Several important trends have been identified as a result of the analysis of cloud
rotational data in Sect. 3. It seems clear, in the first place, that angular velocity
vectors in isolated clouds and complexes show a preferential orientation with
respect to the galactic plane; a feature which would support an origin for cloud
angular momenta in galactic rotation. This trend is not however shared by
clumps and condensations within the clouds. Secondly, it appears that cloud
rotation may be important for the stability of a surprisingly large number of these
clouds, and influence observed aspect ratios. Thirdly, it appears that the trends
for angular velocity and specific angular momentum are inconsistent with
angular momentum conservation, turbulent vorticity, and models of
axisymmetric, isothermal, non-magnetic clouds. Finally, it appears that angular
momentum vectors for rings and (principally) disks possess a tendency towards
non-random orientation, whilst rotational stabilisation is likely also to be
important; characteristics which are to be found in neither clumps nor
condensations. It is also notable that trends in J/M, J and with cloud radius R
differ from those of other sub-groups in this study.
It would appear, in brief, that disks are generically different from most other
clouds investigated here; a feature which may argue for a physically distinct
evolutionary sequence and, in all probability, reflects their differing
spatio-kinematic structures. It is apparent, for instance, that these sources not only
display typically large aspect ratios (although intrinsic values of this parameter
are likely to be even greater), but also that angular velocities are among the most
extreme, and the proportionate mass of embedded stars
is substantial (viz.
Table 1). As a result, and more than for any other cloud subgroup, disk
momentum depends upon the proportion of angular momentum carried by the
stellar mass fraction, and the degree of angular momentum transfer that has
occurred during protostellar contraction and subsequent evolution.
Although we have previously noted that turbulent vorticity gradients appear too
large to explain observed overall trends in , this is less the case for certain
cloud subgroups. In particular, the variation in dln
/dlnR = -0.67 predicted by
Fleck & Clark (1981) is not too different from that estimated for clouds (
) and condensations (
) taken separately.
The theory of Fleck and Clark requires however to be somewhat revised. In
particular, these authors assume strict energy cascade from large to small
turbulent eddy scales, whence turbulent velocity . In reality,
however, it seems that most of the clouds in this study are likely to be
characterised by supersonic turbulence (e.g. Myers 1983), and compressible
fluid interactions, whence
(R) may depart considerably from the trend
predicted by Kolmogoroff theory (Fleck 1983).
If, in place of this, one therefore employs the observed relation (see
for instance Myers (1983), and also the recent commentary by Phillips 1998), it
is then possible to evaluate a revised vorticity gradient dln
/dlnR = -0.5.
Although this latter parameter is somewhat greater than supposed before, it
would still (within uncertainties) be consistent with the relations noted for clouds
and condensations. In the case of condensations alone, therefore, it may be
possible to comprehend observed variations in rotational parameters in terms of
turbulent interactions. Such an explanation is likely to be less relevant in the case
of isolated clouds and complexes, however, given the orientational disposition of
their vectors .
It may also, on the other hand, be possible to explain certain of the functional
trends in rotation in terms of magnetic braking. Thus, where cloud fields are
appreciably greater than in the intercloud medium, and the density contrast
between cloud and exterior medium is given by , angular momentum would
be transferred outwards over a time-scale (Gillis et al. 1974, 1979;
Mestel & Paris 1979, 1984)
![]() |
(6) |
where the free-fall timescale
![]() |
(7) |
How does this compare with observations? The first characteristic to note is that
the gradient dln(J/M)/d is actually less than would be predicted for
isothermal models of non-magnetic rotating clouds. If one assumes, on the other
hand, that the logarithmic decrement in J/M arises primarily from magnetic
braking, and that there is an evolutionary trend from large to small cloud
structures, then a fractional reduction in specific angular momentum
would imply comparatively large radial changes
. It is apparent, in brief, that the decrement in J/M is not only uniform
and continuous in R and M, but appears also to be comparatively shallow; we
perceive no evidence for the strong magnetic braking which has been presumed
heretofore.
Several routes might be suggested whereby this problem could be side-stepped.
Thus, it is possible to assume that values B have been greatly overestimated; a
presumption which seems unlikely given the observations of this parameter
through Zeeman splitting (cf. Myers & Goodman 1988). An alternative
possibility is that a large fraction of clouds are magnetically supercritical, and
possess density contrasts , leading to reduced values of
(McKee et al. 1993); a situation which may be particularly applicable to GMC's
(McKee
1989).
Finally, we note that cloud contraction velocities (where
is the Alfven
velocity) would lead to the trapping of Alfven waves (Mouschovias 1989), and a
considerable reduction in the rate of angular momentum transfer. In particular,
given that
![]() |
(8) |
then for G we obtain
(R/pc)0.78 km s-1 (where we have also
substituted for M(R) from Table 2). Given also that free-fall collapse velocities
km s-1, then
for
pc. Trapping
may therefore be possible over comparatively short periods, where contraction
occurs at velocities comparable or greater than the free fall velocity
- a
situation which may, in turn, arise through external cloud compression by winds
and expanding shells (e.g. Elmegreen & Lada 1977; although note that radial
decrements in
are likely to be less steep given a dependency
,
(Gordon 1988)). The mean velocity of contraction for clouds taken as a
whole, on the other hand, is on the order of
km s-1,
where
yr-1 is the mean galactic rate of star formation,
is the
efficiency of star formation (Vrba 1977), and
is the mass of gas in
the form of molecular complexes (Solomon & Sanders 1980). The parameter
(which may be regarded as lower limit velocity for quiescent and
continuous contraction) is therefore only a little less than
for moderately
sized clouds.
It is therefore conceivable that a trapping mechanism of kind noted above may indeed operate to reduce rates of angular momentum transfer; although the effectiveness of this process is undoubtedly enhanced where contraction proceeds in fits and starts, rather than through a uniform global decrease in radius.
Finally, we have failed in the above discussion to address several outstanding
questions, including the unusually close correlation between angular momentum
J and non-virial cloud mass M (Fig. 6), and the strange disparity in rotational
properties between disks, and both clumps/condensations and larger cloud
structures. In this latter respect, we note that one conceivable solution to the
(possible) orientational disparity between clumps/condensations and disks may
be that clumps, after all, are not rotating; that despite the attribution of rotation to
these features in the literature, we are in fact (say) witnessing the superposition
of differing, unrelated features. A problem with this supposition, however, is that
the broad trends in , J, and J/M noted for clumps and condensations are also
closely similar to those determined for clouds - and not too far removed from
those for disks as well (although to be sure, disks are in this respect somewhat
different from all other subgroups). Such a correspondence would not be
anticipated were gradients to arise from random clump superposition.
This can be expressed in a slightly more precise way. Thus, if we assume that
projected clump radii are, in the mean, invariant with cloud size, and that the
mean separation between unresolved clump-pairs is also constant (consistent
with the approximate invariance in cloud column densities), then the typical
angular velocity attributed to such superpositions would be
(where
is the line of sight velocity dispersion due to turbulence). If we
assume virial stability, and employ a relation dln
/dlnM = 0.73 based on a
least squares analysis of the present results (thermal velocity contributions to
line width can normally be regarded as small, and have been ignored (viz.
Myers 1983)), then cloud mass
. As a consequence, one would then
anticipate
, and (given
from Table 2)
. These
relations are not consistent with the trends noted in Sect. 3.
On the other hand, it is by no means unreasonable that clump orientations should
be so disordered; supersonic and magnetic interactions are sufficient to ensure
appreciable orientational randomisation of the angular velocity vectors . The
real mystery, in all probability, is why fossil echoes of prior orientations should
be retained by disk-like structures alone.
Copyright The European Southern Observatory (ESO)