We adressed here the question of abiotic photochemical production of
and
and
the astrobiological relevance of the detection of these molecules on extrasolar planets by future
space observatories (Darwin and TPF). The
two possible sources leading to an
accumulation are the photolysis of
,
and
of
O when associated with hydrogen escape. We
first showed qualitatively that these two mechanisms interfere with each other, and are thus
limited in habitable planet atmospheres, where both
and
O are expected. To tackle quantitatively
the problem, we developed new photochemical and thermal models of planetary atmospheres.
The simulation were conducted on 7 main types of terrestrial planet atmospheres (presented in
Table 3), which include present Mars and plausible early Earth and Mars atmospheres.
According to our simulations, the
photolysis proved to be an efficient
way to build up a significant oxygen level in two general cases. The first one is a dry atmosphere,
where the recombination of
is not catalysed by the products of
O photolysis. The second is a
humid atmosphere made of more than one bar of
:
in this case the temperature profile does not allow
O to reach
altitudes where it could be photolysed. In such cases,
-rich atmospheres
with an
layer as dense as on Earth can be built without the intervention of life.
However, we demonstrated that the search for life remains possible, at least within the wavelength range
of the Darwin instrument (5-20 m), by selecting only the spectra displaying the simultaneous signature of
,
O and
,
that we called the "triple signature''.
Indeed, the need for water to make the planet habitable and the
masking effect at Darwin resolution filter out any
-rich atmosphere
built from
photolysis.
Moreover, future instruments of higher spectral resolution, able to resolve
the
signature among the
bands, will also allow to discount
ambiguous cases, as the presence of these high pressure
bands
warns the observer about the possible abiotic origin of
.
We also investigated an eventual false positive detection due to
the enrichment in
that follows the photolysis of water vapor associated to hydrogen escape.
In this case, the production of
is maintained by a constant delivery of water
in the upper atmosphere via
hydrated particles. It is possible to "tune''
the model in such a way that a significant build-up of
occurs.
However, besides the fact that the required conditions
are unrealistic or result in a non-observable case (due to large
zodiacal emission),
is destroyed by the products of
O photodissociations
while
is produced. This prevents the formation of a detectable ozone layer.
We have thus demonstrated the robustness of the biogenic
detection scheme
based on the triple CO2-H2O-O3 IR signature that we propose for Darwin,
as the risk of false positive proves to be low.
We showed in contrast that
relatively high
content can be reached abiotically (up to 50 mbar
in our sample), which could be a major concern for experiments
aiming at detecting photosynthetic life using information on
alone.
Note that searching the triple signature instead of
alone is not restrictive
as
O and
are expected in habitable planets and display
strong IR bands.
Although it may be more important to avoid
"imposters'' than to miss an ambiguous signal from
some inhabited planet, "false negative cases'' and the conditions under which
oxygenic photosynthesis can effectively transform the atmosphere
have also to be discussed (Selsis 2002). For the
Earth itself, the triple signature would have allowed a remote
detection of life for only about half of its history: the almost
equally long period where biogenic
was probably the main
greenhouse gas should be studied in great detail when trying to search
for life beyond photosynthetic species.
All these questions are very important for the optimal design of any
ground or space experiment like Darwin and TPF aiming at the
observation
and search for
biosignatures in the atmospheres of terrestrial exoplanets; in all
cases photochemical models will be of great help, as we have seen here.
Acknowledgements
This work was funded by Programme National de Planétologie and GDR Exobiologie (INSU/CNRS). We thank Dr. A. Léger and Dr. M. Gargaud for critically reading the draft of this paper and Dr. W. Traub for his numerous and constructive comments that led to this final version.
Copyright ESO 2002