Annu. Rev. Astron. Astrophys. 1996. 34:
155-206 Copyright © 1996 by Annual Reviews. All rights reserved |
We now discuss the mechanisms generating large-scale fields that have been presented in the previous section. We begin by considering first the small-scale magnetic fields.
4.1. Random Magnetic Fields
The interstellar medium is turbulent and thus any embedded magnetic
field must have a random small-scale component. The presence of this
component is crucial in all theories of large-scale dynamo action.
There are several mechanisms that produce fluctuations
in the interstellar magnetic fields:
(a) tangling of the large-scale field by turbulence and from
Parker and thermal instabilities, (b) compression of ambient
magnetic fields by shock fronts associated
with supernova remnants and stellar winds,
and (c) self-generation of random magnetic fields by turbulence
(small-scale dynamo).
All of these mechanisms act together, and each imprints its own statistical
properties onto the magnetic fields.
The available observational and theoretical knowledge of random
magnetic fields and their maintenance in the ISM is rather poor.
Instead, crude descriptions in terms of global quantities such as
mean magnetic energy are usually applied.
A widely used concept is that of equipartition between the magnetic and
kinetic energy in the turbulence
(Kraichnan 1965,
Zweibel & McKee
1995),
which implies that the rms random magnetic field strength is
given by b
Beq
(4
v2)1/2, with v the
rms turbulent velocity and
the density. The
equipartition value is
significant in that the Lorentz force is expected to become comparable to
the forces driving the turbulent flow as equipartition is approached.
(This Beq is not to be confused with the equipartition
field strength
in Sections 2 and 3,
where equipartition refers to the estimated cosmic-ray
energy density used to deduce the field strength from the synchrotron
emission.) Interstellar turbulence is often treated as an
ensemble of random Alfvén waves
(McIvor 1977,
Ruzmaikin & Shukurov
1982,
McKee & Zweibel
1995) for which the equipartition holds
exactly. Magnetic fluctuations are accompanied also by fluctuations
in density
(Armstrong et al 1995),
so that other mechanisms, possibly
nonpropagating fluctuations, must contribute to the interstellar turbulence
(Higdon 1984).
The random magnetic fields in the Milky Way are typically 4-6 µG
(Ohno & Shibata
1993), close to Beq.
Another component of the random magnetic field, one that is associated with
interstellar (super) bubbles, is observed in the Milky Way
(Heiles 1989,
Heiles et al 1993,
Vallée 1993).
The magnetic field in HI shells, detected via the Zeeman effect,
seems to be concentrated in filaments with the magnetic pressure larger
than the gas pressure.
The field strength in magnetic bubbles around OB associations, as
obtained from
Faraday rotation measurements, follows the density dependence b
expected for a shocked medium.
The small-scale dynamo
(Kazantsev 1968,
Meneguzzi et al 1981)
must be an important source of interstellar random magnetic fields
(Sokoloff et al 1990).
A distinctive feature of this component of the interstellar field,
item (b) above, is that it is organized in intermittent
magnetic ropes of small filling factor and lengths comparable to the
correlation length of the turbulence (50-100 pc).
The rms strength of the magnetic fluctuations generated by this mechanism
is possibly close to the equipartition value, but the field within the
filaments may be significantly higher
(Belyanin et al 1993).
For example, three-dimensional simulations of convective small-scale
dynamo action at magnetic Reynolds numbers of about 1000
(Nordlund et al 1992) give
Brms = 0.4Beq and
Bmax = 3Beq.
We note that in the interstellar gas of elliptical galaxies
a small-scale dynamo may be the only source of magnetic fields,
generating random fields of µG strength and a
few hundred parsecs in scale
(Moss & Shukurov 1996).