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At least 1,153 records · Page 64Linked to original sources
PubMed1995

Very low temperature formaldehyde reactions and the build-up of organic molecules in comets and interstellar ices.

We have investigated thermally promoted reactions of formaldehyde (H2CO) in very low temperature ices. No such reactions occurred in ices of pure formaldehyde. However, addition of trace amounts of ammonia (NH3) were sufficient to catalyze reactions at temperatures as low as 40 K. Similar reactions could take place in interstellar ices and in Comets and produce considerable amounts of organic molecules.

Ammonia↗
PubMed1995

Carbonaceous matter in cometary dust and coma.

The analysis of carbonaceous matter in p/Halley's dust and coma via mass spectrometry of positive ions is reviewed. Dust impact generated ions were analyzed by the PUMA instrument aboard VEGA I, and coma plasma ions by the PICCA instrument aboard GIOTTO. For the organic molecules results an overall C:H:O:N ratio of 1.:1.4:0.6:0.1. Most of this polymer material can formally be understood as an aggregation of monomers C2H2, CH2O, and HCN. Special emphasis is given to possible aromatic, especially heterocyclic, and other unsaturated ions, and their importance for abiotic chemical and prebiotic evolution. Aspects of the potential heterogeneous catalysis in liquid water at the inorganic grain backbone structure found by this analysis, too, are also treated.

Acetylene↗
PubMed1995

Polycyclic aromatic hydrocarbon ions and the diffuse interstellar bands.

Neutral naphthalene (C10H8), phenanthrene (C14H10), and pyrene (C16H10) absorb strongly in the ultraviolet and may contribute to the extinction curve. High abundances are required to produce detectable structures. The cations of these PAHs absorb in the visible. C10H8+ has 12 discrete absorption bands which fall between 6800 and 5000 angstroms. The strongest band at 6741 angstroms falls close to the weak 6742 angstroms diffuse interstellar band (DIB). Five other weaker bands also match DIBs. The possibility that C10H8+ is responsible for some of the DIBs can be tested by searching for new DIBs at 6520, 6151, and 5965 angstroms, other moderately strong naphthalene cation band positions. If C10H8+ is indeed responsible for the 6742 angstroms feature, it accounts for 0.3% of the cosmic carbon. The spectrum of C16H10+ is dominated by a strong band at 4435 angstroms in an Ar matrix and 4395 angstroms in a Ne matrix, a position which falls very close to the strongest DIB, that at 4430 angstroms. If C16H10+, or a closely related pyrene-like ion is indeed responsible for the 4430 angstroms feature, it accounts for 0.2% of the cosmic carbon. We also report an intense, very broad UV-to-visible continuum which is associated with both ions and could explain how PAHs convert interstellar UV and visible radiation into IR.

Argon↗
PubMed1995

Isotopic ratios in planetary atmospheres.

Recent progress on measurements of isotopic ratios in planetary or satellite atmospheres include measurements of the D/H ratio in the methane of Uranus, Neptune and Titan and in the water of Mars and Venus. Implications of these measurements on our understanding of the formation and evolution of the planets and satellite are discussed. Our current knowledge of the carbon, nitrogen and oxygen isotopic ratios in the atmospheres of these planets, as well as on Jupiter and Saturn, is also reviewed. We finally show what progress can be expected in the very near future due to some new ground-based instrumentation particularly well suited to such studies, and to forthcoming space missions.

Atmosphere↗
PubMed2003

Control of metabolic energy by space systems. Part 1: theoretical reports of space flow structure and function.

In past papers, a notion emerged that space had elements common to the energy of atomic shells to which it could flow by paths to control metabolic energy of animate systems. This paper examines several authors on the structure and function of space energy wave bundle flows seeking mechanisms for metabolic control. The application of time to these waves provides two compartments, time symmetric and time asymmetric, respectively imaginary and real, in a sensitively balanced state as part of a specific system from space to orbits. Disturbance to the balance, where minimal, results in a reflection outside the system to the heat bath consistent with physiology. Arbitrarily more than minimal, results in pathology. A black-hole-like monitor maintains the balance in alliance with a multi-system space stream, the meridian of traditional Chinese medicine. This macroscopic state is now consistent with manipulation using conventional electronics, by way of remedy.

Animals↗
PubMed2003

Control of metabolic energy by space systems. Part 2: possible distribution at metabolic cycle chemicals.

Assimilation of many concepts and observations on an energy force providing a control over metabolic chemical interaction with a force in space itself is possible. The force is assumed to integrate with the atomic orbits of the metabolic chemicals, leaving its path from space as a fluctuation for realisation of two components, a non-linear space-rich part and a linear space-poor part. The pair are associated by a balance leading to non-linear behaviour imposed upon an otherwise linear output of the orbital energy and the actual control is vested in the balance. Examples are cited for the integration of the fluctuation during protein and nucleoprotein function and for cyto-structural mechanisms which may allow a selection of space elements to provide for evolution of unique family elements for enhanced control, much as the optical physicists have selected squeezed light elements for refined quantal function. Methods for rational therapies emerge from these refinements.

Animals↗
PubMed1996

Pros and cons in the search for extraterrestrial intelligence.

I propose a new term, 'galactic organism with distinct intelligence', for the extraterrestrial forms, with which humans can make contact. This is because, among the three existing terms: (a) 'the search for extraterrestrial intelligence' 'excludes biology and is inelegant'; (b) 'extraterrestrial' does not distinguish between the micro-organisms and highly-evolved intelligent life-forms; and (c) 'unidentified flying object' projects a sense of mysticism. On the presence of galactic organisms with distinct intelligence, scientists belong to three camps. Astronomers, physicists and some biochemists belong to the believers group. Evolutionists are in the doubters category. The third camp is represented by the 'uncommitted'. Approaches for contacting galactic organisms with distinct intelligence would take three steps. These are: (a) radioastronomical observations in the galaxy and interstellar space for the presence of organic matter; (b) initiating radio contact and listening to any transmitted message, as set out by the search for extraterrestrial intelligence program, and (c) landing instruments and humans in the galaxy.

Astronomical Phenomena↗
PubMed2001

Our life is protected by the Earth's atmosphere and magnetic field: what aurora research tells us.

Our sun is an average middle-aged star. Without the sun, there would be no atmosphere, no water, and no life on the Earth. The sun is constantly changing, providing the Earth with energy through a complicated chain of processes that occur in space surrounding the Earth. This paper demonstrates that life on Earth is protected by two barriers, i.e., the atmosphere and the magnetic field, against otherwise menacing events in space. Because of these shielding effects, we, peacefully sitting on the Earth's surface, are not aware of a number of critical and potentially dangerous episodes that are taking place only 100 km above the Earth's surface. The aurora, which dances in the polar sky also because of the two barriers, is sending us a crucial hint about what is happening in space.

Animals↗
PubMed2003

Astrobiology, the transcendent science: the promise of astrobiology as an integrative approach for science and engineering education and research.

Astrobiology is rapidly gaining the worldwide attention of scientists, engineers and the public. Astrobiology's captivation is due to its inherently interesting focus on life, its origins and distribution in the Universe. Because of its remarkable breadth as a scientific field, astrobiology touches on virtually all disciplines in the physical, biological and social sciences as well as engineering. The multidisciplinary nature and the appeal of its subject matter make astrobiology ideal for integrating the teaching of science at all levels in educational curricula. The rationale for implementing novel educational programs in astrobiology is presented along with specific research and educational policy recommendations.

Biological Evolution↗
PubMed2003

Termolecular ion-molecule reactions in Titan's atmosphere. IV. A search made at up to 1 micron in pure hydrocarbons.

The results of a study of ion-molecule reactions occurring in pure methane, acetylene, ethylene, ethane, propyne, propene, propane, and diacetylene at pressures up to 40 microns of pressure are reported. A variety of experimental methods are used: The standard double resonance in an ICR, for determination of the precursor ions and the modulated double resonance ejection in an ICR, for the determination of the daughter ions. The FA-SIFT technique was used for validation and examination of termolecular reactions with rate coefficients that are less than 10(-26) cm(6) s(-1). An extensive database of reaction kinetics already exists for many of these reactions. The main point of this study was the determination of the accuracy of this database and to search for any missing reactions and reaction channels that may have been omitted from earlier investigations. A specific objective of this work was to extend the study to the highest pressures possible to find out if there were any important termolecular reaction channels occurring. A new approach was used here. In the pure hydrocarbon gases the mass spectra were followed as a function of the pressure changes of the gas. An initial guess was first made using the current literature as a source of the reaction kinetics that were expected. A model of the ion abundances was produced from the solution of the partial differential equations in terms of reaction rate coefficients and initial abundances. The experimental data was fitted to the model for all of the pressures by a least squares minimization to the reaction rate coefficients and initial abundances. The reaction rate coefficients obtained from the model were then compared to the literature values. Several new channels and reactions were discovered when the modeled fits were compared to the actual data. This is all explained in the text and the implications of these results are discussed for the Titan atmosphere.

Atmosphere↗
PubMed2003

Formation of neutral molecules of potential stellar interest by neutralisation of negative ions in a mass spectrometer. The application of experiment and molecular modelling in concert.

This paper is a modified version of a lecture which describes the synthesis, structure and reactivity of some neutral molecules of stellar significance. The neutrals are formed in the collision cell of a mass spectrometer following vertical Franck-Condon one electron oxidation of anions of known bond connectivity. Neutrals are characterised by conversion to positive ions and by extensive theoretical studies at the CCSD(T)/aug-cc-pVDZ//B3LYP/6-31G(d) level of theory. Four systems are considered in detail, viz (i) the formation of linear C(4) and its conversion to the rhombus C(4), (ii) linear C(5) and the atom scrambling of this system when energised, (iii) the stable cumulene oxide CCCCCO, and (iv) the elusive species O(2)C-CO. This paper is not intended to be a review of interstellar chemistry: examples are selected from our own work in this area.

Astronomical Phenomena↗
PubMed2001

Radiation dose from reentrant electrons.

In estimating the crew exposures during an extra vehicular activity (EVA), the contribution of reentrant electrons has always been neglected. Although the flux of these electrons is small compared to the flux of trapped electrons, their energy spectrum extends to several GeV compared to about 7 MeV for trapped electrons. This is also true of splash electrons. Using the measured reentrant electron energy spectra, it is shown that the dose contribution of these electrons to the blood forming organs (BFO) is more that 10 times greater than that from the trapped electrons. The calculations also show that the dose-depth response is a very slowly changing function of depth, and thus adding reasonable amounts of additional shielding would not significantly lower the dose to BFO.

Aerospace Medicine↗
PubMed2001

Development of personal neutron dosemeters at the PTB and first measurements in the space station MIR.

A passive neutron dosemeter with thermoluminescence and etched-track detectors was used in the space station MIR in 1995 and 1997 and during some shuttle flights to MIR. High neutron doses of about 200 microSv d-1 were measured with track detectors, while the contribution of protons to the track density was estimated to be small. An active personal dosemeter based on silicon diodes providing a direct readout, improved sensitivity and spectrometric properties is proposed for additional monitoring. Firstly, measurements with a prototype were performed in the stray radiation fields of the CERN-EU Reference Radiation Facility. When mounted on a phantom at different positions, both the passive and the active dosemeter provide the directional distribution of neutrons via an unfolding procedure. This can be helpful for a better understanding of the complex radiation field in space and for comparisons with calculations.

Calibration↗
PubMed2001

Neutron measurements using bubble detectors--terrestrial and space.

Like all other radiation monitors currently used in the space program, the bubble detector (which has flown on several missions) was adapted from a technology that was developed for terrestrial radiation. Bubble detectors are the most recent technology for applications in personal neutron dosimetry. They are now regarded as a mature technology and are used in many countries as a neutron dosimeter of record with approval from the respective regulatory authorities. Extensive type testing and QA of bubble detectors has been done by numerous groups, many of these to show that bubble detectors meet national radiation protection requirements prior to their acceptance as a dosimeter of record. In fact, it has been stated "Only bubble detectors achieve a sufficiently low detection threshold (to meet ICRP-60 recommendations)..." (Portal and Dietze, 1992).

Calibration↗
PubMed2001

Russian measurements of neutron energy spectra on the Mir orbital station.

Results of the experiments on neutron energy spectra measurements within broad energy range from 5 x 10(-7) to 2 x 10(2) MeV aboard the Mir orbital station and equivalent neutron dose estimation are presented. Four measurement techniques were used during the experiments. The shape of spectra and their absolute values are in good agreement. According to those experiments, an equivalent neutron dose depends upon effective shielding thickness and spacecraft mass. The neutron dose mentioned is comparable with that of ionizing radiation. Neutron flux levels measured aboard the Mir station have shown that a neutron spectrometer involving broad energy range will be used within the radiation monitoring systems in manned space flights.

Extraterrestrial Environment↗
PubMed2001

Energy spectra of HZE-particles inside the International Space Station.

To measure the energy spectra of low energy ions inside the International Space Station (ISS) we will expose three stacks of CR-39 plastic nuclear track detectors aligned to the three coordinate axes of the space station. The energies of cosmic ray nuclei at the stack surfaces can be determined by reconstructing the trajectories of ions stopping inside the detector material and by measuring their ranges. To measure only HZE (high charge Z and energy E) ions with charges of Z6 stopping in our experiment a special batch of CR-39 detectors with low sensitivity will be used. This detector material has been already tested by an exposure to carbon ions at the GSI accelerator in Darmstadt, Germany.

Carbon↗
PubMed2001

The cosmic ray actinide charge spectrum derived from a 10 m2 array of solid state nuclear track detectors in Earth orbit.

The DIAS-ESTEC Ultra Heavy Cosmic Ray Experiment (UHCRE) on the Long Duration Exposure Facility, collected approximately 3000 cosmic ray nuclei with Z > 65 in the energy region E > 1.5 GeV nucleon-1 during a six year exposure in Earth orbit. The entire accessible collecting area of the solid state nuclear track detector (SSNTD) array has been scanned for actinides, yielding a sample of 30 from an exposure of approximately 150 m2 sr yr. The UHCRE experimental setup is described and the observed charge spectrum presented. The current best value for the cosmic ray actinide relative abundance, (Z > 88)/(74 < or = Z < or = 87), is reported.

Actinoid Series Elements↗
PubMed2001

Anomalous cosmic ray carbon and oxygen tracks in CN-Kodak.

For observation of low energy cosmic ray particles we used CN-Kodak nuclear track detectors on Cosmos satellites. In solar quiet periods during solar minima conditions the detectors registered anomalous cosmic rays (ACRs). The ACRs are characterized by flux enhancements of several elements and it is known that the carbon enhancement is small compared with that of oxygen. In all of our quiet-time exposures the relation between carbon and oxygen was extremely small (C/O ~ 0.03). But in two quiet-time periods of 14.03.96-11.06.96 and of 15.12.97-14.04.98 we have identified many tracks as carbon in a L-R diagram. As a result the observed C/O ratio appears to be more than 0.5, whereas other experiments show no evidence of enhanced flux of carbon during these periods. The reason for the unexpected response of CN-Kodak is discussed.

Carbon↗