stars and brown dwarfs was also reduced by a factor of 3.
Copyright: The material on this page is the property of Matthew Bate. Any of my pictures and animations may be used freely for non-profit purposes (such as during scientific talks) as long as appropriate credit is given wherever they appear. Permission must be obtained from me before using them for any other purpose (e.g. pictures for publication in books).
Simulation & visualisation by Matthew Bate, University of Exeter unless stated otherwise.
Notes on formats:
Quicktime: Plays directly in Powerpoint only on an Apple computer. Can be played under Windows by downloading the FREE Quicktime player from Apple. Can be played under Unix/Linux using xanim.
MPEG-4: Can be played using Windows Media Player or Quicktime player. Small file size.
Movie comparing the evolutions of the original cloud (left) and the denser cloud (right).
Available formats for 61 second animation (30 frames/sec):
"The Origin of the Initial Mass Function and its Dependence on the Mean Jeans Mass in Molecular Clouds"
Bate, M. R., Bonnell, I. A., 2005, MNRAS, 356, 1201-1221. (Preprint)
The calculation models the collapse and fragmentation of a 50 solar mass molecular cloud that is 0.180 pc in diameter (approximately 0.6 light-years). At the initial temperature of 10 K with a mean molecular weight of 2.46, this results in an thermal Jeans mass of 1/3 of a solar mass. The free-fall time of the cloud is 63,000 years and the simulation covers 89,000 years.
The cloud is given an initial supersonic `turbulent' velocity field in the same manner as Ostriker, Stone & Gammie (2001). We generate a divergence-free random Gaussian velocity field with a power spectrum P(k) \propto k-4, where k is the wave-number. In three-dimensions, this results in a velocity dispersion that varies with distance, lambda, as sigma(lambda) \propto lambda1/2 in agreement with the observed Larson scaling relations for molecular clouds (Larson 1981). This power spectrum is slighly steeper than the Kolmogorov spectrum, P(k)\propto k11/3. Rather, it matches the amplitude scaling of Burgers supersonic turbulence associated with an ensemble of shocks (but differs from Burgers turbulence in that the initial phases are uncorrelated).
The calculation was performed using a parallel three-dimensional smoothed particle hydrodynamics (SPH) code with 3.5 million particles on the United Kingdom Astrophysical Fluids Facility (UKAFF). It took approximately 50000 CPU hours running on up to 64 processors. The SPH code was parallelised using OpenMP by M. Bate. The code uses sink particles (Bate, Bonnell & Price 1995) to model condensed objects (i.e. the stars and brown dwarfs). Sink particles are point masses that accrete bound gas that comes within a specified radius of them. This accretion radius is to set 5 AU. Thus, the calculation resolves circumstellar discs with radii down to approximately 10 AU. Binary systems are followed to separations as small as 1 AU.
High resolution, unannotated (1800x1800 pixel) versions that are suitable for
are available on request by emailing Matthew Bate at: mbate[@]astro.ex.ac.uk
Images will be placed below when available. Click on the images below to view medium resolution, annotated (600x600 pixel) versions.
Copyright: Matthew Bate, University of Exeter.