2023 – 2024

La ACADEMIA EAI es un programa educativo internacional organizado y difundido por el Centro de Astrobiología (CAB), CSIC-INTA, Madrid, con el apoyo del Instituto Europeo de Astrobiología (EAI). Proporciona un marco para reunirse en línea con la comunidad internacional de astrobiología y adquirir conocimientos interdisciplinarios a través de una serie de seminarios impartidos por expertos en estos campos. La audiencia de la Academia se conecta desde más de 32 países y todos los continentes, con una participación media de 120 asistentes por seminario. Las ediciones anteriores son accesibles a través del canal youtube del CAB (2021-2022, 2022-2023).

El programa de la Academia EAI para el curso 2023-2024 comenzará este 4 de octubre. Los seminarios se ofrecen de forma gratuita y se retransmiten online vía zoom cada dos semanas los Miércoles de 15:00 a 16:00 CET (hora de Madrid). Las charlas serán impartidas por expertos de renombre mundial, que responderán a las preguntas planteadas por el público tras su intervención. Todos los seminarios serán grabados para su futura disponibilidad en el canal youtube del CAB.

Al final del curso académico, el CAB otorga un certificado de participación a quienes asistan a un mínimo de 10 seminarios. Para que podamos hacer un seguimiento de la asistencia, deberá introducir su nombre y afiliación en el chat del seminario cuando entre en la sala (Zoom).

El registro está cerrado.

LIST OF SPEAKERS AND TOPICS

Dr. Helmut Lammer
Space Research Institute (IWF), Austrian Academy of Sciences, Graz
Austria

Evolution of planetary environments
January 10th, 2024

Early Phase of habitable planets

The talk focuses on the evolution of stellar and geophysical conditions that allow complex multi-cellular life forms to originate on terrestrial planets with atmospheres that are dominated by N2/O2. It is shown that the earliest accretion processes set the initial parameter stages for terrestrial planets to end up as Earth-like Habitats. The most relevant factors and time scales such as the accretion time of terrestrial planets and the lifetime of the protoplanetary disk will be discussed. Competition between these time scales will determine if an accreting terrestrial planet may end up inside the habitable zone as a sub-Neptune with a primordial atmosphere or not. Other relevant factors like the availability of the initial amount of heat-producing radioactive elements such as 40K, 238U, and 232Th on early planets and their role in shaping habitable environments, including a planet thermal evolution and hence the right tectonic regime that is necessary for life as we know it will also be addressed. Since these elements can be lost during planet formation, one can expect that many terrestrial planets inside the habitable zone will have internal heat budgets and tectonic regimes that are different than those of Earth. Finally, a newly derived formula that can be used for the estimation of the number of potential Earth-like Habitats in the Milky Way that can be constrained by the detection of main atmospheric species, obtained from future space and large ground-based telescopes, will also be discussed.
Link to the video

Dr. Manuel Scherf
Space Research Institute (IWF), Austrian Academy of Sciences, Graz
Austria

Evolution of planetary environments
January 24th, 2024

Dr. Frances Westall
Centre de biophysique moléculaire (CBM), CNRS, Orleans
France

Traces of early life on Earth
March 6th, 2024

Why early life is so important to the search for extraterrestrial life

There are many missions (and future missions) searching for extraterrestrial life in the Solar System and on exoplanets. The stakes are high with enormous consequences ensuing bona fide detections – for the researchers involved, for the decision makers who fund research and/or space missions, as well as for the general public. While exoplanet research is particularly geared to traces of evolved life, ranging from organisms having developed some form of photosynthesis to SETI and technosignatures, Solar System studies are more “modest” and realistic in the sense that we know we are looking for life resembling (but not identical to) terrestrial anaerobic microorganisms. Evolved life on Earth (from oxygenic phototrophs onward) co-evolved with a geological and environmentally changing world that has no counterparts in the Solar System (unless some form of geological evolution took place on Venus). The early Earth, on the other hand, was relatively simple geologically speaking: mostly ocean planet, paucity of emergent landmasses, mostly CO2 atmosphere, environment dominated by volcanism and hydrothermal activity etc. When life emerged on Earth more than 4 billion years ago (Ga), and for about a billion years, it was totally controlled by geological processes. The appearance of anoxygenic photosynthesis and the gradual instauration of global plate tectonics leading to the formation of continental landmasses paved the way for the greater influence of life on the environment and geological processes. However, apart from possibly Venus, plate tectonics did not occur on other bodies in the Solar System and technologies are not yet at a stage to detect it on exoplanets. What was life like on the very early Earth before the emergence of photosynthesis? I will show our research of nearly 30 years into some of the oldest traces of life, concentrating specifically on chemotrophs, organisms that obtain their energy from oxidation of inorganic substances (chemoautolithotrophs) or from oxidation of pre-existing organic matter (chemoorganotrophs), as examples of the kinds of primitive life forms that might inhabit or have inhabited planets or icy satellites in the Solar System. Chemolithoautotrophs are believed to have been the first forms of life on Earth and microorganisms using similar kinds of metabolisms are likely to be the most common in the Universe – they do not leave detectable atmospheric traces. In particular, I will underline the challenges of studying their fossilised remains to prove both biogenicity and syngenicity, even here on Earth where we have access to unlimited and highly sophisticated equipment. As a fore taste, our recent PhD student Laura Clodoré has just published a paper detailing the painstaking steps necessary for such studies: Clodoré, L. et al., 2024. Multi-Technique Characterization of 3.45 Ga Microfossils on Earth: A Key Approach to Detect Possible Traces of Life in Returned Samples from Mars. Astrobiology 24. Published Online: 20 Feb 2024, https://doi.org/10.1089/ast.2023.0089.
Link to the Video

Dr. Marta Ruiz Bermejo
Centro de Astrobiología (CAB), INTA-CSIC, Madrid
Spain

Prebiotic chemistry and the carbon cycle
April 17th, 2024

HCN chemistry: Feedback between Prebiotic Chemistry and Materials Science

In this talk, a general overview of the hydrogen cyanide (HCN) chemistry will be showed, from the first HCN oligomerization observed by Proust in 1806 to the new proposed insights in prebiotic chemistry and the most recent advances in materials science, and the feedback between both fields. The hydrogen cyanide (HCN) is a ubiquitous molecule in the Universe. It has been detected in a wide range of environments with astrobiological interest, such as interstellar clouds, star-forming regions, planetary nebulae, interplanetary dust, comets, meteorites and atmospheres of satellites and planets such as Titan and Pluto and very recently in the plumes of Enceladus. In a terrestrial context, HCN can be identified in volcanic eruptions and hydrothermal vents and may have been relatively abundant in the atmosphere of the early Earth. Currently, HCN is considered a key compound in novel proposals regarding scenarios and hypotheses related to the first stages of increasing molecular complexity that led to the rise of life. It has been suggested that the HCN has significant implications for the prebiotic generation of several important bioorganics and related and intermediate compounds, such as amino acids, canonical and non-canonical nucleobases, and other N-heterocycles, as well as carboxylic acids and sugar derivatives. On the other hand, the HCN can spontaneously polymerize in the presence of bases, such as NH3 or Et3N, and free radicals from ionizing radiation, and they occur over a wide range of conditions. This singular polymeric system can also be produced from its soluble salts (NaCN or KCN), its trimer and tetramer, namely, aminomalononitrile and diaminomaleonitrile, respectively, or from its hydrolysis products, such as formamide. Furthermore, it has been suggested that HCN polymers may be the major components of the dark matter present on the surface of meteorites and comets. In addition, beyond the interest in HCN polymers in the fields of astrochemistry, prebiotic chemistry and astrobiology, these fascinating substances are inspiring new materials and present interesting properties that can lead to promising applications.

Dr. Juan Pérez-Mercader
Senior Research Fellow, Harvard University. Cambridge, Massachusetts. USA & Profesor de Investigación in Spain's National Research Council (CSIC)
Spain

The evolutionary tree of life
April 24th, 2024

Why and How to Make Non-biochemistry Based Life in a Test Tube

Living systems on Earth are open complex chemical systems. Using biochemistry, they all (i) process information, (ii) metabolize, (iii) self-reproduce and (iv) evolve. Starting with an aqueous homogeneous blend of biochemistry-free chemicals, and using biochemistry-free Polymerization Induced Self-Assembly (PISA), we demonstrate the autonomous, chemistry-controlled 1-pot synthesis and boot-up of micron-scale vesicles (“protocells”) exhibiting all the above properties. Driven by carbon chemistry and the dynamics of a growing vesicle, the time evolution of these protocells parallels the lifecycle of natural extant biology. They autonomously boot-up, display periodic growth and collapse during several consecutive cycles, self-reproduce (driven by molecular degradation in their lumen), provide heritable variation and show chemotaxis. They also show a “struggle for life” and “competitive exclusion”, thus offering a steppingstone towards Darwinian evolution. These results are a first laboratory realization of synthetic, minimal, autonomous, non-biochemical life, or “Bernal’s generalized life”. They offer insights into the laboratory creation of artificial life, of new functional materials and of multiple pathways for the prebiotic formation and evolution of precursor protocells en route to the first biochemical living systems on Earth. In the realms of Astrobiology and Exoplanets these results greatly expand our horizons for the potential presence of life in the Universe.

Dr. Laura Sanchez
Centro de Astrobiología (CAB), INTA-CSIC, Madrid
Spain

Traces of early life on Earth
May 8th, 2024

Lipid biomarkers, those fatty guys key for the search of (early and extraterrestrial) life

Dr. Laura Silva
Osservatorio Astronomico di Trieste, National Institute of Astrophysics (INAF), Trieste
Italy

Evolution of planetary environments
May 15th, 2024

Climate and habitability of rocky planets

Dr. Ludmila Carone
Space Research Institute (IWF), Austrian Academy of Sciences, Graz
Austria

Evolution of planetary environments
May 29th, 2024

The importance of magma oceans to constrain habitability

Dr. Barbara Cavalazzi
Department of Biological, Geological, and Environmental Sciences, University of Bologna, Bologna
Italy

Traces of early life on Earth
June 12th, 2024

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