Following the success of the COPCA 2022 Conference, we are proud to announce a second iteration: the COPCA 2024 Conference will take place between 15-18 October 2024 in Valletta, Malta!
The Collisions Physics and Chemistry and their Applications (COPCA) conference in 2024 will bring together scientific researchers from several interdisciplinary fields to share their research and results. This year, a particular focus will be placed on processes relevant to radiation chemistry and physics, astrophysics and astrochemistry, and materials science.
This year, the conference will take place alongside a thematically-related workshop of the COST Action CA20129 “Multiscale Irradiation and Chemistry-Driven Processes and Related Technologies” (MultIChem). Sessions related to this workshop will be held on 15 and 16 October 2024. For more information on this COST Action, please click here.
The venue for the conference is the Aula Magna, situated at the Valletta Campus of the University of Malta.
The early bird conference fee (applicable up to 31 May 2024) is €425. From 01 June 2024 onwards, the regular conference fee of €575 will apply. Options are also available for accompanying persons.
Early career researchers (ECRs), including undergraduate and postgraduate students as well as post-doctoral researchers, are particularly encouraged to attend and to contribute to the success of COPCA 2024. In order to encourage the participation of ECRs, a session will be held to allow several ECRs to showcase their work in 10-minute presentations. These presentations will be judged by an independent panel and prizes will be awarded to the best presentations!
By Peter McArdle, Hans Huybrighs, Prasanna Deshapriya, Ottaviano Ruesch, and the EPEC future research working group.
The field of sample return is developing rapidly around an increasing number of missions. What facilities and techniques are needed to handle such samples? Will sample return dominate other fields of planetary science? We discussed these questions and more with Dr. Enrica Bonato, who developed the Sample Return Lab at DLR and worked with samples from Hayabusa2 and legacy samples from Luna 24.
Sample of lunar regolith retrieved by the Soviet mission Luna24 in 1976 and donated to the Institute for Cosmos Research, which was part of the Academy of Sciences of the German Democratic Republic (GDR) during the GDR which after 1990 it became the DLR Institute for Planetary Research in Berlin-Adlershof. Credit: DLR.
Can you tell us about your academic background?
I earned my PhD in planetary science, undertaking my research jointly at the Natural History Museum (NHM) in London and the University of Glasgow. My project focused on the thermal metamorphism of carbonaceous chondrites. Following this, I took on a short postdoctoral position at the NHM, where I worked on lithium mining. I am passionate about public engagement, and I explored various outlets for this during my time at the NHM.
After completing my postdoc, I transitioned into the role of lab developer and manager for the newly established DLR sample return lab. When I started this role, there was no lab to speak of! I played a crucial role in planning and outfitting the lab in addition to getting it ready for its intended use as a sample return facility and curation center. As part of my responsibilities at DLR, I am proud to be a member of the Hayabusa 2 and MMX analysis teams.
What advice would you give to early career researchers who would be interested in a similar role to yours?
The key to securing my role as a lab developer manager was ‘delving behind the scenes’ of various instruments during my postdoc. This allowed me to become an independent user of these instruments, by becoming involved in everything from sample preparation, instrument set up and operation to data analysis. Attending numerous training events organised by instrument and software suppliers also proved invaluable experience.
For those intrigued by the prospect of joining sample return missions, I believe being in the right place at the right time is crucial. However, I suggest that early-career researchers (ECRs) with an interest in these missions reach out to existing team members. By doing so, they can explore opportunities to support the mission in various ways.
“I suggest that early-career researchers with an interest in these missions reach out to existing team members.”
Enrica Bonato
How do you see the future of sample return?
We are currently in a golden age for sample return. Multiple missions have successfully returned samples from asteroids (Hayabusa, Hayabusa2, OSIRIS-REx) and the moon (Chang’e 5) in recent years. At the same time new missions are in preparation to return samples from Mars and its moon Phobos (MMX, Mars Sample Return).
I believe that it won’t stop here. In the coming decades, we will witness sample return missions expanding to an increasing number of objects. I am particularly excited about the prospect of sample return missions from Ceres and comets. As part of the sample return mission process, we are also dedicated to enhancing the handling and analysis of samples already on Earth. The collection, transportation, and storage of samples from other planets demand a detailed understanding of material properties, necessitating a new specialisation within the field of planetary science.
“We are currently in a golden age for sample return.”
Enrica Bonato
We can analyse samples much better in a lab on Earth than by using limited instruments on space missions. Will there be a shift towards sample return missions at the cost of traditional space missions?
Enrica Bonato carrying out acceptance tests of the Electron Microprope Analyser (EPMA) at JEOL GmbH in Freising (Germany). Credit: DLR..
“Sample return missions will complement other planetary science missions.”
Enrica Bonato
I believe that sample return missions will complement other planetary science missions. It’s crucial to bring a diverse array of instruments to the objects we’re interested in. On one hand, we need to assess and identify sites that are intriguing and suitable for sample return. On the other hand, we also need to conduct broader investigations of the objects to provide context for the analysis of the samples.
What are the main challenges for sample return in the coming decades?
Challenges will come from the new sample environments that we will access and new types of materials that we will sample, for example a potential future sample return mission from Venus’ surface. Building a spacecraft that can land on Venus’ extremely hostile surface and return a sample is extremely challenging. Challenges will also arise from returning a new type of sample: ice. So far the samples returned are rocks. Sampling ices from Ceres, comets or icy moons and keeping them frozen throughout cruise, the landing and later in storage on Earth brings unique challenges. Some of these technologies already exist in other fields, but a lot of new development is needed.
How did you plan the outfitting of the new sample return lab for DLR?
Dr Enrica Bonato and Dr Jörn Helbert (Head of the Planetary Laboratories at the DLR Institute for Planetary Research in Berlin-Adlershof) attending acceptance tests of the Electron Microprope Analyser (EPMA) at JEOL GmbH in Freising (Germany). The instrument will be moved to the SAL laboratory facilities as soon as the setup of the clean room is completed. Credit: DLR
I was the only person working on this project, alongside the grant holder, who also served as my supervisor. Before my involvement, there were already some initial planning and key milestones in place. My goal was to implement and adapt this plan throughout my time at DLR. I focused on specific techniques, aiming to establish a unique and specialised niche for the lab. Considering both the institute’s requirements and the broader scientific community, I selected instruments and managed their procurement. The next step in the project would be to upgrade the lab to a curation facility.
What are the key features of a dedicated sample return lab? And how might these differ from an equivalent Earth science lab?
The features are quite similar to an Earth science lab. Analyses often take place in labs at universities or research institutes, not necessarily tailored for a particular incoming sample. One notable distinction is the need for personnel to wear lab clothing and adhere to specific standards in sample handling so as not to contaminate samples.
Does the sample return lab at DLR possess any distinctive instruments or employ unique techniques for the analysis of samples that are not currently accessible to the broader community elsewhere?
The sample holders for XRD (X-Ray Diffraction) analysis allow for preparation within a glove box and subsequent analysis of the samples without exposure to air. Additionally, another unique feature is a sample transport shuttle that facilitates vacuum conditions between the Electron Microprobe and SEM (Scanning Electron Microscope), ensuring a controlled environment for the sample.
Acceptance tests of the Electron Microprope Analyser (EPMA) at JEOL GmbH in Freising (Germany). The instrument will be moved to the SAL laboratory facilities as soon as the setup of the clean room has been completed. Credit: DLR.
Exciting years ahead for sample return. Thanks Enrica!
Research Infrastructures (RIs) as key players of strategic autonomy in a changing global context
the socio-economic and environmental impact of RIs
the broad ecosystems of RIs.
In a mix of presentations and panel discussions, representatives of the European Commission, the Belgian Science Policy Office (BELSPO), the European Strategy Forum for Research Infrastructures (ESFRI), national policy makers and participants in a range of research infrastructures, discussed current challenges and future visions for the European RI community.
The conference also provided an opportunity to see and discuss the new ESFRI Landscape Analysis 2024. The Landscape Analysis provides a contextualised overview of the European RI ecosystem, identifying the main RIs operating transnational access in Europe, in all fields of research, and major new or ongoing projects. The Landscape Analysis 2024 will provide the framework for the next ESFRI Roadmap, which will set out strategic guidance for research infrastructures for the next 10-20 years.
Royal Belgian Library. Credit: Creative Commons/EmDeePresentation of the ESFRI Landscape Analysis at the Belgian Presidency Conference on ‘Research Infrastructures in a Changing Global, Environmental and Socio-economical Context.
As planetary science is such an interdisciplinary field, Europlanet works within a collaborative ecosystem of related astronomy and space RIs and networks, which include Opticon, Radionet, JIVE, Lofar, ChETEC-INFRA and the Square Kilometre Array (SKA).
The idea for an Astronomy & Space Network of Networks (NeoNs) was proposed in 2023, during a day of sessions at the Europlanet Research Infrastructure Meeting (ERIM) 2023 in Bratislava. The aim of Astronomy & Space NeoNs is to foster collaboration and provide coordinated feedback on astronomy and space science topics to policy makers. The first action of Astronomy & Space NeoNs was to provide feedback on the draft Physical Sciences and Engineering Domain of the ESFRI Landscape Analysis in 2023.
This input has clearly been noted. Astronomy & Space NeoNs is referenced in the Landscape analysis as “a recent network of RIs dedicated to Astronomy and Space Science, which facilitate transnational access to infrastructures”.
Importantly, due to feedback from Europlanet, coordinated through NeoNs, the title of the subdomain in PSE has been changed from ‘Astronomy and Particle Physics’ to ‘Astronomy, Astroparticle Physics and Space Sciences’. Although planetary science and related topics were previously covered in the description of this subdomain, the broadening of the title removes ambiguity and means that planetary science, astrobiology, astrochemistry are now explicitly included and given prominence under the PSE Domain.
Europlanet is also namechecked in the ESFRI Landscape Analysis document:
“…new facilities under construction are fully aligned and complementary with the major upcoming missions in space (such as the study of dark energy via Euclid, launched in 2023, the study of exoplanets via PLATO and ARIEL, the study of gravitational waves via LISA, space exploration such as the proposed missions to the Moon and Mars). Space-based observatories will require significant investment by European partners to secure leadership in missions led by ESA or in partnership with NASA, JAXA and other international space agencies. Experimental facilities should be complemented by e-infrastructures to cope with the rapidly developing Big Data capabilities of Machine Learning and Artificial Intelligence. Such networks of Research Infrastructures have been established (e.g. Opticon, Radionet, Europlanet) and are an essential part of the European Research Area. There is a long and successful European heritage here, and huge future potential across all areas of Astronomy, to include commercial return, computing and technology, training and outreach.”
These outcomes demonstrate the potential value of collaboration through Astronomy & Space NeoNs for the planetary community. The next steps in developing NeoNs will be discussed at the European Astronomical Society (EAS) Annual Meeting in Padova from 1-5 July.
The need for flexibility in legal structures for RIs was also raised at the conference in Brussels. The organisational structure for RIs favoured by the EC is the European Research Infrastructure Consortium (ERIC), a specific legal form designed to facilitate the establishment and operation of Research Infrastructures of European interest. ERICs are ‘participated by States’ and require approval at the national government level with council representatives usually appointed by government agencies. As of 22 December 2023, there are 28 ERICS, which represent only a fraction of the pan-European RI networks established over the last three decades. For small and medium-sized DRIs, the ERIC model may not be either optimal or practical, for example, when the DRI largely comprises facilities within universities and industry, and/or there is a need for flexibility in the type of infrastructure offered to communities.
Since 2021, Europlanet has been involved in the co-organisation of workshops for small to medium-sized Distributed Research Infrastructures (DRIs). In early 2024, Europlanet coordinated a survey to find out more about the ecosystem of DRIs, including the research areas covered, the DRIs’ funding models, their structures and plans for sustainability. Preliminary analysis of the survey responses show that, as alternatives to the ERIC structure, several DRIs have opted for the Association Internationale Sans But Lucratif (AISBL) model, which was adopted by Europlanet in 2023, or the French Loi 1901.
A fourth, in-person DRI workshop is planned in Budapest on 18 September 2024 as part of the Hungarian Presidency of the European Council, and the establishment of a formal DRI network is also being discussed. Further details about the workshop’s agenda and registration will be published soon.
Watch the recordings of Day 1 and Day 2 of the conference.
In dieser Lektion befassen wir uns mit dem pH-Wert bestimmter Umgebungen auf dem Mars und damit, wie sich dies auf seine potenzielle Bewohnbarkeit auswirken kann.
Zur Erinnerung: Lehrernotizen, Präsentationen und alle Inhalte können zur Anpassung und Verwendung in Ihrem Klassenzimmer heruntergeladen werden. Vergessen Sie nur nicht, uns als Quelle anzugeben (siehe “Nutzung der Ressourcen”).
Übersicht
Altersgruppe:
10-14
Benötigte Ausrüstung:
Computer
Projektor
Zeit der Lektion:
45 Minuten (einschließlich 1 Video)
Behandelte Themen:
Chemie (pH)
Biologie (Leben in Extremen)
Astronomie (Mars-Oberflächenbedingungen).
Lernergebnisse:
Gliederung der Aktivität: Verstehen, wie der pH-Wert des Mars die Bewohnbarkeit des Roten Planeten beeinflussen kann.
Nach Abschluss dieser Aktivität können die SchülerInnen:
Verstehen der pH-Skala.
Beschreiben Sie, wie Faktoren auf dem Mars den pH-Wert beeinflussen können.
Diskutieren Sie, wie der pH-Wert die Bewohnbarkeit beeinflusst.
Hintergrundmaterial:
Was ist der pH-Wert?
Aber bevor wir auf die Auswirkungen des pH-Werts eingehen, kann uns jemand erklären, was mit pH-Wert gemeint ist?
(Antworten nehmen)Mit dem pH-Wert messen wir den Säuregrad und die Alkalität. Basen und Säuren werden als chemische Gegensätze betrachtet, da die Wirkung einer Säure darin besteht, die Hydroniumkonzentration (H O3+ ) im Wasser zu erhöhen, während Basen diese Konzentration verringern. Eine Reaktion zwischen wässrigen Lösungen einer Säure und einer Base wird als Neutralisation bezeichnet, wobei eine Lösung aus Wasser und einem Salz entsteht, in der sich das Salz in seine einzelnen Ionen aufspaltet. Wenn die wässrige Lösung mit einem bestimmten gelösten Salz gesättigt ist, fällt jedes weitere Salz aus der Lösung aus.
pH-Skala
Der pH-Wert wird in der Regel anhand der pH-Skala gemessen. Verbindungen mit niedrigem pH-Wert sind sauer, was von einer starken Säure bei pH 1 bis zu einer schwachen Säure bei pH 6 reicht. pH 7 gilt als neutral und ein pH-Wert darüber ist basisch, von pH 8 bis 14.
Diskutieren Sie, wie Ihrer Meinung nach der pH-Wert auf dem Mars sein könnte?
Jetzt, da Sie einige Hintergrundinformationen haben, was würden Sie erwarten, dass der durchschnittliche pH-Wert auf dem Mars ist?
(Antworten nehmen)
Wie können wir den pH-Wert feststellen?
Um dies zu wissen, müssen wir zunächst in der Lage sein, den pH-Wert zu bestimmen. Wie können wir das tun?
(Antworten nehmen)
pH-Skalen sind oft farbig. Dies ist auf die übliche Verwendung einer Lösung zurückzuführen, die Universalindikator genannt wird und zur Anzeige des pH-Werts ihre Farbe ändert. Bei Anwesenheit einer Säure färbt er sich rot, bei neutralem pH-Wert wird die Lösung grün und bei Anwesenheit einer Base tiefblau/violett. Es gibt jedoch auch andere Indikatoren wie Phenolphthalein, das sich in Gegenwart einer Base rosa färbt und bei einer Säure keine Farbänderung zeigt. pH-Indikatoren finden sich sogar häufig in der Küche – wie der Saft eines Rotkohls, der sich in Gegenwart einer Base blau-grün und bei einer Säure rosa färbt.
Video: Erkennung des pH-Wertes
Hier haben wir ein Video, das den Farbwechsel einer Lösung bei Verwendung eines Universalindikators zeigt:
Hintergrundinformationen zum Video: In diesem Video wird eine Lösung von schwach konzentriertem Natriumhydroxid (NaOH) gezeigt. Universalindikatorlösung wird hinzugefügt, die die Lösung violett färbt. Anschließend wird eine 5%ige Essigsäurelösung in Form von handelsüblichem weißem Kochessig zugegeben. Die Lösung mit dem Universalindikator färbt sich rot.
Was ist passiert? Warum?
Bitte diskutieren Sie in Gruppen, was Sie in diesem Video beobachtet haben. Warum, glaubt ihr, ist das passiert?
(Zeit für Gruppendiskussion einplanen)
(Antworten nehmen)
Rio Tinto Fluss
Es gibt auf der Erde Gebiete mit extremen pH-Werten. Ein solcher Ort ist der Fluss Rio Tinto in Spanien. Der pH-Wert des Rio Tinto erreicht in einigen Bereichen des Flusses einen Wert von bis zu 2,3, was zeigt, dass diese Umgebung sehr sauer ist. Dieser niedrige pH-Wert wird durch Wechselwirkungen zwischen Gestein und Mikroorganismen im Fluss verursacht, die als Gesteins-Wasser-Biologie-Wechselwirkungen bekannt sind. Dies führt dazu, dass große Mengen an Verbindungen wie Schwefelsäure, Sulfate und Eisen(III)-Eisen im Flusswasser vorhanden sind. Letzteres verleiht dem Rio Tinto seine charakteristische rote Färbung.
In dieser extremen Umgebung wurden sowohl eukaryotische als auch prokaryotische Organismen beobachtet, die unter den sauren Bedingungen gedeihen. Daher ist der Rio Tinto ein analoges Planetenfeld, das uns Aufschluss über die Aussichten auf Leben in extremen Umgebungen anderswo im Sonnensystem geben kann.
Wie wirkt sich CO2 auf den pH-Wert aus?
Zurück zum Mars: Die Marsatmosphäre besteht hauptsächlich aus Kohlendioxid, und an den Polen des Mars gibt es große Ablagerungen von festem Kohlendioxid.
Welche Auswirkung hat Kohlendioxid Ihrer Meinung nach auf den pH-Wert? Bitte diskutieren Sie in Gruppen.
(Zeit für Gruppendiskussion einplanen)
(Antworten nehmen)
Wenn Kohlendioxid in Wasser gelöst wird, entsteht Kohlensäure, die den pH-Wert auf dem Mars senkt. Kohlensäure ist etwas, dem viele Menschen täglich in Form von kohlensäurehaltigen Getränken begegnen. Wenn Sie jemals einen merkwürdigen Nachgeschmack in kohlensäurehaltigem Wasser bemerkt haben, ist dies auf das Vorhandensein von Kohlensäure zurückzuführen. Einer der Gründe, warum bei der Entwicklung von kohlensäurehaltigen Getränken so viel Zucker verwendet wird, besteht darin, genau diesen Geschmack zu überdecken.
Wie könnte sich dies auf die Bewohnbarkeit auswirken?
Wie würde sich Ihrer Meinung nach das Vorhandensein von Kohlensäure auf die mögliche Bewohnbarkeit des Mars auswirken? Bitte diskutieren Sie in Gruppen.
(Zeit für Gruppendiskussion einplanen)
(Antworten nehmen)
Rückblick
Nach dieser Lektion sollten die Schüler in der Lage sein, diese Fragen zu beantworten:
Was zeigt eine pH-Skala an?
Welche Faktoren auf dem Mars (früher oder heute) könnten den pH-Wert beeinflussen?
Wie könnte sich der pH-Wert auf die Bewohnbarkeit des Mars auswirken?
In dieser Lektion befassen wir uns mit der Entwicklung von Salzschichten und dem Potenzial für ihre Bewohnbarkeit.
Zur Erinnerung: Lehrernotizen, Präsentationen und alle Inhalte können zur Anpassung und Verwendung in Ihrem Klassenzimmer heruntergeladen werden. Vergessen Sie nur nicht, uns als Quelle anzugeben (siehe “Nutzung der Ressourcen”).
Übersicht
Altersgruppe:
10-14
Benötigte Ausrüstung:
Computer
Projektor
Zeit der Lektion:
45 Minuten (einschließlich 1 Video)
Behandelte Themen:
Chemie (Zustände der Materie)
Biologie (Leben in Extremen)
Astronomie (Mars-Oberflächenbedingungen).
Lernergebnisse:
Gliederung der Aktivität: Verstehen Sie die Entstehung von Salzpfannen durch den Mechanismus der Verdunstung.
Nach Abschluss dieser Aktivität können die SchülerInnen:
Verdunstung kritisch prüfen
Zustände der Materie verstehen
Beschreiben Sie, wie sich Salzgehalt und Austrocknung auf die Bewohnbarkeit einer Umgebung auswirken.
Hintergrundmaterial:
Verdunstung
Zunächst einmal müssen wir uns mit der Verdunstung befassen. Kann jemand erklären, was mit Verdunstung gemeint ist?
(Antworten nehmen)
Verdampfung ist der Prozess, bei dem eine Flüssigkeit von einem flüssigen in einen gasförmigen Zustand übergeht. Dies kann viele Formen annehmen – das häufigste Beispiel ist ein Prozess, der oft als Lufttrocknung bezeichnet wird. Dies geschieht dadurch, dass Flüssigkeitsmoleküle an der Oberfläche in einen Dampf entweichen. Ein weiteres Beispiel ist das Sieden, das auftritt, wenn die Temperatur einer Flüssigkeit ihren Siedepunkt überschreitet (im Falle von Wasser ist dies 100 ⁰C). Wenn Wasser die Temperatur von 100 ⁰C überschreitet, wird es zu Dampf. Entgegen der landläufigen Meinung ist Dampf unsichtbar, und die Wolken, die man über kochendem Wasser sehen kann, sind in Wirklichkeit Dampf oder Wasserdampf, der wieder zu Tröpfchen flüssigen Wassers kondensiert.
Aggregatzustände der Materie
Wir haben bereits über die Idee der Materiezustände gesprochen, aber kann jemand erklären, was die Materiezustände sind?
(Antworten nehmen)
Ein fester Zustand behält seine Form bei. Seine Moleküle sind viel stärker strukturiert und haben nicht die verfügbare Energie, um sich frei zu bewegen. Bei den meisten Verbindungen ist ihre feste Form die dichteste Form. Es gibt jedoch Ausnahmen von dieser Regel, z. B. Eis, das eine geringere Dichte hat als flüssiges Wasser. Dies ist auf seine molekulare Struktur als Festkörper zurückzuführen.
Wenn eine Verbindung mehr Energie erhält und schmilzt, haben wir die flüssige Form einer Verbindung. Eine Flüssigkeit ist ein Fluid, das heißt, sie kann fließen und die Form ihres Behälters annehmen. Einige Flüssigkeiten können recht instabil sein, sie verdampfen leicht oder benötigen sogar einen hohen Druck, um sich überhaupt zu bilden, wie z. B. Kohlendioxid. Wenn ein Feststoff wie Kohlendioxid unter normalem Erddruck von einem Feststoff zu einem Gas wird, spricht man von Sublimation. Der letzte Aggregatzustand, der im Rahmen dieser Lektion behandelt wird, ist, wie bereits erwähnt, Gas. Gase sind wie Flüssigkeiten flüssig und füllen je nach ihrer Dichte den gesamten verfügbaren Raum aus.
MakgadikgadiSalzpfannen und Formation
Auf diesem Foto sehen wir die Makgadikgadi-Salzpfannen in Botswana. Dies ist eine riesige Salzfläche, die für die Erforschung der Mikrobiologie in Gebieten mit hohem Salzgehalt sehr wertvoll geworden ist.
Diskutieren Sie, wie diese Umgebung entstanden ist
Diskutieren Sie in Gruppen, wie diese Umgebung entstanden sein könnte.
(Zeit für Gruppendiskussion einplanen)
(Antworten nehmen)
Video: Wie geschieht das?
Hier haben wir ein Video, das zeigt, wie sich eine Umgebung wie die Makgadikgadi Salzpfannen gebildet haben könnte.
Hintergrundinformationen zum Video: In diesem Video haben wir eine gesättigte Lösung von Natriumchlorid (NaCl). Wenn das Wasser weggekocht wird, wird die Lösung übersättigt. Bei weiterer Verdampfung wird sie übersättigt und das Natriumchlorid fällt aus der Lösung aus. Das Natriumchlorid hat eine viel höhere Dichte als der Wasserdampf und liegt deutlich unter seinem Schmelzpunkt, geschweige denn unter seinem Siedepunkt. Wenn also das Wasser verdampft, bleiben die dichteren festen Verbindungen wie das Natriumchlorid zurück.
Glaubst du, dass dort Leben überleben kann?
Bitte diskutieren Sie in Gruppen, ob Sie glauben, dass Leben in einer Umgebung mit so hohem Salzgehalt überleben kann.
(Zeit für Gruppendiskussion einplanen)
(Antworten nehmen)
Salz- und austrocknungstolerante Bakterien
Austrocknung (ein Zustand extremer Trockenheit) ist eine häufige Belastung, der Bakterien in der natürlichen Umgebung ausgesetzt sind. Daher haben sie eine Vielzahl von Schutzmechanismen entwickelt, um die durch den Wasserverlust verursachten Schäden abzumildern. Einige Arten haben Mechanismen entwickelt, die entweder dazu beitragen, anfällige Zellbestandteile vor Schäden zu schützen, oder die Wasser sequestrieren, um eine Dehydrierung zu vermeiden. Zu diesen Mechanismen gehören die Veränderung der Membranzusammensetzung oder die Modifikation von Lipopolysacchariden, um die Membranen während des Austrocknens zu stabilisieren, sowie die Anhäufung von kompatiblen gelösten Stoffen wie Trehalose, die Zytoplasma- und Membranbestandteile schützen können. Dies hat einige zu der Annahme veranlasst, dass Leben in extremen Umgebungen wie dem hohen Salzgehalt auf dem Mars überleben könnte.
Rückblick
Nach dieser Lektion sollten die Schüler in der Lage sein, diese Fragen zu beantworten:
Was sind die verschiedenen Zustände der Materie?
Können Sie das Konzept der Verdunstung erklären?
Wie könnten Salz und Austrocknung die Bewohnbarkeit des Mars beeinflussen?
Europlanet Joins Swiss Space Area at Fantasy Basel
The space area at the 2024 edition of FANTASY BASEL, the Swiss Comic Con, had an exhibition and hands-on activities led by the Swiss Space Museum and its partners, including the National Centre of Competence in Research (NCCR) PlanetS and colleagues from Europlanet.
This year, we asked again the important question: what do you think a comet smells like? Over the three days, we collected 328 creative responses to this question, and talked to up to 10,000 attendees on the stand overall.
Responses ranged from :
Acacia honey
Fresh rain
A dusty cellar
Dirt mixed with water
Toilet cleaner
Flowers
Urine
A mossy cave
Old socks
Burned rock with caramel
Waste with mint
Incense and sandalwood
Holy somke1
Bergamot
Stone dust
Skunk
Sulfur and rose
Fizzer sweets
My cat after it went under the dusty bed
Out of this world 😉
Vick’s Vapo-Rub
Rotten dust / feet
Menthol
Sandalwood
Foul eggs
Esoteric store
Tiger balm
Chalk
The zoo
and many more!
Many thanks to the organisers for a fantastic event!
Europlanet Transnational Access on Show at ATOMKI-Hosted Workshop
The HUN-REN Nuclear Research Institute (ATOMKI) recently hosted a two-day workshop on Radiation-Driven Chemistry in Astrophysics and Planetary Science. Around 45 international participants attended and discussed developments in astrochemistry and present the latest results of research. The first day finished with a round-table discussion on some of the challenges and opportunities for the astrochemistry community
Several presentations over the two days featured work carried out through the Europlanet 2024 Research Infrastructure (RI) Transnational Access programme in the ATOMKI laboratories.
Find out more about how the ATOMKI facilities have been developed through support from the Europlanet 2024 RI project.
Report from the Radiation-Driven Chemistry in Astrophysics and Planetary Science Workshop
(Reposted in English from the original on the ATOMKI website, with thanks to ATOMKI and the workshop organising committee.)
The HUN-REN Nuclear Research Institute (ATOMKI) recently hosted specialists researching chemical processes in outer space. The aim of the two-day event called Radiation-Driven Chemistry in Astrophysics and Planetary Science Workshop was to review the development directions of astrochemistry and to present the latest results of measurements carried out in the ATOMKI laboratories in the framework of international collaborations.
The starry sky is magical and enchanting. Humanity has been preoccupied with the regularities observed in the movement of celestial objects since its inception. In addition to observing with the naked eye, thanks to the development of technical devices, we first used binoculars and then spectroscopic (spectroscopic) methods to spy on the sky. And the space tools launched into outer space expanded our horizons and our possibilities explosively. Today, many disciplines deal with the study of our remote environment.
Astrophysics – hand in hand with astronomy – deals with the origin, history and structure of the world, the creation of chemical elements, and nuclear physical processes taking place in stars. Nuclear astrophysics research is largely carried out with the help of particle accelerators, where nuclear physics reactions are created, modeling the processes taking place in stars.
Astrochemistry studies the chemical processes taking place in outer space. How do more complex molecules form in the cradles of stars, in these very cold and distant molecular clouds, in the thin layers of ice containing atoms and smaller molecules deposited on the particles of cosmic dust? What chemical transformations take place on the surface and atmosphere of planets, moons, comets, and asteroids?
According to research, it is becoming more and more obvious that cosmic radiation and the high-energy particles emitted by stars, such as photons, ions and electrons, play a decisive role in these chemical processes. Their flow is called the stellar wind or, in the case of the Sun, the solar wind.
With the help of instruments on the ground and in space, we can also determine the chemical composition of very distant celestial bodies and nebulae. Among the hundreds of molecules detected in outer space, you can find the building blocks of living organisms, as well as larger organic molecules. Astrobiology deals with the study of the processes leading to the creation of life.
Molecules in the distant regions of outer space can be identified with the help of space telescopes (such as the James Webb Space Telescope) that use the method of radio astronomy and spectrum analysis in the infrared range (spectroscopy), and thus learn something about the chemical processes taking place there. In the closer places, within the Solar System, the probes of the space missions perform direct sampling and measurements.
However, in order to interpret the data, it is necessary to model the effect of cosmic radiation, the stellar wind, and the solar wind on molecules and thus on chemical processes here on Earth in laboratory conditions. Most of the processes taking place in the Solar System can be modeled with the help of high-energy ions and electrons created by ATOMKI’s particle accelerator equipment, ion and electron sources. Dozens of foreign groups come to the institute every year to take advantage of the facilities offered by the equipment.
With the particle beam, ices of a special composition are irradiated, such as are found on the surface of icy celestial bodies in our Solar System. Chemical changes are followed by infrared spectroscopic methods. In the research in this direction at the institute, the focus of attention is currently on the experimental modeling of the processes taking place on the icy moons of the planet Jupiter. With these experiments, ATOMKI supports the Jupiter Icy Moons Explorer (JUICE) mission of the European Space Agency (ESA).
April 25-26, 2024. The two-day meeting that took place between The majority of the 43 participating researchers came from Europe and America. The cooperating partners reported on the results of their measurements carried out in the laboratories of ATOMKI. The leading researchers of the profession analyzed the directions of the development of astrochemistry and reviewed the opportunities and challenges that arise in relation to astrochemistry in the fields of space research, space industry and climate research. The experts visited ATOMKI’s particle accelerator equipment and laboratories, where research conducted in international cooperation can continue in the future.
This workshop is organised and supported by the Europlanet 2024 Research Infrastructure (RI) project, which has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 871149.
Report Summary: Sound knowledge of the processes and conditions that drive hydrothermal systems is one of the prerequisites to understand not only the geological, geochemical, and geophysical evolution of our planet and other terrestrial planets, especially Mars, but also to shed light on the origin and early evolution of life since hydrothermal systems can be hospitable to certain life forms.
The use of the unique experimental set-ups of the reaction chambers at Open University allows determination of the mass transport of dissolved metals with either continuous sampling of the fluid or recirculation the fluid with built-in Ti gaze as precipitation traps. We used this set up to better understand environmental conditions during active hydrothermal alteration.
The source rocks of the experiments were fresh basalts from the Indian ocean ridge that served as analogue material to the Martian surface. The fluid was Indian ocean seawater sampled 100m above seafloor.
We observed precipitation of minerals like Ca-sulphates, NaCl, FeOOH and Fe-Mg-Na-containing clay minerals, but also native Ta and Fe-Ni-Cr alloy. While the ions of the mineral phases originated from leaching of the basalt, the metals might have come from the stainless-steel tube that served as container of the Ti gaze.
Based on the newly formed minerals, the pH – redox state – conditions can be deduced. This information is a prerequisite together with the cations enriched in the post-run fluid phase to allow geochemical reaction-path modelling which will be the next step after the post-run fluids are analysed at Kiel University.
Report Summary: In the search for evidence of ancient terrestrial life there are some obstacles. Purported biosignatures have been identified in a range of ancient mineral deposits, including silica. However, some of these signatures can also be generated under abiotic conditions, which brings into question their biological origin. In addition, the oldest fragments of the Earth’s crust are at least 3.8 Gyr, and would have experienced significant metamorphic alteration since their formation. Therefore, any preserved biosignatures could have also undergone extensive modification during metamorphism potentially making some of them unidentifiable. This project aimed to examine the effect of metamorphism on the modification of biosignatures preserved in silica deposits.
Silica sinters were synthetically created in the laboratory via evaporation in the presence and absence of microbes. These samples were then exposed to simultaneous high temperature and high pressure conditions using the end-loaded piston-cylinder at the (Exo) Planetary Interior Simulation Laboratory (PISL), VU University, Amsterdam. Samples were individually subjected to pressures and temperatures of 650 °C and 12 kbar, respectively, for 20 hours. Raman spectroscopy and GC-MS will be used to assess changes in mineralogy and to quantify changes to organic molecules. Initial results obtained after returning to my home institution show that the high pressure and high temperature conditions experienced in these experiments led to changes in the crystalline structure of the samples. This resulted in samples transforming from silica glass to quartz.
22-EPN3-124: Unfolding Geochemical Evolution of the Subcontinental Lithospheric Mantle Recorded by Diamond-Forming Carbon and Water Rich (C-O-H) Mantle Fluids Throughout Time
Report Summary: Fibrous diamonds from the Voorspoed, Venetia and Koffiefontein mines record deep mantle events involving C-O-H fluid types, alongside gem diamonds containing mineral inclusions that were related to modification episodes of the Kaapvaal lithospheric region. Although a connection has been made, the longstanding debate between diamond formation in the mantle and the relationship between gem diamonds and fibrous diamonds is yet to be resolved.
While we have extensive radiometric dating of mineral inclusions trapped in gem diamonds, alongside knowledge about the major and trace elements of C-O-H fluid microinclusions in diamonds, their radiogenic isotopic data is insufficient (e.g. Sr, Nd, and Pb isotopes). High-precision Sr-Nd-Pb isotope TIMS analyses of C-O-H mantle fluids in diamonds from these three prime locations in the Kaapvaal craton were preformed using a novel laser ablation diamond-in-water technique, combined with ultra-low blank column chromatography and 1013 Ohm resistors.
The team successfully processed and analysed 12 samples from Voorspoed, 5 from Venetia and 5 from Koffiefontein mines, as well as standards and blanks. The collected data show intriguing Sr-Nd-Pb relationships that vary between diamonds carrying different C-O-H fluids. The team has further data processing and calculations to complete, as well as correlate the isotopic ratios with trace element compositions to fully understand the results and their geological significance. The outcome of this Europlanet project is expected to provide new insights into the complex tectonic history of this lithospheric province, the fluids themselves and the connection between different diamond types and their formation mechanism.
Report Summary: The formation of bedded barite (BaSO4) deposits in the low-sulfate environments of the early Earth has been a long-standing paradox despite decades of field and geochemical studies. In this project, the team investigated the Si isotope geochemistry of chert (SiO2) dykes and beds found in association with barite to evaluate roles of hydrothermal fluids and seawater during barite formation. A total of 14 chert samples from three localities in the ~3.3 Ga Mapepe and Mendon Formations of the Barberton Greenstone Belt, South Africa were microdrilled and dissolved using sodium hydroxide digestion. Pure silicon fractions were obtained using cation exchange chromatography columns, and analysed for 29Si/28Si and 30Si/28Si isotope ratios by multi-collector inductively-coupled plasma mass spectrometry (MC-ICP-MS) in wet plasma mode using standard-sample bracketing for mass bias correction. Measured silicon isotope ratios (δ30Si) range from 0.27 to 1.29‰. Chert dykes (n = 6) and bedded cherts (n = 3) have similar silicon isotopic compositions, with an average δ30Si value of 0.88‰ for the dykes and 0.80‰ for the bedded cherts. Black chert from the Mendon formation is isotopically distinct (δ30Si = 0.45‰) from the Mapepe Formation cherts. These results tentatively suggest that the chert dykes and bedded cherts associated with barite formed from isotopically-heavy seawater (δ30Si > 0‰), and that the role of high-temperature hydrothermal fluids (δ30Si < 0‰) was limited.
20-EPN2-117: To the Root of a Problem – Exploring Mars’s Rootless Cones Based on the Geomorphometry of Icelandic Analogues
Sebastiaan de Vet (TU Delft, Netherlands) and Lonneke Roelofs (Utrecht University, Netherlands) to TA1.1 – Iceland Field Sites, MATIS Dates of visit: 04-12 July 2022
Rootless cones are created by steam explosions when lava flows interact with local water sources. Consequently, these landscape features offer a unique palaeo-environmental insight into the conditions at the time of the eruption. Rootless cones have also been identified on planet Mars. The aim of this project was to identify geomorphological and morphometric characteristics of Icelandic rootless cones and use these insights to infer the formation conditions and palaeo-environmental significance of rootless cones on the planet Mars. While features on Mars can only be studied remotely through satellite data, this project leverages the accessibility of lcelandic analogues to study their morphologies and properties in fine details. The rootless cone groups in the Younger Laxa Lava are uniquely and specifically suited for this purpose; they offer a morphological variety along various gradients of lava-water interactions.
During the field project the team intended to map representative rootless cones in the Younger Laxa Lava in high-resolution during a drone-assisted photogrammetric survey and analyse high-resolution Digital Terrain Models to quantitatively compare rootless cones on lceland and Mars. However, logistical issues arising in the aviation industry during Summer 2022 resulted in a temporary loss of fieldwork gear. The project was thus refocussed to carry out a field campaign to collect representative pilot-dataset to meet parts of the initial goals and prepare for a future follow-up campaign.
Banner image: A rootless cone at Myvatn Lake, Iceland. Credit: Hansueli Krapf/CC BY-SA 3.0
22-EPN3-005: Spatial Relationship Between Biosignatures and Their Geologic Context by Large-scale Geoscientific Mapping at Rio Tinto, Spain
Visit by Alessandro Frigeri (INAF, Italy) and Giacomo Panza (intern at INAF, University of Bologna, Italy) to TA1.2 Rio Tinto (Spain). Dates of visit: 07-11 November 2023
Report Summary: Since the early 2000’s, Rio Tinto has been a critical witness plate for the investigation of extremophiles and it is recognized to be a mineralogical and geochemical analog of Mars (Amils et al., 2014). The Mars Analog Rio Tinto Experiment (MARTE), in particular, demonstrated that the Rio Tinto biosphere extends at least 900 meters below the land surface with a high potential of anaerobic microorganisms to be present (Stoker et al., 2008). Host rocks, however, are exposed at the surface in sediments and rocks of the Rio Tinto watershed, providing potential for key investigations.
The Rio Tinto 2023 field campaign was held between November 7th and November 18th 2023 at Rio Tinto Terrestrial Analogue. The campaign team was made by Alessandro Frigeri (INAF, Italy), James Skinner (USGS, US), Giacomo Panza (undergrad student at University of Bologna, intern at INAF) and Felipe Gomez as the TA Field expert (Centro de Astrobiologia, Madrid).
The campaign focused on geologic surveying and mapping the spatial relationship of the rocks where extremophile life develops today and has evolved through the geologic times. When bacteria proliferate within a solid media in a natural environment, microbial life alters the hosting environment chemically and physically. When the hosting media are soils and rocks, geological aspects like color, grain size, texture, and composition will be altered by the presence of life. Before the campaign, the team prepared a context cartographic base from remote sensing data from which they defined three sites of interest with different geological characteristics where to observe and map biosignatures.
In the field, the team applied traditional geological field large-scale mapping techniques coupled with photogrammetric drone surveys and drafted specific geoscientific mapping themes describing the geospatial setting of biosignatures at Rio Tinto Planetary Field Analogue in Spain.
22-EPN3-77: Preservation of Organic Matter in Glacial Lakes: Implications for Martian and Icy Moon Biosignatures
Visit by Charlotte Spencer-Jones (University of Durham, UK) and Sevasti Filippidou (Imperial College London, UK) to TA1.4 AU Greenland Kangerlussuaq Field Site (Greenland). Dates of visit: 25 July – 02 August 2023
Report Summary: In the search for extra-terrestrial life, environments that have previously contained water are a key target. Glacial environments, such as those found in Greenland, are highly dynamic ephemeral systems with a range of habitat types that support many different species, from bacteria and archaea to large mammals and higher plants. Organic carbon (OC) compounds, the fundamental building blocks of life, can be used to trace different species and/or biogeochemistry. The aim of the fieldwork campaign was to characterise OC in the lake water column to establish OC synthesis patterns in glacial lakes. In this study we collected water, sediment, and soils from 13 sites from a range of lake types near Kangerlussuaq, Greenland.The second phase of this study will be to characterise organic compounds within the samples. The outcome of this work will be to establish the key parameters that control organic compound preservation with the potential to impact the interpretation of putative extra-terrestrial biosignatures.
Read the full scientific report with kind permission by Charlotte Spencer-Jones and Sevasti Filippidou.
22-EPN3-127: Silcrete deposits of the Kalahari Desert as potential analogs for silica-rich deposits on Mars
Visit by Maxime Pineau (Laboratoire d’Astrophysique de Marseille (LAM), France) and Simon Gouzy (Laboratoire de Planétologie et Géosciences (LPG), France) to TA1.5 Makgadikgadi Salt Pans (Botswana). Dates of visit: 21-28 August January 2023
Report Summary: Hydrated silica occurs in various forms depending on the geological context and as such are good tracers for paleoenvironmental reconstitutions on Earth and Mars, as well as a prime exobiological target. Observed on Mars since the early 2000’s, hydrated silica minerals have been used to describe aqueous geological processes in diverse regions. However, geological origins of some deposits are still misunderstood because no satisfactory terrestrial analogues were found. Likewise, the exobiological potential of hydrated silica as a prime host of Mars organic matter remains to be fully ascertained.
The Makgadikgadi Salt Pans show a very high potential to be considered as a terrestrial analogue site for Mars hydrated silica, especially in fluvio-lacustrine geological settings. Maxime Pineau (LAM), Simon Gouzy (LPG), plus 2 other colleagues (Vassilissa Vinogradoff (PIIM) and John Carter (LAM)), spent 9 days at the pans (15 different locations) and sampled numerous samples (over 80s) of silicified clastic sedimentary rocks (i.e., silcretes) and conducted preliminary visible-near infrared spectra with a portable spectrometer.
Field observations and spectral analyses confirm the large amount of amorphous to (micro-)crystalline silica in the samples, along with different clays (e.g., glauconite, sepiolite) and salts (e.g., sulfates). This type of mineralogy, possibly indicating a formation in a fluvio-lacustrine context in semi-desert environments, is reminiscent of some silica-rich deposits on Mars in locations interpreted as potential paleo-lakes. These observations will be completed by further laboratory measurements (spectroscopy, microscopy, geochemical and organic analyses) in order to perform advanced studies in terrestrial geology, comparative planetology (e.g., Mars’ geology) and astrobiological exploration.
Report Summary: The possibility that prebiotic precursors of life formed in the space and were then transported to the early Earth by comets, asteroids and meteorites is a fascinating hypothesis. We focus in this project on hydroxylamine, NH2OH, a key N-bearing species that has been proposed as an important precursor in the formation of amino acids like glycine or alanine. Very recently, hydroxylamine has been detected in the gas phase in dense clouds in the interstellar medium. It has been predicted to form efficiently on dust grains according to laboratory experiments and chemical models. Then, the presence of this species in ISM ices and on the surface of Solar System bodies is probable, and in those surfaces can react to form more complex prebiotic species like amino acids.
Although the chemical pathways leading to the formation of NH2OH in astrophysical ices have been thoroughly studied, the next step in the chemical evolution that would begin with NH2OH as a precursor in ice has, to our knowledge, not been addressed experimentally.
In this TA project the team studied the chemistry induced by Cosmic Rays on ices containing hydroxylamine. They studied pure NH2OH ices and mixtures with H2O, CO and D2O, at 20 K, irradiated with 15 keV H+ ions. In particular, we were interested in finding complex organic molecules in the processed ices, and learning how different ice composition affects the chemistry and the destruction efficiency of NH2OH by Cosmic Rays.
Report Summary: During this TNA visit, the simplest amino acid glycine (NH2CH2COOH), and its deuterated analogs, partially deuterated d3-glycine (ND2CH2COOD) and fully deuterated d5-glycine (ND2CD2COOD), were irradiated using 10 KeV protons. The subsequent products of this processing were then measured using infrared spectroscopy and a quadrupole mass spectrometer. The aim of this was to investigate the products of glycine destruction and investigate if this energetic processing could result in the formation of glycine peptides. The outcome of the TNA visit was the collection of infrared spectra of the irradiation of these molecules and then following this, temperature-programmed desorption measurements. These preliminary results show the formation of CO2, CO, and D2O.
Report Summary: During this TNA visit, the three-ring PAH phenanthrene (C14H10), acetonitrile (CH3CN) and their 1:1 mixture were irradiated using 10 KeV protons. The subsequent products of this processing were then measured using infrared spectroscopy (5000-700 cm-1) and a quadrupole mass spectrometer.
The aim of these experiments was to investigate 1) if energetic processing can modify the structure of solid hydrocarbons and 2) if proton irradiation could trigger the formation of new species. During the visit to Atomki, the team collected infrared spectra of at different proton fluences and then following this, infrared spectra during temperature-programmed desorption (TPD). They also obtained the residues after TPD for ex-situ analysis. The preliminary results show a) the puckering of phenanthrene solid, b) the formation of ethanimine (C2H5N) in acetonitrile solid, c) a complex behaviour of the 1:1 mixture, with puckering and formation of new hydrocarbon species.
Full scientific report published by kind permission of Alessandra Candian and Annemieke Petrignani.
Report Summary: Several of the icy moons of Jupiter possess a liquid water ocean under a thick icy crust. In the especially promising case of Europa, a young surface (>100 Myr), and likely recent cryovolcanicactivity (within the last 8 years) imply the presence of ocean material on the surface. Therefore, observations performed by space missions could determine the ocean’s composition, and derive indications on its potential habitability (presence of chemical gradients providing metabolic energy, quantity and composition of available organic matter…). Characterising Europa’s ocean and its possible habitability requires to understand processes that alter organic and inorganic molecules in this environment. These processes include the processing by energetic ions coming from Jupiter’s magnetosphere and hitting the surface.
In this project, Alexis Bouquet visited the Atomki facility to study the effect of sulfur ion bombardment on methanol, a species that could be indicative of key characteristics of the ocean, pure and within an ice matrix. The alteration of the sample was followed using infrared spectroscopy, and the resulting complex organic residues were retrieved for ultra-high resolution mass spectrometry.
Report Summary: Despite being only the tenth most abundant element in space, sulfur is a component of several biomolecules, making it a key subject for astrochemistry studies. Sulfur containing molecules were observed in the solid phase on the surfaces of icy moons and in the icy mantles of interstellar grains. Despite the seemingly ubiquitous detection of sulfur-bearing species in space, the sulfur budget is still puzzling the scientific community. To address this, Zuzana Kaňuchová and Tom Field conducted an exploratory series of irradiation experiments to determine if species with thiol (-SH) groups may be formed in hydrocarbon-rich ices at temperatures relevant to interstellar matter, the surfaces of Solar System icy satellites, and Kuiper Belt objects.
They implanted 200 keV S+ ions in methane (CH4), ethane (C2H6), ethene (C2H4), and ethyne (C2H2) ices at 20 K and 60 K. Formation (and destruction) of species was monitored via FTIR spectroscopy and quadrupole mass spectrometry. Based on preliminary analysis performed during the TA they decided to conduct one extra (supplementary) experiment to explore the possibility of forming carbon and sulfur-bearing molecules by implanting high-energy carbon (750 keV) ions into hydrogen sulfide (H2S). The preliminary analysis does not indicate the formation of thiols in the investigated hydrocarbon ices as a result of high-energy sulfur ions implantation. However, several new absorption bands appeared in the spectra of all irradiated hydrocarbons, indicating the formation of various alkanes and alkenes. The emergence of a prominent band around ~1600 cm-1 could suggest the presence of carbon in an amorphous form.
Europlanet 2024 RI has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement No 871149.
Europlanet AISBL (Association Internationale Sans But Lucratif - 0800.634.634) is hosted by the Department of Planetary Atmospheres of the Royal Belgian Institute for Space Aeronomy (BIRA-IASB), Avenue Circulaire 3, B-1180 Brussels, Belgium.
