ACTIVE GALAXIES AND QUASISTELLAR OBJECTS, JETS
Jean A. Eilek
Fundamental considerations of the energy supply in large-scale
extragalactic radio sources(``radio galaxies'') led astronomers to
predict that these sources should contain jets or beams that connect
the nucleus of the parent galaxy to the large-scale radio lobes.
These predictions were made shortly after the discovery of the
sources; their proof had to wait for the advent of radio
interferometers. Interferometers produced much higher quality radio
images than those available from early radio telescopes; the jets were
indeed found to be a major feature of all radio galaxies.
RADIO GALAXIES
Strong, double radio sources were first identified with external
galaxies in the 1950s, and in fact the search for optical
identifications of radio sources led to the discovery of quasars in
the 1960s. Over the following couple of decades, data were
accumulated on large numbers of radio galaxies, and a basic picture of
these sources emerged. Radio galaxies generally consist of two fairly
symmetric radio-luminous ``lobes''; the parent galaxy lies midway
between the lobes. The parent galaxy is almost always a giant
elliptical, at least at nearby redshifts; it can also be the dominant
central galaxy in a cluster of galaxies. At high redshift, double
radio sources are found to be associated with quasars (for which the
classification of the parent galaxy is still a matter of discussion)
and with distorted distant galaxies. Not all active galaxies produce
large and powerful radio jets, however. Active nuclei in spirals are
much weaker radio sources, which may involve small jets or may only
lead to uncollimated core sources. Most QSOs are not strong radio
sources; only about 1 in 10 produces the dramatic radio jets which are
the topic of this entry.
The radio structure is typically a few to 10 times the sizes of the
parent galaxy (ie. , 50-200 kiloparsecs (kpc)]; however, smaller (down
to 10 kpc) and much larger (up to 1 Mpc) examples are known. The
spectrum and polarization of the radio emission suggest that the
radiation mechanism is incoherent synchrotron emission, produced by
relativistic electrons spiraling in magnetic fields. Knowledge of the
emission mechanisms allows us to estimate the minimum energy contained
in the radio lobes (that part of it in relativistic electrons and the
magnetic field). This minimum energy, divided by the luminosity,
predicts a very short lifetime. Thus, unless we are seeing these
sources at a very special epoch, there must be either a great deal of
energy hidden in the lobes, or a continuous resupply of energy to the
lobes. One way of doing this is through a ``pipeline'' from the
galactic nucleus; there jets were therefore predicted fairly soon
after radio galaxies were discovered.
Although optical jets had been
known in M87 (a nearby ical elliptical galaxy) and in 3C 273 (a
quasar) for some time, our ding understanding of jets really grew only
after interferometer observations found that jets are common in radio
galaxies and in radio-strong quasars. There are now enough data
(several hundred radio jets are currently known) to justify studying
the basic physics of the jets and to test models against observations.
OBSERVATIONS OF RADIO JETS
This section summarizes important trends in the data. Two examples
are shown, Fig. 1 (3C 175, a 200-kpc-long
source, associated with a
quasar) and Fig. 2 (M87, a 3-kpc-long jet in the
core of a nearby
galaxy). Nearly all of our information on jets comes from radio
observations; only a few jets have been detected at other frequencies
(optical and x-ray).
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Figure 1. Very Large Array (VLA) image of
the radio emission from the quasar 3C 175. The radio source is
approximately 200 Mpc end-to-end. The bright central coincides with the
optical qausar, which is at a redshift of 0.77. Several knots of
enhanced emission can be seen in the jet. The ``snowy'' background in
the image is the noise level of the observation. (Courtesy of
A. Bridle.)
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Almost all of our direct information on jets relates to the
morphology and luminosity of the jets. The jets are very well
collimated structures, with opening angles of no more than a few
degrees; jets in more powerful sources tend to have smaller opening
angles. The jets often remain straight over their entire length. On
the other hand, they can show small wiggles (which do not change the
direction significantly), or they may show gradual or sharp bends
(which do change the jet direction). These bends, small or large,
generally do not disrupt the jet; if the jet is flow is a flow this
flow can turn corners.
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Figure 2. VLA image of the radio emission
from the inner part of the galaxy M87. The jet shown here is about 3
kpc long; it emanates from a source in the core of the galaxy, seen at
the left of this image. Thsi jet sits in the center of a nearby
elliptical galaxy, which is in the Virgo cluster at a distance of
approximately 20 megaparsecs. Complex substructure can be seen in the
jet, as well as a sudden transition from well-collimated to more
disordered flow. Other radio data (not present here) show that the jet
sits inside a large envelope of diffuse radio emission. The ``rings''
around the core and the ``shadows'' above and below the jet are
artifacts of the telescope response and the data reduction
process. (Courtesy of F. N. Owen.)
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In higher-power radio sources, the jets end in ``hot spots'' (small,
bright regions) at the outer edges of the radio lobes. If the jet is
a flow - most likely supersonic in high-power sources - the hot spot might
be where it meets the ambient medium and decelerates through a shock
transition. The radio lobes must then be backflow of the shocked jet
material (perhaps mixed with the surrounding extragalactic gas).
In lower-power radio Sources, the jets broaden and brighten as they
enter the lobes; the surface brightness of the lobes then decays going
away from the galaxy (this is opposite to the surface brightness in
high-power sources). The broadening and brightening can be either
sudden or gradual. If the jet is a flow - perhaps transonic or subsonic
in these sources - the broadening and brightening may represent
deceleration and the onset of turbulence.
Most jets are barely resolved or unresolved, so little can be said in
general about substructure within the jets. The few jets that have
been resolved, however, show dramatic substructure: bright knots, what
appear to be twisted helices of emission, or surface emission (e.g.,
the jet in M87, Fig. 2). It seems
likely that complex substructure
will prove to be the rule rather than the exception.
The basic working model of jets is that they represent an outflow of
matter and energy from the nucleus. However, there has been no direct
measurement of an outflow of jet material (because no emission lines
are seen, Doppler shifts cannot be measured). Proper motion of bright
knots has been detected. Many parsec-scale nuclear jets have been
observed by very long baseline interferometry and motion of bright
knots is commonly detected. The knots move away from the nucleus, at
apparent velocities (projected on the sky) of 2 to 10 times the speed
of light, c. This is believed to result from a speed close to c in a
jet lying close to the observer's line of sight; light travel effects
can account for the apparent superlight speeds. Proper motion has
been searched for from the kiloparsec-scale jet in M87. The data up
to 1990 rule out velocities greater than c (again projected on the
sky); detection of sublight speed proper motion has not yet been
confirmed in this source. It is important to note that these are not
necessarily detections of a material flow speed; they could equally
well be measuring a pattern speed (such as traveling wave).
Another indirect measure of jet speed is possible: the measurement of
side-to-side brightness ratios for the two jets in a particular
source. High-power jets are often asymmetric, with sidedness ratios
ranging from a few to several tens. This is especially true in quasar
jets, but is also seen in high-power radio galaxies.
One possible explanation of this (although not the only one) is that
the sidedness is due to relativistic beaming of the emitted radiation.
A pair of jets, each moving at a velocity v = c, of equal
intrinsic
luminosity, will have an apparent brightness ratio given by
(1 - cos )x, where
x lies between 2 and 3 (depending on the spectrum of
the radio emission) and is
the angle between the jet and the
observer's line of sight. Thus, for cos = 1 (i.e.: for jets moving
with v c
and lying close to the line of sight), strong
side-to-side asymmetrics are seen.
This can, in principle, be used to estimate the average jet velocity
in a set of radio galaxies or quasars. If one has a set of jets whose
orientation (relative to the line of sight) is known to be random (the
``parent sample''), their average sidedness will provide a measure of
their average velocity. This type of analysis has been attempted,
using different sets of observations, and the mean lorentz factor of
the jets [ = (1
- 2)-1/2] has been estimated at between
2 and 10. This
analysis is not yet conclusive, however; several problems remain.
First, it is not yet clear that a proper parent sample exists, so that
the statistical arguments may not be conclusive. Second, it has not
been established that the detailed jet structures seen in high-quality
images are consistent with highly relativistic bulk flow. Third, the
deprojected length of some of the one-sided quasar jets must be
several megaparsecs, which is larger even than clusters of galaxies;
this may be an awkward consequence of the model. Thus the question of
sidedness is tantalizing, but has not yet produced conclusive evidence
on the jet speed.
THE PHYSICS OF RADIO JETS
Work on physical models of the jets is hampered by the fact that none
of the parameters that are likely to be important can be measured
directly. We have little information on the density, internal energy,
composition, velocity, or magnetic field in the jet material. (Note
that the synchrotron emissivity, which we can measure, is a nonlinear
function of the density and energy of the relativistic electrons, and
of the magnetic field. Early work hoped that detection of Faraday
rotation would provide independent information on the gas density and
magnetic field; however, almost all Faraday rotation detected so far
turns out to come from thermal gas surrounding the radio source. ) We
can, however, list some general considerations that any model of the
jets must satisfy.
The total energy supplied to the lobes, over the lifetime of the
source, must be at least as large as the current minimum energy
contained in the lobes plus the net energy radiated over the lifetime
of the source (perhaps 1060 erg; this estimate depends on the
details
of the model as well as on the estimated lifetime). The momentum flux
transported by the jet must be large enough to push the extragalactic
gas aside and establish the current size of the radio source. The
direction of the flow must remain nearly constant over the age of the
source (at least 107 yr, perhaps much longer).
The internal state of the plasma in the radio jet and lobes must be
consistent with the observed synchrotron luminosity. The relativistic
electrons are probably transported out from the galactic nucleus, and
may also be reaccelerated locally in the jet or lobes. These sources
are, in fact, distant laboratories for studying charged-particle
acceleration. The same mechanisms that accelerate cosmic rays, and
the energetic particles in solar flares and supernova remnants, are
likely to be operating in radio galaxies. Shocks and turbulence in
the radio source plasma are currently thought to be the most likely
mechanisms for accelerating the particles.
Models of the sources must also maintain the magnetic field strength
necessary to produce the observed radio synchrotron emission. Because
the plasma is highly conducting, induction will reduce magnetic fields
in the nuclear plasma to very low levels as this plasma expands into
the jet and lobes. It is very likely, therefore, that turbulence in
the plasma maintains a dynamo, which amplifies the magnetic field in
the jet and lobes. If so, this will involve the same processes that
operate to maintain the magnetic field in the Sun and in most of the
planets in the solar system.
Most current models of radio jets assume the jets can be descibed in
terms of directed fluid flow, similar to buoyant smoke plumes or to
supersonic jet-engine exhausts. Numerical simulations, combined with
analytic modeling, have had quite a bit of success in reproducing the
morphology of the sources. This work suggests the high-power sources
are driven by jets that are very supersonic and much less dense than
than the medium into which they propagate. Lower-power sources are
thought to be transonic or subsonic flows; turbulence develops in the
flow, which entrains the surrounding gas and decelerates the flow.
Alternative models have been proposed for these jets, however. It
has been suggested that the jets are magnetohydrodynamic rather than
hydrodynamic phenomena. In these models, the jet morphology and
propagation are controlled as much or more by magnetic and electric
forces as by the inertia and turbulent stresses that govern fluid
flow. In addition, it has been proposed that the jets are
collisionless particle beams - where only electric and magnetic forces
on charged particles are important in the jet dynamics.
At this point, there are more competing models of jets than there
are ways to discriminate between them. The next major advance in this
field might involve a more specific comparison of the data with the
models, than has been done up to now, in order to verify or disprove
some of the theories described previously. When this is accomplished,
the jets should be important tools for studying other astrophysical
problems. They will provide probes of their local environment,
through their interaction with the extragalactic gas, and with the
local gravitational potential. But, perhaps their most interesting
use will be to study the central engine in active galactic nuclei; why
do some (but not all) active nuclei produce these jets, and how do
they do so?
Additional Reading
Begelman, M. C., Blandford, R. D., and Rees, M. J. (1984). Theory of
extragalactic radio sources. Rev. Mod. Phys. 56 255.
Bridle, A. H. and Perley, R. P. (1984). Extragalactic radio jets.
Ann. Rev. Astro. 22 319
De Young, D. S. (1976). Extended extragalactic radio sources. Ann Rev.
Astron. Ap. 14 447.
Hughes, P., ed. (1991). Beams and jets in
Astrophysics. Cambridge University Press, Cambridge.
Kellermann, K. I. and Owen, F. N. (1988). Radio galaxies and
quasars. In Galactic and Extragalactic Radio Altronomy, G. L.
Verschuur and K. I. Kellermann, eds. Springer-Verlag, New York, p.
563.
Miley, C. (1980). The structure of extended extragalactic radio
sources. Ann. Rev. Astron. Ap. 18 165.
See also Active Galaxies and Quasistellar Objects, Superluminal
Motion; Galaxies, Radio Emission; Jets, Theory of.