71 research outputs found
A Turbulent Model for the Interstellar Medium. II. Magnetic Fields and Rotation
We present results from two-dimensional numerical simulations of a supersonic
turbulent flow in the plane of the galactic disk, incorporating shear,
thresholded and discrete star formation (SF), self-gravity, rotation and
magnetic fields. A test of the model in the linear regime supports the results
of the linear theory of Elmegreen (1991). In the fully nonlinear turbulent
regime, while some results of the linear theory persist, new effects also
emerge. Some exclusively nonlinear effects are: a) Even though there is no
dynamo in 2D, the simulations are able to maintain or increase their net
magnetic energy in the presence of a seed uniform azimuthal component. b) A
well-defined power-law magnetic spectrum and an inverse magnetic cascade are
observed in the simulations, indicating full MHD turbulence. Thus, magnetic
field energy is generated in regions of SF and cascades up to the largest
scales. c) The field has a slight but noticeable tendency to be aligned with
density features. d) The magnetic field prevents HII regions from expanding
freely, as in the recent results of Slavin \& Cox (1993). e) A tendency to
exhibit {\it less} filamentary structures at stronger values of the uniform
component of the magnetic field is present in several magnetic runs. f) For
fiducial values of the parameters, the flow in general appears to be in rough
equipartition between magnetic and kinetic energy. There is no clear domination
of either the magnetic or the inertial forces. g) A median value of the
magnetic field strength within clouds is G, while for the
intercloud medium a value of G is found. Maximum contrasts of up to
a factor of are observed.Comment: Plain TeX file, 25 pages. Gzipped, tarred set of Tex file plus 17
figures and 3 tables (Postscript) available at
ftp://kepler.astroscu.unam.mx/incoming/enro/papers/mhdgturb.tar.g
Highly Compressible MHD Turbulence and Gravitational Collapse
We investigate the properties of highly compressible turbulence and its
ability to produce self-gravitating structures. The compressibility is
parameterized by an effective polytropic exponent gama-eff. In the limit of
small gama-eff, the density jump at shocks is shown to be of the order of
e^{M^2}, and the production of vorticity by the nonlinear terms appears to be
negligible. In the presence of self-gravity, we suggest that turbulence can
produce bound structures for gama-eff < 2(1-1/n), where 'n' is the typical
dimensionality of the turbulent compressions. We show, by means of numerical
simulations, that, for sufficiently small gama-eff, small-scale turbulent
density fluctuations eventually collapse even though the medium is globally
stable. This result is preserved in the presence of a magnetic field for
supercritical mass-to-flux ratios.Comment: 4 pages, 3 postscript figures. Latex, uses aipproc.sty Contribution
to the Conference Proc. of the 7th Annual Astrophysics Conference in
Maryland, STAR FORMATION, NEAR AND FAR, eds. Stephen S. Holt and Lee G. Mund
Influence of Cooling-Induced Compressibility on the Structure of Turbulent Flows and Gravitational Collapse
We investigate the properties of highly compressible turbulence, the
compressibility arising from a small effective polytropic exponent
due to cooling. In the limit of small , the density jump at shocks is
shown to be of the order of . Without self-gravity, the density
structures arising in the moderately compressible case consist mostly of
patches separated by shocks and behaving like waves, while in the highly
compressible case clearly defined long-lived object-like clouds emerge. When
the forcing in the momentum equation is purely compressible, the rotational
energy decays monotonically in time, indicating that the vortex-stretching term
is not efficient in transferring energy to rotational modes. This property may
be at the origin of the low amount of rotation found in interstellar clouds.
Vorticity production is found to rely heavily on the presence of additional
terms in the equations. In the presence of self-gravity, we suggest that
turbulence can produce bound structures for , where is
the typical dimensionality of the turbulent compressions. We support this
result by means of numerical simulations in which, for sufficiently small
, small-scale turbulent density fluctuations eventually collapse even
though the medium is globally stable. This result is preserved in the presence
of a magnetic field for supercritical mass-to-flux ratios. At larger polytropic
exponents, turbulence alone is not capable of producing bound structures, and
collapse can only occur when the medium is globally unstable. This mechanism is
a plausible candidate for the differentiation between primordial and
present-day stellar-cluster formation and for the low efficiency of star
formation.Comment: 20 pages, 12 Postscript figures. Uses aas2pp4.sty. Accepted in Ap
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