ABC-Net_2007-08_scope_and_facilities

ce57980a-13d5-483b-8aca-62652b4d11ed-160330211918.doc
Astrobiology Lecture Course Network (ABC-Net)
Winter Semester 2007/2008
1. Introduction
Astrobiology is a newly emerging field of science. The scope of Astrobiology comprises the
study of the overall pattern of chemical evolution of potential precursors of life, in the
interstellar medium, and on the planets and small bodies of our solar system; tracing the
history of life on Earth back to its roots; deciphering the environments of the planets in our
solar system and of their satellites, throughout their history, with regard to their habitability;
and searching for other planetary systems in our Galaxy. Hereby, Astrobiology provides clues
to the understanding of the origin, evolution and distribution of life and its interaction with the
environment, here on Earth and in the universe.
Scientists from a wide variety of disciplines are gathering in the study of Astrobiology,
including astronomy, planetary research, organic chemistry, palaeontology and the various
sub disciplines of biology including microbial ecology and molecular biology. Space
technology plays an important part by offering the opportunity for exploring our solar system,
for collecting extraterrestrial samples and for utilising the peculiar environment of space as a
tool. However, this full expertise in Astrobiology is not always available at a single
university.
To overcome this problem the European Space Agency (ESA) proposed an innovative format
of tele-teaching based lectures: experts from different European universities covering the
various fields of Astrobiology agreed to contribute and created the first successful pilot
project in the academic year 2005/06: an Astrobiology Lecture Course Network (ABC-Net).
On 23 October 2007 the ABC-Net and ESA officially kick-off the second academic year for
this inititative: again the organisation of the event shall be conducted and supported by the
ESA and its Erasmus Center. The tele-teaching shall be mainly based on three
telecommunication tools:
• Live video-conferencing. Teaching sites should be equipped with ISDN.
• iLinc e-learning tool, live and on-demand, delivering video and PPT presentations.
• On-demand video and slides via streaming video. The recorded lectures will also be
available ESA websites mentioned at the end of this document.
The diagrams at the end of this document provide support to the audio/video
technicians/engineers that will have to set up the technical installations at the University
sites.
The course will provide 17 lecture hours which corresponds to 2-5 ects (to be confirmed).
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Figure 1. Location of the ABC-Net members
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2. ABC-Net 2007/08 Lecture plan
Each lecture starts Tuesdays at 14:00 (CET) and lasts for 60 min followed by a 15 min
questions and answer period
2.1 Participating university, institution, lecturer and contact
person:
1. ESA-ESTEC, Noordwijk, the Netherlands
Lecturer: Jorge Vago, Rene Demets and Massimo Sabbatini,
Contact person: Massimo Sabbatini, e-mail massimo.sabbatini@esa.int
2. Finland: University of Turku,
Lecturer: Harry Lehto, Kirsi Lehto
Contact person: Kirsi Lehto, e-mail klehto@utu.fi
3. France: University of Paris 12 & Paris 7,
Lecturer: Francois Raulin, Herve Cottin, and Gabriel Tobie (University of Nantes)
Contact person: Hervé Cottin, email cottin@lisa.univ-paris12.fr, Francois Raulin, e-mail
raulin@lisa.univ-paris12.fr
4. Germany: Technical University of Dresden, Germany;
Lecturer: Stefanos Fasoulas, Helga Stan-Lotter (University of Vienna), Heike Rauer (TU
Berlin), and Petra Rettberg (DLR, Köln)
Contact person: Tino Schmiel, e-mail tino.schmiel@tu-dresden.de
5. Germany: MPI Solar System Research with Universities of Braunschweig and Göttingen,
Lecturer: Fred Goesmann
Contact person: Dieter Schmitt e-mail schmitt@mps.mpg.de
6. Italy: University Tuscia, Viterbo,
Lecturer: Raffaele Saladino
Contact person: Raffaele Saladino, e-mail saladino@unitus.it
7. Italy: University of Napoli,
Lecturer: A. Rotundi (
Contact person: John Robert Brucato, e-mail brucato@na.astro.it;
8. Poland: University of Szczecin,
Lecturer: Ewa Szuszkiewicz, Franco Ferrari
Contact person: Ewa Szuszkiewicz, e-mail szusz@univ.szczecin.pl
9. Portugal: New University of Lisbon,
Contact person: M.E. Webb, e-mail: ew@fct.unl.pt
10. Russia, University of St. Petersburg
Contact person: N. Gontareva, e-mail ngontar@mail.cytspb.rssi.ru
11. U.K. Open University, Milton Keynes,
Lecturer: Charles Cockell, Monica Grady
Contact person: Charles Cockell c.s.cockell@open.ac.uk and Tracey Ward: e-mail
t.a.ward@open.ac.uk
12. Technical management: Massimo Sabbatini, ESA-ESTEC, Erasmus Centre, Directorate of
Humanspaceflight, Microgravity and Exploration, e-mail: massimo.sabbatini@esa.int
13. Scientific coordinator: Gerda Horneck, DLR, Institute of Aerospace Medicine, Köln,
Germany, gerda.horneck@dlr.de
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Lecture
No. Week Date Lecturer Institution Place of lecture Title
1 44 30.10.2007 A. Brack // H. Lehto University of Turku University of Turku Introduction (15 Min) // From Big Bang to the molecules of life (45 Min)
2 45 06.11.2007 E. Szcuszkiewicz University of Szcecin University of Szcecin Planet Formation
3 46 13.11.2007 H. Cottin University of Paris 12 CNES Paris Basic prebiotic chemistry
4 47 20.11.2007 K. Lehto University of Turku University of Turku From molecular evolution to cellular life
5 48 27.11.2007 R. Saladino University of Viterbo University of Viterbo Role of catalysis on synthesis of biomolecules
6 49 04.12.2007 F. Ferrari University of Szcecin University of Szcecin Hunting protein ancestors
7 50 11.12.2007 H. Stan-Lotter Univ. Salzburg University of Dresden Extremophiles, the physico-chemical limits of life (growth and survival)
8 51 18.12.2007
J. Vago/R. Demets/M.
Sabbatini ESA/ESTEC ESA/ESTEC ESA Astrobiology missions and facilities within the HME directorate
9 3 15.01.2008 S. Fasoulas University of Dresden University of Dresden
Astrodynamics and technology aspects of astrobiology missions
in our solar system
10 4 22.01.2008 C. Cockell OU, Milton Keynes OU, Milton Keyes Habitability in our solar system and beyond
11 5 29.01.2008 M. Grady OU, Milton Keynes OU, Milton Keynes Astrobiology of terrestrial planets with emphasis on Mars
12 6 05.02.2008 G. Tobie University of Nantes CNES Paris Astrobiology of Jupiter's moon Europa
13 7 12.02.2008 F. Raulin University of Paris 12 CNES Paris Astrobiology of Saturn's moons Titan and Enceladus
14 8 19.02.2008 F. Goesmann
University
Braunschweig/Göttingen MPS Sonnenforschung Astrobiology of comets
15 9 26.02.2008 P. Rettberg DLR, Köln University of Dresden Planetary Protection Requirements
16 10 04.03.2008 H. Rauer Tu Berlin University of Dresden Exoplanets, detection and habitability
17 11 11.03.2008 A. Rotundi University of Napoli University of Napoli Methods for analysing cosmic dust
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3. ABC-Net 2007/08 Abstracts
Date Lecturer Place Title
30/10/07 A. Brack Univ Turku Short introduction into Astrobiology
H. Lehto University of
Turku
From Big Bang to the molecules of life
Abstract: Evolution of the universe predates both the chemical evolution and the evolution
of life. We will summarise the origin of the critical elements for life, the CHNOPS, and the
initial formation of molecules. From cosmological models we can understand the origin of
hydrogen and helium. Later hydrogen will be required when water is formed. Helium,
which appears quite useless for life, turns out to be a critical factor in the synthesis of
carbon leading to heavier elements. The second compound of water, oxygen, is formed in
the hot cores of stars. Once these elements get from the stars back into the cool interstellar
space they begin forming interstellar clouds, where a vast spectrum of molecules is formed.
The observed properties of these molecules, and the larger dust particles will be reviewed.
These will the play an important role in the formation of planets in the accretion disks of a
metal rich population of stars. This material reprocessed by the newly formed star and other
planets “rains” on the young planet in the form of meteorites, comets and asteroids creating
a supply of raw materials needed for the prebiotic evolution and the eventual biological
evolution of life.
06/11/07 E.
Szcuszkiewicz,
University
of Szcecin
Planet formation
Abstract: The most natural environment for the existence of life and its development is a
planet orbiting a star. We have only one, but extremely good example for that, namely the
planet Earth circling around the Sun. There are quite a few conditions which need to be
satisfied for life to be present on our planet and this will be the subject of a separate lecture.
Here, we would like to focus on the more basic question of how planetary systems form and
evolve. We adopt a methodology which proved itself to be powerful and successful in the
field of stellar evolution, which means, we make use of the fact that there are many stars
with their planetary systems in the sky in different stages of their evolution. By observing
them and building models we can reconstruct the time sequence and find out the most
plausible scenarios for planet formation. Our methodology is justified, because we know
already more than 200 mature, fully developed planetary systems and numerous examples of
protoplanetary discs, which are believed to be the sites where planets are born. During this
lecture we review the life history of our planetary system. We will admire how our present
Solar System has been born, starting from the molecular cloud collapse, after passing
through a deeply embedded protostellar phase and successively through a T Tauri phase.
Next, we will watch how planetesimals and protoplanets form in protoplanetary discs via
sedimentation and agglomeration until the final system arises after 4.6 mld years of its
evolution. The Hubble Space Telescope, the Spitzer Space Telescope, the James Clerk
Maxwell Telescope, among other missions and instruments, helped us to put together the
different stages of this scenario. Advanced numerical simulations promise an even more
detailed story, as they predict precisely the robust features in the structures of protoplanetary
discs and the architectures of planetary systems. These predictions will be verified by present
and future observatories like COROT (COnvection, ROtation and planetary Transits),
Herschel, ALMA (Atacama Large Millimetre/Submillimetre Array), James Webb Space
Telescope, Kepler and a few others. At the end of this lecture we consider briefly also what
will happen with a planetary system, like our own, during further evolution of the central
star, when the star enters a Red Giant phase and finally become a white dwarf.
13/11/07 H. Cottin University of Basic prebiotic chemistry
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Paris 12
Abstract: Before life could arise on a planet, atoms have to organise themselves into
complex biological molecules such as proteins, RNA, or DNA. Such elaborated structures
can’t appear by themselves at once, they result from a complex chemical evolution, starting
with the simplest organic compounds. At some point, at some yet to define stage of
complexity and organisation of matter, an important step is made and chemistry turns into
biology.
This lecture is devoted to the study of prebiotic chemistry; it focuses on the very first steps of
the chemical evolution: the synthesis of the building blocks of the molecular engine of any
known living organism on Earth. In a previous lecture of this series, how atoms form in stars
was explained. Now we consider how atoms can spontaneously combine to make molecules,
before discussing the molecular evolution to cellular life in the next lecture.
In the first part of this lecture living systems are dismantled into more elemental fragments:
organic molecules. To address the origin of life, the next question would be how those
fragments can be synthesized in an abiotic manner. After a short historical review about the
chemistry of life different tracks are explored: an endogenous production of the molecules of
life, within the Earth atmosphere or in the depths of primitive oceans, or an exogenous
source of prebiotic molecules through space delivery via meteorites and comets. The
chemical pathways of synthesis of the building blocks of life will then be described.
20/11/07 K. Lehto University of
Turku
From molecular evolution to cellular life
Abstract: First, the essential features of cellular life will be considered; what is required for
life, and what are the criteria of life. Nucleic acids, genetic code and its expression system
are conserved and ubiquitous properties of all life forms, and therefore are assumed to be the
most original functional units of life. Molecular analysis of these structures gives suggestions
of how they may have been involved in the early molecular evolution, and what functions
they may have provided to the early (precellular) replicators. By going backwards, step by
step, one sees which inventions had to precede each stage of early evolution: genetically
encoded proteins had to exist prior to the establishment of the Last Universal Common
Ancestor (LUCA), and RNA-mediated RNA-replication, or so called RNA world, had to
predate genetically encoded proteins. Some cellular RNA-molecules, which have different
enzymatic activities and are highly conserved between different organisms are supposed to
be relicts from this era. Still, many questions related to the early molecular evolution remain
open. We do not know, for instance, the prebiotic synthesis routes for the nucleotides, how
life chose to use the distinct nucleotides and amino acids in their distinct chiralic forms, how
the first functional polynucleotides were assembled, or how the earliest life forms were
confined.
27/11/07 R. Saladino University of
Viterbo
Role of catalysis on synthesis of biomolecules
Abstract: Prebiotic chemistry plays a central role in the investigation of the possible
scenarios of the early chemical environments. Its goal is to shed light on the events involved
in the synthesis of initial biomolecules and on the self-organization processes that led the last
common ancestor. Even though a well defined scenario for the physico-chemical conditions
on the primitive Earth is not available, one can assume that a synthetic pathway, in order to
be considered prebiotic, should use the simplest chemicals and the most common conditions
present at that time. Low molecular weight molecules such as carbon dioxide, hydrogen
cyanide, formamide and formaldehyde, easily formed from the primitive atmosphere by
ultraviolet light, heat or electric discharge as energy sources, have been considered as
prebiotic precursors. The catalysis played a crucial role in the prebiotic synthesis of
biomolecules starting from these chemical precursors. Several minerals and metal oxides
characterized by chemical, redox and photochemical catalytic properties were widely
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diffused on the primitive Earth. These compounds, when components of a reaction mixture,
could have enhanced the efficacy of prebiotic syntheses, affecting the selectivities of the
reactions and furnishing local microenvironments able either to concentrate dilute reagents
or to preserve newly formed biomolecules from degradative processes. In this lecture we will
focus on the main concepts of catalysis applied to prebiotic chemistry, including
homogeneous and heterogeneous catalysis, multifunctional catalysis and autocatalysis.
Different examples on the role of catalysis in the synthesis of biomolecules starting from
simple precursors will be discussed with a special attention to the synthesis of sugars,
peptides and oligonucleotides. Examples of prebiotic synthesis of biomolecules with non
terrestrial minerals as well as multi-components catalysis will be also described.
04/12/07 F. Ferrari University of
Szcecin
Hunting protein ancestors
Abstract: In searching the origin of life it is possible to apply two different approaches. The
first one is a down-to-top approach, in which, starting from inanimated matter, like for
instance basic organic compounds or aminoacids, one tries to reproduce the processes and
the conditions that gave birth to the first living beings about 3.85 Ga ago. Alternatively, one
may attempt to extract hints about the first steps of the evolution of life from the observation
of present organisms. This top-down approach is based on the fact that all living forms have
a common ancestor, so that it is licit to assume that some of its vestiges are still preserved
inside the genetic code of current cells and bacteria. Indeed, it is well known that there are
structures inside proteins, like structural motifs and folds, which seem to be intimately
connected with evolution. For example, while there are about 100,000 expressed proteins in
eukariotic systems, there are much fewer motifs and folds, a fact that is related to the
pathways of evolution. In this lecture some aspects of the top-down approach will be
illustrated. After a brief review of the known structures in proteins and other macromolecules
which are relevant for life, a discussion will follow about the physical and chemical
properties of biopolymers. Physical and chemical laws were in fact present during the period
in which life started on the Earth and have certainly put constraints on the formation of the
earliest biopolymers. Therefore, they can be exploited in order to guess how the genome of
the most primitive organisms looked like. The information about the general characteristics
of ancient life forms obtained using physical and chemical arguments may be used in the
search of the remnants of the first genes which could be inside modern genes for instance
due to processes of gene fusion. The lecture will end up with a discussion about the physical
experimental methods that allow the detection of possible substructures inside biopolymers
like proteins or DNA.
11/12/07 H. Stan-
Lotter
University of
Dresden
Extremophiles, the physico-chemical limits of life
(growth and survival)
Abstract: Extreme environments are characterized by physical and chemical parameters
which were considered lying outside the range which is suitable for life. In recent years, the
notion of what constitutes life-limiting conditions in an environment has undergone dramatic
changes: microorganisms and occasionally higher organisms were discovered, which not
only tolerate, but thrive under ranges of temperatures, pH values, pressures, salinity, ionizing
radiation etc. previously thought to destruct biomolecules and organisms. Some of the
mechanisms responsible for these life styles are in the process of being elucidated. The
presence of liquid water is a prerequisite for growth under all kinds of conditions; however,
survival of resting stages, such as spores or dormant forms, was shown to occur in vacuum
and in space conditions for several months. The detection of numerous viable prokaryotes
and spores in subterranean locations, such as basalt, granite, ancient halite and sediments,
suggests the possibility of extensive longevity, perhaps over millions of years.
The implications of these discoveries for the search for extraterrestrial life are severalfold:
the probability of finding prokaryotic life in environments such as the subsurface of Mars or
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the salty ocean of the Jovian moon Europa appears greatly enhanced, and the potential for
panspermia is considered more plausible than ever before.
18/12/07 J. Vago &
M. Sabbatini
ESA/ESTEC ESA Astrobiology missions and facilities within
the HME directorate
Abstract missing
15/01/08 S. Fasoulas University of
Dresden
Astrodynamics and technology aspects of
astrobiology missions in our solar system
Abstract: Content:
1. Launch
• scenarios, Δv, launch windows,
• Constraints for biological payloads
2. Interplanetary trajectories
• Transfer trajectories,
• space environment,
• constraints for biological payloads
3. (Re)Entry, Descent, Landing
• Entry in different atmospheres (CO2, CH4, …),
• problems to biological payloads
4. Mission subsystems
• Energy system,
• Thermal system,
• Communication, Data Handling & Transfer,
• Interaction to biological payloads
5. Return-to-Earth Missions
• possibilities,
• technical constraints to probes, …
Paragraph 1 to 5 shall be summarised for astrobiology missions to planets (Mars), asteroids,
comets and/or moons (Europa)
22/01/08 C. Cockell OU, Milton
Keynes
Habitability in our solar system and beyond
Abstract: What do we mean by ’habitability’ ? Habitability depends on the organisms that
are considered and it is defined by the chemical and physical tolerances for a given
organism. As we currently have no direct evidence for life on another planet, habitability is
necessarily constrained by our knowledge of life on Earth. We use our knowledge of the
extremes of life on Earth to assess extraterrestrial environments and the plausibility that they
can support life. I will discuss the use and limitations of the concept of ’habitability’ and
provide examples of how we assess the habitability of other worlds using organisms from
extreme environments on Earth. I will discuss how considerations of energy availability
(redox couples), the presence of water and carbon sources have shaped our view of the
habitability of other planets and will eventually be used to assess the habitability of
extrasolar planets. The formulation of a definition of ’habitability’ can greater assist us in
defining the possibilities for life elsewhere.
29/01/08 M. Grady OU, Milton
Keynes
Astrobiology of terrestrial planets with emphasis
on Mars
Abstract missing
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05/02/08 G. Tobie University of
Paris 12
Astrobiology of Jupiter’s moon Europa
Abstract: The data returned by the Galileo spacecraft strongly suggest that a liquid
water layer, several tens of kilometers thick, exist beneath the cold icy surface of Jupiter's
moon Europa. This internal ocean would be in contact with the inner silicate core, possibly
volcanically active. Interestingly, the (P,T) conditions at the silicate-ocean boundary are
quite similar to those existing on the Earth's sea floor where organisms live without solar
energy. The study of Europa is therefore essential to answer such as: does life exist
everywhere water is present? Can life arise and develop in an environment where there is no
sunlight ? What source of energy may be used by the microorganisms?
The existence of an internal ocean is surprising since the satellite was expected to be frozen
due to its very cold surface temperature (~100 K). For several years, tidal dissipation has
been invoked to explain the possible presence of an ocean within Europa. Tidal dissipation
comes from the viscoelastic response of the satellite to the 3.55-days tidal forcing. In the
Laplace resonance, Io and Ganymede force the eccentricity of Europa. As it travels around
Jupiter on an eccentric orbit, Europa is subjected to a periodical deformation. Due to the
viscoelastic properties of its materials, viscous dissipation by shear friction occurs within
each internal layer. Tidal dissipation in the inner core may heat up the outer silicate layer
resulting in volcanism similar to the one observed on Io. Thermal evolution models indicate
that the silicate core could have reached an highly dissipative state only if Europa
experienced larger tidal forcing in the past. Future exploration of Europa is required to
determine the exact depth of the liquid layer and to assess the possibility of seafloor silicate
volcanism.
The lecture reviews our present knownledge on Europa: its geology and its internal structure.
Models of tidal dissipation and thermal evolution and their implications for the development
of biogenic activity are presented. Concepts for future exploration missions toward Europa
are summarized, with particular emphasis on the search for liquid water and on the
exobiological potential of that "ocean" satellite.
12/02/08 F. Raulin University of
Paris 12
Astrobiology of Saturn’s moons Titan and
Enceladus
Abstract: Titan, largest satellite of Saturn, with a diameter of 5150 km, is the only satellite in
the Solar System having a dense atmosphere. Since the discovery of the properties of this
atmosphere, especially its main molecular composition – dinitrogen (N2) with a few percents
of methane (CH4) – by the Voyager spacecraft observation in the early 80ties, Titan is
considered as one of the most interesting bodies of the Solar System with regard to
astrobiology. Indeed such an atmosphere is very favorable to the production of organic
compounds as demonstrated by the Miller’s now historical experiment and the many similar
experiments which were done later on. The likely presence of a complex organic chemistry
in Titan’s atmosphere was also directly supported by the detection of many organic
compounds detected by Voyager, and by several observations of Titan’s atmosphere from
ground-based and Earth orbit telescopes. These discoveries were one of the main motivations
of the scientific community for going back to the Saturn system with a very ambitious
planetary mission: Cassini-Huygens. Most of our current knowledge of Titan is based on the
new and very fresh observations done by Cassini-Huygens, coupled to laboratory
experiments, including simulation experiments, and theoretical modeling (in particular
photochemical models and ionospheric chemical models of the atmosphere, and models of
the internal structure of the satellite). The lecture presents some historical data on Titan
before Cassini-Huygens, before describing the Cassini-Huygens mission and its scientific
payload. Then the models of formation and of internal structure of Titan are summarized and
the general astrobiology of Titan is presented. Each of the three main astrobiological aspects
- similarities with the Earth, organic chemistry and habitability – are described. Among the
several fully unexpected discoveries done by the Cassini-Huygens mission are the
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observations of important geological activities on Enceladus, a smaller satellite of Saturn,
with a radius of only 250 km. These observations and their potential astrobiological input are
briefly described. New concepts for future exploration missions of Titan and Enceladus are
presented as a conclusion.
19/02/08 F.
Goesmann
MPS Lindau Astrobiology of comets
Abstract missing
26/02/08 P.
Rettberg
University of
Dresden
Planetary Protection requirements
Abstract: ESA’s space exploration programme Aurora aims at the robotic and human
exploration of the solar system with Mars, the Moon, Europa and the asteroids as the most
likely targets. Mars is selected as the destination of the first Aurora Flagship mission
ExoMars, followed by a Mars Sample Return mission. The scientific objectives of the
ExoMars mission are the search for past and present life on Mars, the identification and
characterization of possible hazards to future human exploration and the enhancement of our
knowledge about the Martian environment in general. The reach these ambitious goals the
importance of planetary protection measures becomes obvious. Planetary protection is the
term that describes the aim of protecting solar system bodies (i.e. planets, moons, comets,
and asteroids) from contamination by terrestrial life, and retroactive protecting Earth from
possible life forms that may be returned from other solar system bodies. Planetary protection
is necessary (i) to maintain the possibility to study these other solar system bodies in their
pristine states, (ii) to avoid terrestrial contamination that would obscure the possibility to find
indigenous life elsewhere and (iii) to ensure that the Earth's biosphere is protected from
potential extraterrestrial sources of biological contamination. COSPAR, the Committee of
Space Research, has formulated a planetary protection policy and defined planetary
protection guidelines based on article IX of the UN Outer Space Treaty from 1967. The
planetary protection procedures that have to be applied to a given spacecraft are determined
by the type of mission (e.g. flyby, orbiter, lander, rover) and the biological interest posed by
the spacecraft’s destination. Landers and rovers destined towards objects of high biological
interest must undergo careful cleaning and sterilization. A Mars lander mission is classified
as planetary protection category IVb/c with extremely low bioburden limits among other
stringent requirements, if the landing is planned in a so called ‘special region’ with the
potential for the existence of extant Martian life. All other landers on Mars are classified as
category IVa with less stringent, but still technically challenging requirements concerning
bioburden limits. In this lecture the planetary protection requirements, the bioburden limits
and the principle methods and procedures to fulfill these requirements will be discussed in
detail.
04/03/08 H. Rauer University of
Dresden
Exoplanets, detection and habitability
Abstract: Since the mid-90’s the number of detected extrasolar planets around dwarf stars is
rapidly increasing. Today, we know that our solar system is only one among many planetary
systems of very different nature. Many of their characteristics know up to now came
unexpected, questioned the traditional theories of planet formation. Nevertheless, our view of
planetary systems is still very restricted. Mainly large giant planets have been found so far
due to detection limits of the methods used. In the near future the already working space
mission CoRoT (CNES) and the upcoming mission Kepler (NASA) are expected to find the
first Earth-sized, terrestrial planets. Many of these terrestrial planets detected will probably
be on short-period orbits or larger than Earth, forming to new classes of potentially habitable
planets, so-called “hot-Earth” and “super-Earth”. However, under which conditions
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terrestrial extrasolar planets are providing habitable conditions still remains to be
investigated. Habitability depends e.g. on the atmospheric composition and climate.
Atmospheric models are used to predict the climatic conditions on different types of
terrestrial planets and to predict the spectroscopic signatures of a potential biosphere. Such
biospheric signals can be investigated by planned space missions like Darwin (ESA). The
lecture will present the methods to detect extrasolar planets, the main characteristics of the
planets found so far and the expectations we have concerning habitable planets and the
potential to detect biosignals in their atmosphere.
11/03/08 A.
Rotundi
University of
Napoli
Methods of analysing cosmic dust
Abstract: Analysing extraterrestrial dust samples, i.e. Interplanetary Dust Particles (IDPs)
and cometary dust collected in situ (Stardust samples), is critical to understand the role
played by dust grains in driving the formation of complex molecular compounds relevant for
the prebiotic chemistry occurred in the early Earth. In particular, one of the driving forces for
cometary dust study is looking for confirmation of the historical theory, hypothesized by
Halley, published by Newton in his Principia in 1686, and developed more or less
continuously ever since that comets may have played an important role for the development
of life on Earth. The extent to which comets enriched the primordial Earth with reactive C-
bearing molecules and water is not known. The estimate of the endogenous contribution to
Earth’s organic inventory during this period is in the order of 108
-1010
kg year-1
, while the
flux of organic matter delivered to the Earth via comets and asteroids, averaged over the
heavy bombardment period, may have been even larger at around 1011
kg year-1
.
Organic molecules have been detected in comets by comet fly-bys and by astronomical
observations. The presence of C-bearing molecules in comets is to be expected based on
numerous astronomical observations in which complex organic molecules have been
detected, in dense molecular clouds and the diffuse interstellar medium. Dense clouds are
known to contain mixed molecular ices. The radiation processing of these ices could
produce a host of organic species, including some of astrobiological interest. Molecular
clouds are the parent reservoirs of protoplanetary disks, like the solar nebula, where grains
were further irradiated and the effects of which may be at least as important as those
occurring in the diffuse Interstellar Medium (ISM). Organic molecules in comets could
show a higher complexity than the diffuse ISM due to the reaction with fine grains of
variable compositions such as ices and silicates as well as carbon grains and various
molecules. Silicates act as catalysts for the reaction of organic molecules to higher
complexity. The catalytic effects of cosmic dust analogues in prebiotic reactions have been
studied in the laboratory at high temperatures and in conditions simulating the environments
assumed for the early Earth. A large suite of complex organic molecules have been
synthesized in the gas phase on the surface of cosmic silicate dust analogues.
We will illustrate the methods of analysis and recent results obtained on cometary grains.
The laboratory techniques that identify the C-rich entities present in the dust grains, provide
information on their organic component, morphology, mineralogy and chemical
composition. In particular, micro-Raman and micro-infrared spectroscopy, Field Emission
Scanning Electron Microscopy and Energy Dispersive X-ray analyses have been applied on
grains extracted from the Stardust aerogel cometary collector. The results of these analyses
in terms of the nature of the organic matter present and a comparison of these findings with
what is known about organic molecules in the ISM will be discussed.
Following All All Examination
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4. ABC-Net 2007/08 mailing list:
André BRACK brack@cnrs-orleans.fr
c.s.cockell@open.ac.uk c.s.cockell@open.ac.uk
fasoulas@tfd.mw.tu-dresden.de fasoulas@tfd.mw.tu-dresden.de
François Raulin raulin@lisa.univ-paris12.fr
gerda.horneck gerda.horneck@dlr.de
goesmann goesmann@mps.mpg.de
Grady Monica M.M.Grady@open.ac.uk
helga.stan-lotter helga.stan-lotter@sbg.ac.at
Hervé COTTIN cottin@lisa.univ-paris12.fr
Harry lehto hlehto@utu.fi
John Robert Brucato brucato@na.astro.it
Jorge.Vago Jorge.Vago@esa.int
Kirsi Lehto klehto@utu.fi
Michel Viso michel.viso@cnes.fr
Natalia Gontarova ngontar@mail.cytspb.rssi.ru
Petra Rettberg petra.rettberg@dlr.de
Rauer Heike heike.rauer@dlr.de
rotundi rotundi@uniparthenope.it
Sabbatini Massimo massimo.sabbatini@esa.int
Saladino saladino@unitus.it
Schmiel Tino tino.schmiel@mailbox.tu-dresden.de
Schmitt Dieter schmitt@linmpi.mpg.de
Szusz szusz@univ.szczecin.pl
Tobie Gabriel Gabriel.Tobie@univ-nantes.fr
Ward T.A T.A.Ward@open.ac.uk
Webb Maria ew@fct.unl.pt
ESA-ESTEC video conferencing and iLinc points of contact:
Melanie Cowan Melanie.Cowan@esa.int
Jimmy Geogiades jimmyg@parsecinfo.nl
Master Control Room 0031 71 565 6322
iLinc isslinc.spaceflight.esa.int/virtual
streaming video on demand streamiss.spaceflight.esa.int
12

5. Connectivity Diagrams
Figure 2: Connectivity Diagram
13

Figure 3: ilinc connectivity
14

Figure 4: VC and iLinc connectivity
15

ABC-Net_2007-08_scope_and_facilities

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