Search

Nowadays, it is universally accepted that the exodus of the peoples from the African continent all those millenia ago gave the rest of the world our populations; it is a historical fact that it is they are the ones who migrated across the globe in the great human diasporas. It is a pitiful shame that the very same continent which spawned the original trailblazing migrations is hit by a double whammy. First, the descendants of those earliest peoples invaded Africa continent to enslave, pillage and plunder which ostensibly caused a halt in the advancement of Africa as a global contender and resulted in an apparent lack of comparable education for the surviving local populace; this is still all too obvious across the African continent. Second, it is largely the actions of the developed nations which brought about the climate change which is now having a profound effect on the African continent. My presentation will focus on the outcomes from NoRCEL’s recent Blue Earth Project (BEP2022) interactive event which illustrates the relevance of the need for a more improved level of climate change education in Africa.

Currently there are low levels of access to high quality education and learning facilities in certain developing nations, especially in sub-Saharan Africa. For example, at best, some university facilities there are barely comparable to western high school levels and, at worse, they don’t even have modern laboratory equipment; the basics that they do have being relics from the 1960’s and 70’s. In addition, I know of at least one secondary school in Malawi where there are two “sittings” —a morning session for one set of pupils and an afternoon for the second. Both with the same teachers. That is to say, there is both the lack of qualified teachers and they cannot afford to expand the school. During the last six years I myself have been promoting science throughout parts of the developing world, principally through astronomy because this is one science which is common to humanity. I have given numerous oral presentations on space in general, astrochemistry, astrobiology and astrophysics as well as helping to promote an interest in these subjects by holding specific workshops. Until now, I have been operating as a “one-man band” and the challenge is to encourage students to become involved and active in astronomy, astrophysics, astrochemistry and astrobiology (theastrocsiences) and then to support them should they wish to progress further and take up a career in these fields. There are many difficulties to overcome, including lack of awareness and inclusion with the wider world, as well as a severe lack of funding. The many talented and able students who could become assets in the field of astronomy are missing out and if only they had the opportunity, they could really develop their capabilities and become excellent researchers and astronomers. In order to even stand a chance of making this happen, we need liaison with European established organisations that can deliver both expertise, funding and definitive, quantifiable schemes which will raise the expectations of these students as well as the universities. The ultimate goal is to put astronomy on the curriculum. The interest I have so far been able to generate amongst students is intense and I have been inspired by their enthusiasm, so the time is now right to develop and widen these activities in a more organised and proactive manner and this is where NoRCEL comes into force. Currently, NoRCEL is researching the possibility of setting up a virtual Science Education Institute which will be launched next year in conjunction with Professor Golden Gadzirayi Nyambuya of the National University of Science & Technology, Bulawayo, Zimbabwe.

The amino acid condensation reaction on a heterogeneous mineral surface has been regarded as one of the important pathways for peptide bond formation. Keeping this in view, we have studied the oligomerization of the simple amino acids, glycine and alanine, on nickel ferrite (NiFe2O4), cobalt ferrite (CoFe2O4), copper ferrite (CuFe2O4), zinc ferrite (ZnFe2O4), and manganese ferrite (MnFe2O4) nanoparticles surfaces, in the temperature range from 50–120 oC for 1–35 days, without applying any wetting/drying cycles. Among the metal ferrites tested for their catalytic activity, NiFe2O4 produced the highest yield of products by oligomerizing glycine to the trimer level and alanine to the dimer level, whereas MnFe2O4 was the least efficient catalyst, producing the lowest yield of products, as well as shorter oligomers of amino acids under the same set of experimental conditions. It produced primarily diketopiperazine (Ala) with a trace amount of alanine dimer from alanine condensation, while glycine was oligomerized to the dimer level. The trend in product formation is in accordance with the surface area of the minerals used. A temperature as low as 50 oC can even favour peptide bond formation in the present study, which is important in the sense that the condensation process is highly feasible without any sort of localized heat that may originate from volcanoes or hydrothermal vents. However, at a high temperature of 120 oC, anhydrides of glycine and alanine formation are favoured, while the optimum temperature for the highest yield of product formation was found to be 90 oC.

This is a report from NoRCELs Blue Earth Project symposium BEP2022 held online on January 8th, 2022. We are reporting the outcome pertaining to the following question: Is Humanity Settling its own Fate on Ecological Survival? A succinct conclusion drawn is that the Earth is facing the sixth mass extinction of flora and fauna; this being different from the previous five extinctions, in that it is entirely due to mankinds activities. Five invited eminent speakers delivered their input, highlighting the fact that there is extensive deterioration of the environment at large, coupled with an unprecedented demise of ecosystems leading to the extinction of species across the globe.

Is there life beyond Earth? An ideal research program would first ascertain how life on Earth began and then use this as a blueprint for its existence elsewhere. But the origin of life on Earth is still not understood, what then could be the way forward? Upcoming observations of terrestrial exoplanets provide a unique opportunity for answering this fundamental question through the study of other planetary systems. If we are able to see how physical and chemical environments similar to the early Earth evolve we open a window into our own Hadean eon, despite all information from this time being long lost from our planet’s geological record. A careful investigation of the chemistry expected on young exoplanets is therefore necessary, and the preparation of reference materials for spectroscopic observations is of paramount importance. In particular, the deduction of chemical markers identifying specific processes and features in exoplanetary environments, ideally “uniquely”. For instance, prebiotic feedstock molecules, in the form of aerosols and vapours, could be observed in transmission spectra in the near future whilst their surface deposits could be observed from reflectance spectra. The same detection methods also promise to identify particular intermediates of chemical and physical processes known to be prebiotically plausible. Is Ariel truly able to open a window to the past and answer questions concerning the origin of life on our planet and the universe? In this paper, we discuss aspects of prebiotic chemistry that will help in formulating future observational and data interpretation strategies for the Ariel mission. This paper is intended to open a discussion and motivate future detailed laboratory studies of prebiotic processes on young exoplanets and their chemical signatures.

In this paper the hypothesis that prions and prion-like molecules could have initiated the chemical evolutionary process which led to the eventual emergence of life is reappraised. The prions first hypothesis is a specific application of the protein-first hypothesis which asserts that protein-based chemical evolution preceded the evolution of genetic encoding processes. This genetics-first hypothesis asserts that an “RNA-world era” came before protein-based chemical evolution and rests on a singular premise that molecules such as RNA, acetyl-CoA, and NAD are relics of a long line of chemical evolutionary processes preceding the Last Universal Common Ancestor (LUCA). Nevertheless, we assert that prions and prion-like molecules may also be relics of chemical evolutionary processes preceding LUCA. To support this assertion is the observation that prions and prion-like molecules are involved in a plethora of activities in contemporary biology in both complex (eukaryotes) and primitive life forms. Furthermore, a literature survey reveals that small RNA virus genomes harbor information about prions (and amyloids). If, as has been presumed by proponents of the genetics-first hypotheses, small viruses were present during an RNA world era and were involved in some of the earliest evolutionary processes, this places prions and prion-like molecules potentially at the heart of the chemical evolutionary process whose eventual outcome was life. We deliberate on the case for prions and prion-like molecules as the frontier molecules at the dawn of evolution of living systems.

Methyl cyanide (CH3CN) is the simplest of the organic nitriles found in space. It was first identified in the molecular clouds, Sagittarius Sgr A and Sgr B in 1971, through its emission lines in the vicinity of 2.7 mm from the J = 6 ® 5 transition. In 1974 it was also reported in comet Kohoutek. CH3CN, has since been detected in the Hale Bopp comet and, as of 2009, there are no less than 58 hot molecular core objects in which CH3CN had been found. Methyl cyanide has also been discovered beyond the Milky Way galaxy, in the NGC 253 galax, which lies in the local group of galaxies, some 10 million light-years from Earth[1]. It has also been detected in the interstellar medium (ISM) where it is thought to be made on the grain mantles. Upon irradiation of the Irradiation of methyl cyanide (CH3CN) ice at 15 K with 200 keV Protons, we observed several compounds. Although this experiment was conducted under different conditions than comparable ones carried out by other researchers (eg Hudson and Moore 2004; Hudson, Moore et al. 2008), similar results were obtained. The objectives were to determine which molecules would form upon irradiation of CH3CN ice. The astrophysical ice of CH3CN is present in the ISM, comets, solar bodies (eg Titan) and other galaxies. These places receive radiation fluxes from levels of only a few eV to in excess of MeV cm-2 s-1, the result being that complex molecules are formed - eg HCN/CN-, HCCCN, H2C=C=NH and CH4. This experiment was carried out using 200 keV protons, and so replicated a particular radiation level similar to that present in space. It was discovered that, upon the irradiation of CH3CN under laboratory conditions, the same molecules as Hudson et al 2004 were formed. These molecules may then play an important role in the wider astrobiological context. For instance, HCN is vital in the formation of nitrogenous compound. Please insert your abstract HTML here.

It is believed that some of the necessary organic molecules may have been formed in specific areas of space (namely dark molecular clouds, eg Horsehead nebula) and delivered on to the Earth during the early heavy bombardment period of its history, approximately 4.3-4.0 billion years ago. These organic molecules may have played a pivotal role in the formation of life on Earth. In addition, it is believed that life on Earth was formed within a very short geological time frame of only 200-300 million years. So, it is not unreasonable to suppose that these molecules were initially made in space which in effect could be, metaphorically speaking, a huge chemical laboratory. The research (drawn from my own experimental astrochemistry) highlighted during this oral presentation focuses on the formation of molecules under a variety of simulated space conditions (eg different temperatures, levels of radiation energies and types of impinging radiations). There are two sorts of chemistry that take place in space, solid and gas phase, and although only 25% of the chemistry in space occurs in the solid phase, this will be the focus of my oral presentation.

Mars exploration motivates the search for extraterrestrial life, the development of space technologies, and the design of human missions and habitations. Here, we seek new insights and pose unresolved questions relating to the natural history of Mars, habitability, robotic and human exploration, planetary protection, and the impacts on human society. Key observations and findings include:–high escape rates of early Mars' atmosphere, including loss of water, impact present-day habitability;–putative fossils on Mars will likely be ambiguous biomarkers for life;–microbial contamination resulting from human habitation is unavoidable; and–based on Mars' current planetary protection category, robotic payload(s) should characterize the local martian environment for any life-forms prior to human habitation.Some of the outstanding questions are:–which interpretation of the hemispheric dichotomy of the planet is correct;–to what degree did deep-penetrating faults transport subsurface liquids to Mars' surface;–in what abundance are carbonates formed by atmospheric processes;–what properties of martian meteorites could be used to constrain their source locations;–the origin(s) of organic macromolecules;–was/is Mars inhabited;–how can missions designed to uncover microbial activity in the subsurface eliminate potential false positives caused by microbial contaminants from Earth;–how can we ensure that humans and microbes form a stable and benign biosphere; and–should humans relate to putative extraterrestrial life from a biocentric viewpoint (preservation of all biology), or anthropocentric viewpoint of expanding habitation of space?Studies of Mars' evolution can shed light on the habitability of extrasolar planets. In addition, Mars exploration can drive future policy developments and confirm (or put into question) the feasibility and/or extent of human habitability of space.

Modern terran life uses several essential biopolymers like nucleic acids, proteins and polysaccharides. The nucleic acids, DNA and RNA are arguably life’s most important, acting as the stores and translators of genetic information contained in their base sequences, which ultimately manifest themselves in the amino acid sequences of proteins. But just what is it about their structures; an aromatic heterocyclic base appended to a (five-atom ring) sugar-phosphate backbone that enables them to carry out these functions with such high fidelity? In the past three decades, leading chemists have created in their laboratories synthetic analogues of nucleic acids which differ from their natural counterparts in three key areas as follows: (a) replacement of the phosphate moiety with an uncharged analogue, (b) replacement of the pentose sugars ribose and deoxyribose with alternative acyclic, pentose and hexose derivatives and, finally, (c) replacement of the two heterocyclic base pairs adenine/thymine and guanine/cytosine with non-standard analogues that obey the Watson–Crick pairing rules. This manuscript will examine in detail the physical and chemical properties of these synthetic nucleic acid analogues, in particular on their abilities to serve as conveyors of genetic information. If life exists elsewhere in the universe, will it also use DNA and RNA?

It is increasingly likely that many non-communicable diseases of humans and associated animals are due to the degradation of their intestinal microbiomes, a situation often referred to as dysbiosis. An analysis of the resultant diseases offers an opportunity to probe the function of these microbial partners of multicellular animals. In our view, it now seems likely that vertebrate animals and their microbiomes have coevolved throughout the Ediacaran–Cambrian transition and beyond, operating by semiochemical messaging between the multicellular host and its microbial community guest. A consideration of the overall role of the mutualistic intestinal microbiome as an enclosed bioreactor throws up a variety of challenging concepts. In particular: the significance of the microbiome with respect to the immune system suggests that microeukaryotes could act as microbial sentinel cells; the ubiquity of bacteriophage viruses implies the rapid turnover of microbial composition by a viral-shunt mechanism; and high microbial diversity is needed to ensure that horizontal gene transfer allows valuable genetic functions to be expressed. We have previously postulated that microbes of sufficient diversity must be transferred from mother to infant by seemingly accidental contamination during the process of natural birth. We termed this maternal microbial inheritance and suggested that it operates alongside parental genetic inheritance to modify gene expression. In this way, the adjustment of the neonate immune system by the microbiome may represent one of the ways in which the genome of a vertebrate animal interacts with its microbial environment. The absence of such critical functions in the neonate may help to explain the observation of persistent immune-system problems in affected adults. Equally, granted that the survival of the guest microbiome depends on the viability of its host, one function of microbiome-generated semiochemicals could be to facilitate the movement of food through the digestive tract, effectively partitioning nutrition between host and guest. In the event of famine, downregulation of microbial growth and therefore of semiochemical production would allow all available food to be consumed by the host. Although it is often thought that non-communicable diseases, such as type 2 diabetes, are caused by consumption of food containing insufficient dietary fibre, our hypothesis suggests that poor-quality food is not the prime cause but that the tendency for disease follows the degradation of the intestinal microbiome, when fat build-up occurs because the relevant semiochemicals can no longer be produced. It is the purpose of this paper to highlight the possibility that the origins of the microbiome lie in the Precambrian and that the disconnection of body and microbiome gives rise to non-communicable disease through the loss of semiochemical signalling. We further surmise that this disconnect has been largely brought about by heavy metal poisoning, potentially illuminating a facet of the exposome, the sum total of environmental insults that influence the expression of the genetic inheritance of an animal.

The synthesis of prebiotic molecules from simple precursors is believed to be a crucial scheme in order to study the origin of life processes. The present study describes the one-pot synthesis of purine and pyrimidine nucleic acid bases in the presence of pre-biologically significant binary metal oxide nanoparticles, metal ferrites, namely NiFe2O4, CoFe2O4, CuFe2O4, ZnFe2O4 and MnFe2O4. The products identified are cytosine, isocytosine, 4(3H)-pyrimidinone, adenine, hypoxanthine and purine. The ability of isocytosine (a constitutional isomer of cytosine) to recognize cytosine and guanine through normal and reversed Watson-Crick pairing respectively, demonstrates an important storyline for the genesis of ancient nucleic acids. The relevance of other synthesized nucleic acid bases with respect to the origin of life is also discussed. The divalent metal ions in iron oxide make it an appropriate catalytic system because it demonstrates excellent catalytic performance for the nucleic acid bases synthesis with significantly high yield, as compared to pure iron oxide and some other minerals like silica, alumina, manganese oxides and double metal cyanide complexes.

Our paper briefly reviews the connection of the intestinal microbiome to the rise in non-communicable conditions related to atopic disease, obesity and mental health. We consider that the microbiome is best treated as if it were a single entity and have borrowed the terms semiochemical, allomone and kairomone (5) to describe interspecies relationship between the microbiome and ourselves (Fig. 1). We use the term dysbiosis to describe the breakdown of these relationships leading to disease (Fig. 2). As a result of this analysis we tentatively suggest that components of the microbiome assess microbial antigens in our food and pass this information back to our immune system via as yet undescribed chemical messengers: kairomones. We call these hypothetical microbial agents Sentinel Cells. Our suggestion is that atopic disease arises partly as a result of consuming processed food that has insufficient antigens to activate this kairomone feedback mechanism, which atrophies as a result. We note that this is potentially similar to the Old Friends concept of Rook and his co-workers (16). We suggest that obesity is a consequence of dysbiosis-induced waning of the output of allomone-like psychotropic compounds (including the known microbial metabolites dopamine and serotonin) leading to the weakening of the gut-brain axis and a negative effect on mental health. Although dysbiosis can occur in other ways, including antibiotic use and sterile caesarian section, we believe that all these problems can be overcome to provide a future free of these non-communicable diseases.

We re-evaluate research relating to the current theories of the emergence of biological systems. The challenge being that research programmes concerning the emergence of these systems are viewed as the same as those relating to the origin of cells. Cells are strikingly important biological entities, hard wired into the entire field of biology. The development of biological systems took place much earlier than the origin of cells and even before the existence of the Last Universal Common Ancestor (LUCA); a period which could be construed as being preLUCA and which would have taken place during in a ribonucleoprotein world. This latter entity was named FUCA (First Universal Common Ancestor) and could be viewed as a "great-grandmother" to LUCA, from which the three domains of life, namely Archaea, Bacteria, and Eukarya (emerging as a chimera of the two) evolved. RNA-world theories are the focus of mainstream research programmes for the origin of life stricto sensu. In the RNA-world view, self-replication of nucleic acids is seen as one of the most relevant events in the pre-biotic world. Without denying the relevance of self-replication, we argue here that the most germane event which occurred in the pre-biotic world was the crosstalk between nucleic acids and peptides. When these two macromolecules started to interact, the singularity that aggregated the complexity required to produce life began to emerge. Thus, comprehension of the early origins of the translation machinery and the assembly of the genetic code is key. Therefore, the relevance of cell theory and self-replication should be re-evaluated as well as the concept of life itself.

Our Sun is approximately 5 billion years old and the Universe is 14 billion years old, which leaves more than 9 billion years between the Big Bang and the emergence of life on Earth. Here we ask, “are we the first, or has life emerged numerous times in many places elsewhere in the Universe prior to the formation of our Solar System and the subsequent emergence of life on Earth?” Since we have experience of only one life, we need to work with the “tools” which we currently have access to—e.g., deeper knowledge of chemistry. In this chapter, we postulate that life could possibly also be a widespread phenomenon in the Universe, by investigating and unraveling the physical and chemical mechanisms that led to the origins of life on Earth and correlating these with ongoing discoveries in space (e.g., the formation of organic molecules). We consider the formation of the complex organic molecules required for life in the interstellar medium, which is one of the factors affecting the eventual emergence of life. We analyzed various hypotheses that may help to explain the origins of life on Earth and the possibility of life elsewhere in our Solar System (e.g., Enceladus). In addition, the role of genetics, viruses, and extremophiles is examined before coming to a probabilistic conclusion.

SnCl4 or TiCl4 catalysts provided a rapid and efficient detetrahydropyranylation and demethoxymethylation of phenolic ethers and a sequential one-pot intramolecular Friedel–Crafts alkylation of chalcone epoxides under mild reaction conditions. The reaction took 2–3 min to give the phenols and 1-indanones in an excellent yield (90–98%) at 0 °C without affecting other functional groups. With these catalysts, our protocol gave regioselective products as trans-3-aryl-2-hydroxy-1-indanones in an excellent yield (76–98%) and an enantiomeric excess of up to 99.9% under the same conditions.

The amino acid condensation reaction on a heterogeneous mineral surface has been regarded as one of the important pathways for peptide bond formation. Keeping this in view, we have studied the oligomerization of the simple amino acids, glycine and alanine, on nickel ferrite (NiFe2O4), cobalt ferrite (CoFe2O4), copper ferrite (CuFe2O4), zinc ferrite (ZnFe2O4), and manganese ferrite (MnFe2O4) nanoparticles surfaces, in the temperature range from 50–120 °C for 1–35 days, without applying any wetting/drying cycles. Among the metal ferrites tested for their catalytic activity, NiFe2O4 produced the highest yield of products by oligomerizing glycine to the trimer level and alanine to the dimer level, whereas MnFe2O4 was the least efficient catalyst, producing the lowest yield of products, as well as shorter oligomers of amino acids under the same set of experimental conditions. It produced primarily diketopiperazine (Ala) with a trace amount of alanine dimer from alanine condensation, while glycine was oligomerized to the dimer level. The trend in product formation is in accordance with the surface area of the minerals used. A temperature as low as 50 °C can even favor peptide bond formation in the present study, which is important in the sense that the condensation process is highly feasible without any sort of localized heat that may originate from volcanoes or hydrothermal vents. However, at a high temperature of 120 °C, anhydrides of glycine and alanine formation are favored, while the optimum temperature for the highest yield of product formation was found to be 90 °C.

The commissioning of the ALMA array and the next generation of space telescopes heralds the dawn of a new age of Astronomy, in which the role of chemistry in the interstellar medium and in star and planet formation may be quantified. A vital part of these studies will be to determine the molecular complexity in these seemingly hostile regions and explore how molecules are synthesised and survive. The current hypothesis is that many of these species are formed within the ice mantles on interstellar dust grains with irradiation by UV light or cosmic rays stimulating chemical reactions. However, such irradiation releases many secondary electrons which may themselves induce chemistry. In this article we discuss the potential role of such electron induced chemistry and demonstrate, through some simple experiments, the rich molecular synthesis that this may lead to.

This research work investigates the possibility of shielding gravity. The ultimate purpose of this work is to understand the reality behind the concept of Gravitational Shielding (GS) and time dilation. Since the 19th century, scientists have tried to arrive at an understanding of GS via the use of various experiments. Unfortunately, some experiments failed to prove the existence of gravitational shielding, whereas some results proclaimed the possibility of attaining GS. The original phenomenon exhibited by nature cannot easily be understood, but some experiments have demonstrated that the answer may lie behind the mysterious GS. If GS is proved, then in the future, it would be possible to travel across black holes by defying gravity or through any bigger mass having high gravitational field. To unravel the mystery of GS, this work investigates the history of GS and considers the future vision of technologically advanced spacecraft or other warp drive mechanisms with appropriate gravitational shielding. Though the problem is very complex, this research work tries to come to a deeper understanding and explanation of the complexity involved in achieving gravitational shielding.

This paper summarises the oral presentations, their outcomes and conclusions drawn from the meeting entitled: ‘Horizontal Gene transfer and the Last Universal Common Ancestor’ which was held at the Open University, Milton Keynes, UK, on the 5th and the 6th September 2013.

Currently there are five known mechanisms of horizontal gene transfer (HGT): transduction, conjugation, transformation, gene transfer agents and membrane vesicle transfer. The question here is: what part did HGT play in the reorganisation of genetics during the last universal common ancestor (LUCA) epoch? LUCA is a construct to explain the origin of the three domains of life; namely Archaea, Bacteria and Eukarya. This editorial offers a general introduction to the relevance and ultimate significance of HGT in relation to the LUCA. [...].

This paper seeks to review the likelihood of unearthing evidence of the existence of life elsewhere in the Universe. Although it has been demonstrated that life can thrive in the severest of conditions on Earth, detecting its presence in similarly habitable zones elsewhere is proving to be an extremely complex issue. There are many reasons for this, the major ones being that the distances involved are vast; the low potential signal to noise ratio, spatial and spectral resolutions arising from planets with biospheres; and biosignals themselves can be misleading. New telescopes with improved technology are on the horizon which will extend our capabilities, but it is still doubtful that any exploration could venture beyond the borders of our galaxy. Moreover, caution needs to be exercised when assessing the signals emitted by biomarkers as these could be produced abiotically. However, if the focus of the search should be concentrated around the area of M dwarf stars then, as we begin to understand the nature of habitable zones, our chances of eventually achieving our goals will be enhanced.

The results of an experimental investigation of 1 keV electron irradiation of ices (deposited at 30 K) of (i) pure methanol and (ii) of a 1:1 mixture of NH3:CH3OH are reported. Molecular products formed within the ice were detected and monitored using FTIR spectroscopy. The products observed were methyl formate (H3COHCO), methane (CH4), hydroxymethyl (CH2OH), formamide (HCONH2), formic acid (HCOOH), formaldehyde (H2CO), formyl radical (HCO), cyanate ion (OCN−), isocyanic acid (HNCO), carbon monoxide (CO) and carbon dioxide (CO2). The consequences of these results for prebiotic chemistry in the interstellar medium and star forming regions are discussed.

In this Letter the results of an experimental investigation of 1 keV electron irradiation of a 1:1 ice mixture of NH3:CO2 at 30 K was made under ultrahigh vacuum (10(-9) mbar) conditions. Molecular products formed within the ice were detected and monitored using FTIR spectroscopy. The formation of ammonium ions (NH4+), cyanate ions (OCN-), CO was observed leading to the synthesis of ammonium carbamate (NH4NH2CO2). The consequences of these results for prebiotic chemistry in the interstellar medium and star forming regions are discussed. Crown Copyright (C) 2012 Published by Elsevier B.V. All rights reserved.

We report the results of chemical processing induced by 1 keV electron irradiation of a solid N2O ice sample formed at 25 K. Ozone and several oxides of nitrogen (NO2, N2O2, N2O3, N2O4 and N2O5) were observed to form during the irradiation period. Such reactions have important implications for the ice chemistry of outer solar system planets/satellites and interstellar ices.

SnCl4 or TiCl4 catalysts provided a rapid and efficient detetrahydropyranylation and demethoxymethylation of phenolic ethers and a sequential one-pot intramolecular Friedel–Crafts alkylation of chalcone epoxides under mild reaction conditions. The reaction took 2–3 min to give the phenols and 1-indanones in an excellent yield (90–98%) at 0 °C without affecting other functional groups. With these catalysts, our protocol gave regioselective products as trans-3-aryl-2-hydroxy-1-indanones in an excellent yield (76–98%) and an enantiomeric excess of up to 99.9% under the same conditions.

This paper reports on the various nuances of the origins of life on Earth and highlights the latest findings in that arena as reported at the Network of Researchers on Horizontal Gene Transfer and the Last Universal Common Ancestor (NoR HGT and LUCA) which was held from the 3–4th November 2016 at the Open University, UK. Although the answers to the question of the origin of life on Earth will not be fathomable anytime soon, a wide variety of subject matter was able to be covered, ranging from examining what constitutes a LUCA, looking at viral connections and “from RNA to DNA”, i.e., could DNA have been formed simultaneously with RNA, rather than RNA first and then describing the emergence of DNA from RNA. Also discussed are proteins and the origins of genomes as well as various ideas that purport to explain the origin of life here on Earth and potentially further afield elsewhere on other planets.

Planets and their moons are constantly subjected to irradiation from both their respective planetary magnetospheres and the solar wind. Energetic particles (electrons, protons and ions) in such radiation may induce complex chemistry within the icy mantles of such bodies, producing many organic compounds. Such processes can be simulated in laboratory experiments. In this report we present recent results from experiments exploring both molecular synthesis and the morphology of such ices.The morphology of any ice may be characterised by IR and Vacuum Ultra-Violet (VUV) spectroscopy. The latter is particularly useful for studying ices in which infrared inactive molecules like oxygen (O2) are common. We have shown that oxygen forms dimers in typical planetary ices and that, in contrast to previous analysis, many of the chemical reactions within the ice involve such dimer (and larger cluster) chemistry. We also present the results of a series of experiments that explore electron, proton and ion irradiation on Solar System relevant ices such as carbon dioxide (CO2) at different temperatures. Infrared spectra recorded before and after irradiation are used to identify and quantify molecules formed in such irradiation, e. g. ozone. These experiments show that the morphology of the ice plays a critical role in the chemistry.