Observable Characteristics of Extraterrestrial Technological
Xenology Research Institute, 8256 Scottsdale Drive, Sacramento,
California 95828, USA.
Journal of the British Interplanetary
Society 38:106-112 (1985).
Advanced extraterrestrial civilisations which make extensive use of the
fusion fuel resources of their local star and planetary system have numerous
potentially observable characteristics. A circurnstellar nuclear fuel molecular
effusion cloud, the principal observable, rapidly dissociates and neutralises to
the atomic ground state, permitting the detection of hydrogen and tritium
hyperfine transition radio lines at 1420 MHz and 1516 MHz, respectively. The
negligible natural abundance of neutral atomic ground-state tritium suggests
that its hyperfine line, the "tritium waterspout" centred in the radio SETI
"waterhole" band, is ideal for interstellar communication and future SETI
searches. Other possible observables of advanced civilisations include
redshifted neutrino point sources, an artificial radio spectrum, anomalous
blackbody radiation, fission waste absorption lines, Doppler and stellar
spectral anomalies, and extraordinary magnetic fields.
Note: This web version is derived from an earlier draft of the paper
and may possibly differ in some substantial aspects from the final published
Conditions favourable to the development of life, intelligence, and civilisation
may be widespread in the Galaxy. Current programmes to detect these civilisations,
usually involving searches for powerful radio beacons, assume that alien societies
are purposely calling attention to themselves [1-3]. A better approach is to search
for the natural and anticipated byproducts of technological civilisation. This
avoids the tenuous assumption that extraterrestrial intelligences are actively
seeking contact or communication. Still, observing any but the most technologically
rapacious civilisations is difficult with present equipment .
One of the best ways to detect evidence of intelligent activity around
another star is to search for the material effluents of a spacefaring industrial
civilisation. The mainstay of technical civilisation is energy, and nuclear
fusion energy is the only plausible source for long-lived societies. The bulk of
planetary mass in a solar system is likely to be fusionable hydrogen and helium,
and the sun is a natural fusion reactor, so both may plausibly be employed.
However, solar energy alone may be regarded as insufficient because it restricts
the maximum rate of power consumption. Civilisations may wish to release greater
energies than the 1026-1027 watts developed by their sun.
Further, a G0 star typically emits 1044 joules during its main sequence
lifetime, whereas 1 Msun (solar mass) of fusion fuel carefully burned in
a controlled reactor releases 2 x 1041 joules - a considerable motivation
for astrophagy . [Ed. Note 1]
Advanced civilisations may turn to artificial fusion as a supplementary
source of energy. They will begin by cannibalising fusionables from their
planets to be burned in space has based reactors. Later, as their appetite for
energy grows, they may begin draining light element fusionables from their star.
G0 and G1 stars differ by 0.04 Msun, and
an artificial 1% mass deficit would be undetectable with current
instrumentation. Even a 10% deficit might go unnoticed because of our
incomplete understanding of stellar nucleosynthesis.
To recover the full energy theoretically available via fusion,
hydrogen atoms must be burned all the way to iron - Fe has the maximum binding
energy per nucleon, and thus represents the natural endpoint of all fusion
reactions. It is likely that heavy element products of fusion burning will be
used for various constructive purposes - artificial structures, atmospheres,
etc. - in addition to being burned for additional energy. But the closer the
endproducts approach Fe the less fusion energy they can generate per atom
burned, a law of diminishing marginal return which gives a very steep decrease
in fusion efficiency and rising fusion ignition temperatures with increasing
The most likely mode of fusion energy production is hydrogen burning to
4He at temperatures < 4 x 106 K, much like the PPI,
PPII, and PIII chains in stellar nucleosynthesis , which releases 80% of the
available nuclear binding energy in the fuel. Intermediate fusion products
include D (2H), T (3H), 3He, 7Li,
7Be, 8Be, and 8B. The temperature must be
raised to 100 x 106 K to burn 4He to 12C to
extract another 7% of the binding energy, and another 11% can be extracted only
by resorting to temperatures in excess of 109 K. The remaining 2% of
the binding energy escapes as neutrinos. Low temperature fuels will be burned in
preference to higher temperature fuels, with the latter perhaps stored in
tankage until required.
The D-3He reaction has been discussed as a potential propulsion
reaction for interstellar rockets , and Powell  argues that a large-scale
fusion-based civilisation will generate major surpluses of 3He. The
D-T reaction is the most widely studied because it is one of the easiest to
ignite, yields the second-highest energy of any fusion reaction after
D-3He, and is expected to be the fuel used in the first commercial
fusion reactors on Earth [9-. T decays to 3He with a half-life of
12.5 yr and B--emits the second-softest radiation after 187Re (~
103 watts/kg) of any radioactive element, thus may be regarded as a
biologically benign radioisotope. All three isotopes are plausible fusion fuel
candidates, in addition to H and 4He.
2. FUSION ENERGY
OBSERVABLESEmission characteristics of large-scale fusion energy
facilities in circurnstellar orbit include neutrons, accidental leakage of
high-energy plasma fuel/product mixtures, energetic neutrinos, contaminated
reactor wall components, gamma ray photons, and fusion fuel diffusion and
accidental spillage from storage bunkers. Reaction neutrons not absorbed by
breeder blankets and containment walls decay with a half-life of 750 sec into
high-energy protons and electrons which merge into the solar wind. Escaped
plasma particles cannot be slowed appreciably by normal processes and are too
energetic to de-ionise, dispersing rapidly into the interstellar medium along
heliomagnetic field lines and becoming indistinguishable from the primary cosmic
ray background. The neutrino (n) emission is observable
in principle as a point source with a 1-10 eV gravitational redshift relative to
solar emanations, but is unmeasurable using present-day detector technology
[12- and must await the development of high-resolution neutrino spectroscopy.
Contaminated components rich in artificial radionuclides are easily localised
and recycled, and hence arc not readily observable.
Gamma rays are produced in the reactions H(n, g)D,
H(D, g)3He, 3He(4He,
g)7Be, 7Li(p, g)24He, and 7Be(p, g)8Be, and by annihilation of positrons from p(p,
e+, v)D reactions, with energies less than I McV, but these should remain
confined within the reactor vessel. As few as 1035 photons/sec at
1017 Hz released isotropically from near a star 10 pc distant should
be detectable by the orbiting Einstein X-Ray Observatory, but such a flux rate
(~ 10-4 rad/sec, human lethality ~ 103 rads) would
probably render the circurnstellar shell biologically uninhabitable.
Fusion fuel effluence is plausibly observable over interstellar distances.
Fuel will be stored as diatomic ( H2, D2, T2)
or monoatomic (3He, 4He) gas at To£ 300 K. For hydrogen
gas emitted from an artificial circurnstellar shell of radius R (1 AU), the mean thermal velocity vo = (2kTo/2mp)1/2£ 1.57
km/sec << (2GM/R)1/2 = 42.2 km/sec = solar escape velocity,
where 2mp = hydrogen molecular mass, k is Boltzmann's constant and G
is the gravitation constant. Leakage will occur from the surface of the
circurnstellar shell at some rate DM kg/sec, and molecules are subsequently swept from
the solar system by solar wind particle collisions over the age of the
civilisation t. The most
abundant effluent is molecular hydrogen. We assume a thick cloud model such that
DM/mp >> Jw, the solar wind proton flux, and the entire
solar wind is absorbed by the cloud. If n is solar
wind proton number density near the circurnstellar shell and vp is solar wind
velocity at the shell, then Jw = 4pnvpR2 and
the rate of ejection of H2 is limited to Jw. Also, in a perfectly elastic collisional
sequence two protons in molecular form are ejected but one striking proton is
halted, for a net collisional ejection rate of 1/2 (4pnvpR2), So
the number of hydrogen molecules present in the artificial cloud NH2 ~ t[(DM/2mp)-(4pnvpR2)/2].
Molecular hydrogen is dissociated with an efficiency b = ( H2 residence time)/( H2
dissociation lifetime) = tr/td£ 1. For
photodestruction of H2 near the Sun, the best value is td = 5 x 1010 sec [14-. In the
thick cloud model tr = collision time
(tc) + ejection time (te) = (DMt/2mp)/
(4pnvpR2) + (Rb-R)/(vp/2), where Rb is the distance at which the effusion cloud
density falls to the interstellar background. Rb ~ R (no/nb)
1/2, where no is emission number density
near the shell (no = DM/4pR2(2mpvo)) and
nb = interstellar background number
density (~ 0.1 H cm-3), so Rb =
0.0026 DM 1/2 AU ~ radius of
heliopause. For R 1 AU, n
= 5 cm-3, vp ~ 400 km/sec, and
Rb ~ 100 AU: b = 1.0 for NH2³ 1046, 0.001 -
1.0 otherwise. Ionisation time for H in the Solar System is
1016-1017 sec [15-, as compared to 5 x 1010
sec for neutralisation of H+ . Hence fusion fuel leakage may produce a cloud
of fully neutralised atoms surrounding the target star if NH³ 1046,
with number of cloud atoms NH = 2 NH2 ~ DMt/mp. Other neutral fuel atoms may also be present
in varying lesser amounts.
What is DM? Fusion fuel
emissions are due largely to diffusion. Leakage rates are negligible if a small
number of very large fuel tanks are employed exclusively with radius r ~ 109 metres, near the theoretical maximum
structure size in a 1 AU heliocentric orbit for normal building materials .
However, small-scale users will require more convenient storage, of necessity a
very large number of small tanks. If the tanks are spherical and of thickness
t, the entire fleet holds a mass of gas Mg, and Do
is the classical diffusion coefficient, DM = 3DoMg/rt.
For hydrogen gas stored in a zirconium and tritium stored in stainless steel at
300 K, Do ~ 10-15
metres2-sec-1 [ [9-20]. Thus for example, Mg 10-4 MJ (Jovian mass) = 2 x 1023 kg, r = 10 m and t = 1 cm gives
DM = 1010 kg/sec
leakage. For t = 103 - 109 yr,
NH = 1047 - 1053
atoms, more if losses due to fuel processing and transfer operations are taken
into account. So diffusion arguments cannot rule out the existence of dense
artificial clouds near an extraterrestrial civilisation. In the most
fundamental limit, if Lf is total fusion
luminosity available to the civilisation, eH = fusion efficiency of hydrogen = 0.92% c2 joules/kg, and c =
speed of light, then DM£ Lf/eH. For Lf
~ Lsun (Solar luminosity), DM£
1012 kg/sec hydrogen leakage.
2.1 Natural BackgroundThe natural
background levels of neutral atomic H, D, T, 3He, and 4He
in the neighbourhood of a late-type main sequence star should approximate the
local interstellar medium. This is because even though all fusion isotopes are
emitted as solar wind ions and in solar flares [21-25], their velocities are too
high for braking or neutralisation to occur so there is no enhancement of local
background- D, T, and 3He are unimportant in advanced stellar
evolution , and the decay of tritium further ensures its natural absence in
the neutral atomic state.
Current measurements of natural neutral hydrogen abundances in the
interstellar medium range from 0.01-0.2 H cm-3 [27-29], with a mean
value usually taken as 0.1 H cm-3 [30-31]. Relative to hydrogen,
other candidate fusion fuel isotopes have the following natural abundances: D/H
= 2 x 10-6 - 3.5 x 10-4 [27, 32-36]; T/H <
10-11 ; 3He/H = 1-4 x 105 [32-33, 37]; and
4He/H = 0.069 - 0.1 [32-33]. The mean excess of fusion fuel hydrogen
atoms is NH/(4/3pRb3) ~ 7 x
10-14 DMt (H m-3), plausibly up to ~
1013 H m-3
2.2 Optical AnomaliesOptical
emission lines from an artificial light-element effusion cloud should not exist
because of the low cloud temperature and its relatively great distance from
possible sources of excitation. Observable absorption lines from the
hypothetical artificial cloud must have column densities exceeding those of
natural isotopes in the stellar atmosphere, which is unlikely. It is more
difficult to resolve the Lyman and Balmer lines of tritium from those of
deuterium than the deuterium lines from those of hydrogen, so although the
natural background of stellar neutral atomic tritium is negligible a column
density equivalent to that of naturallyoccurring stellar deuterium would
probably be required for tritium detection.
The D/H ratio has been determined by measuring interstellar deuterium
absorption in the UV, from orbiting observatories, in early-type stars and a few
late-type stars [27, 29, 35-36, 38]. Except in the case of Alpha Centauri,
measured H concentration and D/H in the line of sight appear consistent with
other observations and independent estimates for the interstellar medium. D has
yet to be detected in any stellar atmosphere [39-41]. 3He has been
discovered spectroscopically in only a few early-type peculiar stars [42-45] but
not in any later-type star except the Sun .
A final consideration is that to recognise a detected line as a local
anomaly, off-star comparison spectra are required - an impossible requirement
for optical absorption lines except in the rare case of a close visual binary.
2.3 Radio AnomaliesIn radio
frequencies, excited neutral atoms can be observed via recombination lines in
energetic environments such as HII regions . For instance, Palmer 
measured the H 109a recombination line at
5008.923 MHz and the 4He 109a recombination line at
5010.964 MHz to determine the relative abundance of helium in various nebulae.
From the earlier discussion, we expect that most leakage gas will be present in
the neutral atomic state and that recombination lines should be relatively weak.
2.3.1 Hyperfine Transition
LinesThe spontaneous magnetic dipole hyperfine transition is the
only plausible observational characteristic of an artificial, -neutral atomic
gas cloud of hydrogen or helium isotopes in the ground state. However, in
ground-state neutral helium, atomic electrons occupy all available spin states
and hence the spontaneous spin transition is prohibited by the Pauli exclusion
principle. The 3HeI line at 6739.7013 MHz  and the
corresponding 4HeI line arise from a hyperfine transition in the 2s
level, but excitation from 1s2, 1S0) to the
metastable triplet state (1s 2s, 3S1 requires 21.25 eV,
87% of the first ionisation energy, which is not available near late main
sequence stars. Among ground-state hydrogen isotopes, the deuterium hyperfine
line at 327.384 352 5222(17) MHz  has a brightness temperature below that of
the galactic synchrotron background, and hence could only be observed [34,
52-54] in absorption against very bright radio sources with state-of-the-art
equipment. This rules out the radio detection of artificial deuterium
enhancements near main sequence stars except in the rare instance of a normal
star occulting a very active radio source. Thus the neutral hydrogen
ground-state hyperfine transition line at 1420.405 751 768(3) MHz  and the
neutral tritium ground-state hyperfine line at 1516.701 9064(16) MHz  are
the two most promising observational candidates.
2.3.2 The Tritium
WaterspoutIt has most commonly been argued [1-3] that a
technological civilisation wishing to attract attention to itself to initiate
contact would employ a powerful radio beacon. Operation on a single narrowband
frequency against a quiet background would produce an obviously artificial
signal and make most efficient use of available transmitter power.
It is interesting that the tritium line lies almost in dead centre of the
traditional SETI "waterhole" region between the H and OH-spectral lines 11].
Thus, in addition to its value in a search for an artificial effusion cloud of
fusion tritium, the tritium hyperfine line is virtually unique in that its
detection alone is unambiguously artificial - no natural process could account
for its presence. There is no possibility of confusion with H 163a and H 162a
recombination lines, which lie at 1504.646 MHz and 1532.520 MHz, respectively,
nor with the two 4He lines 163a and 162a at 1505.259 MHz and 1533.144
Thus the tritium line is the ideal choice as an interstellar communication
frequency from the standpoint of acquisition. It is a unique signpost to
intelligence, leaping up out of the waterhole to form the "tritium waterspout."
The 1516 MHz tritium hyperfine line lies well outside major radio broadcasting
bands allocated to aviation communications, aeronautical and maritime satellites
at 1542.5-1558.5 MHz, and space operations telemetry at 1525-1535 MHz . A
variety of small fixed and mobile allocations exist between 1435-1525 MHz for
transmissions between fixed stations and land/coastal radar tracking systems, so
care must be taken to eliminate these potentially troublesome, though obvious,
sources of RFI.
Searches for purposeful narrowband CETI beacon signals .might also be
conducted near the hydrogen fine-structure transitions (e.g., 1058 MHz, 3250
MHz, 9910 MHz ) , the hyperfine lines for triplet-state 3HeI,
ground-state 3HeII (8665.649 867(10) MHz , metastable 2S1/2 state
3HeII (1083.354 9807(88) MHz ), and other hyperfine
lines for 3He , 4He, other elements, and various
neutral and ionised molecules . (Hyperfine transitions of excited neutral
atomic hydrogen isotopes all lie <200 MHz and thus would be difficult to
observe). However, many of these transitions may occur naturally  and none
is distinguished as especially attractive for SETI work.
2.3.3 Current Observational
StatusTo date only a handful of full-sky hydrogen-line surveys have
been performed at various ranges of galactic latitude, and there are only a few
published attempts to detect 21-cm radiation emission from stars (most of them
as part of SETI programmes). Of the more than two dozen SETI searches to date
. none is likely to have detected an artificial hydrogen cloud. Kraus
[63-64] and co-workers  are searching the entire sky rather than individual
stars, and correct their frequency of observation to the Galactic Standard of
Rest rather than the usual Local Standard of Rest. SETI observations by
Wielebinskii and Seiradakis in 1977 and by Israel and Tarter in 1981 employed
4-20 MHz bandwidths, so a cloud with a 10 KHz linewidth probably could not be
distinguished. Drake , Horowitz  and Tarter,  used narrow bandwidths
of 0.015-600 Hz/channel, which also would be unlikely to have detected a cloud.
The U.C. Berkeley SERENDIP programme was an all-sky parasitic search which could
not easily detect hydrogen-line enhancements at individual stars . Verschuur
 and Zuckerman with Palmer  searched numerous stars at the proper
frequencies and reasonable bandwidths but, as with many of the above studies,
failed to incorporate an off-star comparison measurement thus ruling out
detection of artificial clouds. Published data on three additional stars
surveyed by Verschurr  cannot rule out the possibility of a cloud up to
several flux units of intensity. Thus existing SETI searches cannot yet exclude
the existence of an artificial hydrogen cloud near even the closest stars. A
search for 21-cm excess would also be sensitive to the existence, but not the
content, of hypothetical radio messages possibly being transmitted to us now.
Individual stars have been observed in radio frequencies, including cm-band
generally [72-75], near 21-cm (e.g., 1415 MHz [76-77]), and 21-cm hydrogen line
observations. As even cm-band emissions of normal stars are expected to be too
weak to detect, searches have concentrated on peculiar and highly energetic
stars such as early-type stars, Of stars, Wolf-Rayet stars, various
emission-line and shell stars, magnetic variables, flare stars, and novae
[78-79]. A very few normal single stars have been observed at cm wavelengths,
with negative results except in the case of X1 Orionis, a G0 V star
10.0 pc from the Sun . Of the 21-cm hydrogen-line observations, the targets
have been A, B, and O stars with known or anticipated interstellar optical
absorption lines [81-85], sky positions near such stars , a few peculiar
stars such as Rho Ophiuchi , and general sky survey positions unrelated to
individual stars for galactic HI mapping. None of these would be sensitive to
artificial hydrogen clouds near Sunlike stars.
There is only one recent report of a search of individual stars at the
tritium hyperfine line . Although it is at, observationally convenient
frequency for radio sky mapping, probably not much more information would be
gained over existing 1415 MHz maps. The only survey spanning the tritium line,
by Kardashev and Gindilis in 1972 covering various frequencies between 1337-1863
MHz, used an all-sky dipole antenna  which would not be sensitive to point
sources of tritium hyperfine radiation.
2.3.4 Future Hyperfine
Line ObservationsIf R = radius of volume
containing the leakage atoms, Ds is the
distance to the star, a = antenna beamwidth, and
N is the number of atoms in the field of view, then
for an unresolved source (a >> Rb/Ds) the
brightness temperature TB of the
artificial cloud is given by TB = CN/A, where the projected area
A = pRb2 and C
= (3hc3/32pk)(A10/w2), for w = hyperfine frequency (Hz) and
h = Planck's constant . A10 is the computed Einstein A transition
probability, which is (fol. Field ) 2.869 x 10-15
sec-1 for hydrogen and 3.493 x 10-15 sec-1 for
tritium. No experimental value for tritium is yet available . The flux of
radio energy of hyperfine wavelength l reaching the Earth is F
= (2k/l2)TbW = (2k/l2) (CN/Ds2),
where W = p(Rb/Ds)2. For the detection limit, taking
Ds in parsecs and F in flux units, NH =
2.77 x 1045 Ds atoms H and
NT = 2.27 x 1045Ds atoms T.
A civilisation which has effluxed more than DMHt ~ NHmp =
(2.77 x 1045) FHDs2mp = 5 x 1020 kg (2 x 10-7
MJ) of hydrogen fusion fuel during its
lifetime t could be detected
at F £ 1 Jy sensitivity and
Ds < 10 pc. Tritium decays with a
half-life th (~ 12.5 yr) regardless of t, so a civilisation which leaks tritium at a rate
greater than DMT
~ (2.27 x 1045)FTDs2mp(th/ln(2))-1 = 7 x 1011
kg/sec (~ 1 Lsun wastage, for eT = 0.64% c2) could be detected at F £ 1 Jy and Ds £ 10 pc. Thus the
tritium limit is less restrictive for t > 22 yr, but has the advantage that
any detection is unambiguously artificial.
The observational frequency in each case must be corrected to the Local
Standard of Rest by compensating for Earth's rotation (± 2 KHz), Earth's orbital velocity around the Sun (± 140 KHz), and the Sun's radial velocity toward the target
star (± 100 KHz). The bandwidth in searches for
artificial clouds should span roughly the expected cloud thermal velocities,
about ± 7.7 KHz for thermal line broadening at 300 K.
A tritium line search is also sensitive to SETI beacons or signals. Assuming
a 15 KHz bandwidth 20 K detector with a one hour integration time, such a search
could detect a 6 MW, 26-metre transmitter antenna 10 pc away pointed at Earth.
Within 20 light-years of the Sun there are 86 stars, 80 of stellar class F-M,
about 70 of which are visible from the northern hemisphere. There are many
reasons for excluding 0, B and A stars from the search , such as the
probable lack of planets, the severe UV environment, and the brief residence
time on the main sequence with the concommitant reduced time for the emergence
and evolution of life. Fifty-three of the nearest stars have now been examined
for narrowband tritium line emissions, using the 26-metre radiotelescope at Hat
Creek Radio Observatory in California, to a sensitivity of 1-20 Jy . No
detections were made.
ADDITIONAL OBSERVABLES OF TECHNOLOGICAL CIVILISATIONSFive other
charactersitics of advanced technological civilisations may be visible across
interstellar distances. Internal communications and power transmission equipment
may generate radio leakage radiation upon which we may "eavesdrop." Large
circurnstellar structures may produce an anomalous blackbody radiation
signature. The use of fission rather than fusion nuclear fuels might give rise
to anomalous solar absorption lines. Large-scale movements of hot photospheric
material may produce unusual spectral line broadening and clearly artificial
ghost tines. Finally, very large-scale technical activities near a star may
require or establish enormous magnetic fields which may be observable via Zeeman
3.1 Artificial Radio
SpectrumSullivan et al.  performed an extensive survey of
all sources of artificial radio energy leakage from Earth. An Arecibo-size
antenna could detect terrestrial UHF television stations from two light-years
away, and the US BMEWS military radars from 20 light-years away. A Cyclops array
 could increase these ranges to 25 light-years and 250 light-years,
respectively. Sullivan et al note that geopolitical boundaries and other
information about human society can be deduced from Earth's leakage radiation,
but an advanced circurnstellar civilisation would present a vastly more complex
picture. However, greater efficiency as well as greater energy are available to
advanced societies so it cannot be assumed that extraterrestrial technological
civilisations are necessarily "noisier" than Earth.
3.2 Anomalous Blackbody
RadiationSolar optical luminosity is decreased according to the
fraction f of the circurnstellar sphere blocked by optically dense orbiting
material structures (i.e., a "Dyson shell"), reducing the stellar visual
magnitude by -2.5 log(1-f) magnitudes. In nearby
stars this produces an evidently distant but otherwise normal star with an
infrared  and radio excess. The radio excess is difficult to detect. At 5
GHz, Arecibo could only detect fully-occulting (f =
1) artificial shells closer than 0.1 parsec. A proposed 10 km space-based
radiotelescope array  could reach at least to 10 parsecs, and a 100 km
system could reach 100 parsecs although this lies considerably beyond existing
The infrared excess is easier to observe. A shell of orbiting artifacts
creates a bimodal blackbody spectrum with two peaks of reciprocal amplitude, one
near 500 nm (spectral class G V star) and the other near 10 microns (300 K shell
of rotating bodies at 1 AU). Although this spectral signature is not
unambiguously artificial, it is clearly unusual and invites further close
scrutiny. The best current near-IR ground-based survey  at 0.8 micron could
only have detected an optically dense artifact shell nearer than 0.01 pc, but
the Infrared Astronomical Satellite (IRAS) permits detection  of
fully-occulting (f = 1) Dyson shells out to 1000 pc
and 1% occulting shells (f = 0.01) to 100 pc. Care
must be taken to develop criteria for distinguishing artificial shells from
stars such as Vega (recently discovered in IRAS data) and Be star MWC 349 ,
both of which display an infrared excess caused by natural circurnstellar
3.3 Fission Product Absorption
LinesWhitmire and Wright  suggest that extraterrestrial
civilisations might use the local star as a repository for radioactive fissile
waste materials, and Gray et al  conducted a brief search for spectral line
enhancements of the expected waste elements for three stars, using an optical
telescope at Kitt Peak National Observatory in Arizona. However, there are
several deficiencies in this approach. For instance, considerations of
convective mixing and stellar lifetimes restrict the possible candidate stars to
the approximate spectral range A5-F2, yet these stars are not thought to be
suitable candidates either for the formation of planets or for the natural
origin and evolution of life.
The major fissionable on Earth is thorium, which is about three times as
abundant as uranium and probably represents more available energy in the
minerals of the Earth's crust than from both uranium and fossil fuels. The
abundance of thorium in the crust is about 12 ppm, about 4 ppm for titanium,
10-6 for radium, and 10-9 for polonium and several other
rare naturally-occurring isotopes. The mass of Earth's crust down to 20 km
assuming a mean density 2670 kg-m-3 is 3 x 1022 kg, of
which 16 ppm are fissionable or 4 x 1017 kg. Collected and burned as
fission fuel, this would release about 0.1% mass energy or only 4 x
1031 joules. Ultimately, all Solar_ System fissiles could conceivably
be mined and burned. Fissile abundances of Th and U in the Solar System  are
3.2 x 10-10 and 1.5 x 10-10, respectively, so total
fissiles are 9.4 x 1020 kg and the total available energy is 8 x
On the other hand, the total amount of fusionable hydrogen (the most abundant
fusion fuel) is about 2 x 1020 kg on Earth, 2 x 1021 kg
for all of the planets but not the Sun, and 2 x 1030 for the entire
Solar System. Fusion fuel can release up to 0.92% of its mass energy, so these
correspond to 2 x 1035 joules from terrestrial sources, 2 x
1042 joules from planetary sources, and 2 x 1045 joules
for the entire Solar System.
So while an expanding civilisation might resort to fissionables as a last
effort, clearly fusion fuels are more cost effective. They are easier to mine or
extract and to transport. They are generally nonradioactive or, in the case of
tritium, only weakly so, and hence may be stored more safely so far as
biological beings and computers are concerned. Combustion of all fissionables in
the Solar System, including those in the Sun, would release only as much energy
as burning the fusion fuel on Earth alone. Fusion fuels are clearly the method
of choice for artificial energy generation on an energy/kilogram basis.
Even if spaceborne fission reactors are employed, using stars as waste
repositories is inadvisable for several reasons. First, if the atomic masses of
the isotopes comprising the discarded matter lie much below or above 56 (Fe),
nuclear binding energy is still available and is lost if not recovered. Second,
the infall of matter towards a star represents a conversion of gravitational
energy to kinetic energy, which is absorbed by the star and effectively lost to
the orbital civilisation, along with the gravitational energy originally added
to the matter to raise it from a planetary surface or atmosphere in the first
place. Third, addition of foreign matter to stellar photospheres may disturb the
natural ionic mix, alter flare and sunspot activity, and cause other undesirable
side effects. Finally, there is little mixing between the photosphere and solar
interior, so material deposited in stars remains there over long periods. If the
star is later mined for its fusion energy physical resources, the discarded
matter must again be raised against a strong gravity field.
3.4 Doppler and Stellar
Spectral AnomaliesLarge-scale technical activities may involve the
removal of mass from the local star of radius Rsun to the circurnstellar shell of radius R. The movement of hot photospheric plasma from Rsun to R will produce a
weak optical (wavelength l)
Doppler component of order Dl = lDv/c. Dv = (2GMsun(Rsun-1R-1))1/2 = 617 km/sec, so at 500 nm,
Dl ~ 1 nm. This is a
potentially larger effect than optical spectrum line broadening due to thermal
velocities and photospheric turbulence (>0.01 nm), stellar rotation (>0.4
nm), or interstellar radial motion (>0.1 nm in the solar neighbourhood), and
can easily be distinguished from double-line spectroscopic binaries.
The exact appearance of the artificial anomaly depends upon unknown stellar
mass extraction trajectories. A single locus for removal and collection would
give rise to single anomalous ghost lines shifted £ 1
nm. Several loci would make multiple ghost lines. Co-rotating loci would produce
time-variable anomalies. Non-localised loci would result in large, probably
asymmetrical, line broadening. These lines could be quite bright. If the natural
energy available to the extraterrestrial civilisation ~ Lsun, then the total plasma mass in transit from
Rsun to R at
any given moment is of order Mp ~
2LsunR/Dv3 = 5 x
1020 kg, about the mass of the solar photosphere. In addition to
direct searches for ghost lines, observed line anomalies in stars classified as
P-Cygni, Wolf Rayet, T Tauri, and Ap magnetic and spectrum-variable should be
re-examined for cases of possible spectral misclassification. Finally, any A0-A9
star showing both strong neutral H and neutral metal lines could be a
misclassified late-type star surrounded by an artificial hydrogen cloud.
3.5 Anomalous Magnetic
FieldsTechnical activities in an artificial circurnstellar shell of
radius R could conceivably involve current loops of
order R giving rise to a free space magnetic
induction of order B = moi/R and magnetic flux FB = 4pBR2 over the spherical habitat shell of energy
EB = FBi = (4p/mo)R3B2,
where mo =
permeability constant. The highest natural fields found in main sequence stars
are 0.1-1 tesla, so a B = 10 tesla field would be
clearly artificial and for R = 1 AU represents EB = 3 x 1042 joules. To establish
this field would require burning ~ I Mj as fusion fuel, which seems excessive.
Artificial fields B < 103 gauss, while
observable via Zeeman line splitting (about 10-4 nm) in optical
spectra, would not be unambiguously artificial when detected near late main
4. CONCLUSIONSThe most observable
characteristic of an advanced extraterrestrial civilisation which makes
extensive use of the fusion fuel resources of its local star and planets is an
effusion cloud of molecular fuel elements. This cloud rapidly dissociates and
neutralises to the atomic ground state. Optical anomalies would be difficult to
observe, but the detection of both the hydrogen and tritium hyperfine transition
radio lines is relatively straightforward. Existing searches at these lines are
not sensitive to artificial fusion fuel clouds. In addition, the low natural
abundance of neutral atomic ground-state tritium suggests that its hyperfine
line, centred in the radio-SETI waterhole band, has minimum background noise and
thus is ideal for interstellar communication and future SETI searches. With one
exception , no SETI searches at the tritium line towards individual stars
have been reported to date. Other observables of advanced civilisations,
including redshifted neutrino point sources, an artificial radio spectrum,
anomalous blackbody radiation, fission product absorption lines, Doppler and
stellar spectral anomalies, and extraordinary magnetic fields, might also serve
as the basis for future SETI research but are considerably more challenging
thanks Francisco Valdes for contributions and comments on an earlier version of
the manuscript. This research was supported by the Xenology Research institute.
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