A colorimetric method for the glucosamine (GlcN) assay was applied for the determination of chitin, which can be hydrolyzed to produce GlcN. A 10-mg sample was mixed with 10 mL of a 5 mol/L HCl ...aqueous solution, and the mixture was kept at 100°C for 12 h. Under these conditions, chitin was completely depolymerized and deacetylated to produce GlcN, even when the sample was a crab shell. A 20-μL aliquot of the hydrolysate was mixed with 20 μL of a 5 mol/L NaOH aqueous solution and 200 μL of a 50 mmol/L Na2SiO3, 600 mmol/L Na2MoO4, 1.5 mol/L CH3COOH and 30% (v/v) dimethyl sulfoxide solution. The mixture was kept at 70°C for 30 min. In the mixture, GlcN reduced the Mo(VI) species to form a blue molybdosilicate anion, which gave an absorbance maximum at around 750 nm. Since N-acetylglucosamine and chitin oligosaccharides could not render the reaction mixture blue, GlcN in the hydrolysate could be assayed colorimetrically with high selectivity. When a standard chitin sample was examined, the GlcN concentration in the hydrolysate was determined to be 0.97 ± 0.02 g/L (as hydrochloride salt), indicating that the sample contained 10.0 ± 0.2 mg chitin (as an N-acetylglucosamine homopolymer). Calcium cation, amino acids, and proteins did not interfere with the GlcN assay. Thus, the proposed method was successfully applied to determine chitin in a crab shell sample.
Mercury has a unique and complex space environment with its weak global magnetic field, intense solar wind, tenuous exosphere, and magnetospheric plasma particles. This complex system makes Mercury ...an excellent science target to understand effects of the solar wind to planetary environments. In addition, investigating Mercury’s dynamic magnetosphere also plays a key role to understand extreme exoplanetary environment and its habitability conditions against strong stellar winds. BepiColombo, a joint mission to Mercury by the European Space Agency and Japan Aerospace Exploration Agency, will address remaining open questions using two spacecraft, Mio and the Mercury Planetary Orbiter. Mio is a spin-stabilized spacecraft designed to investigate Mercury’s space environment, with a powerful suite of plasma instruments, a spectral imager for the exosphere, and a dust monitor. Because of strong constraints on operations during its orbiting phase around Mercury, sophisticated observation and downlink plans are required in order to maximize science outputs. This paper gives an overview of the Mio spacecraft and its mission, operations plan, and data handling and archiving.
An artificial impact experiment is scheduled for 2018–2019 in which an impactor will collide with asteroid 162137 Ryugu (1999
JU
3
) during the asteroid rendezvous phase of the Hayabusa2 spacecraft. ...The small carry-on impactor (SCI) will shoot a 2-kg projectile at 2 km/s to create a crater 1–10 m in diameter with an expected subsequent ejecta curtain of a 100-m scale on an ideal sandy surface. A miniaturized deployable camera (DCAM3) unit will separate from the spacecraft at about 1 km from impact, and simultaneously conduct optical observations of the experiment. We designed and developed a camera system (DCAM3-D) in the DCAM3, specialized for scientific observations of impact phenomenon, in order to clarify the subsurface structure, construct theories of impact applicable in a microgravity environment, and identify the impact point on the asteroid. The DCAM3-D system consists of a miniaturized camera with a wide-angle and high-focusing performance, high-speed radio communication devices, and control units with large data storage on both the DCAM3 unit and the spacecraft. These components were successfully developed under severe constraints of size, mass and power, and the whole DCAM3-D system has passed all tests verifying functions, performance, and environmental tolerance. Results indicated sufficient potential to conduct the scientific observations during the SCI impact experiment. An operation plan was carefully considered along with the configuration and a time schedule of the impact experiment, and pre-programed into the control unit before the launch. In this paper, we describe details of the system design concept, specifications, and the operating plan of the DCAM3-D system, focusing on the feasibility of scientific observations.
BepiColombo Mio, also known as the Mercury Magnetospheric Orbiter (MMO), is intended to conduct the first detailed study of the magnetic field and environment of the innermost planet, Mercury, ...alongside the Mercury Planetary Orbiter (MPO). This orbiter has five payload groups; the MaGnetic Field Investigation (MGF), the Mercury Plasma Particle Experiment (MPPE), the Plasma Wave Investigation (PWI), the Mercury Sodium Atmosphere Spectral Imager (MSASI), and the Mercury Dust Monitor (MDM). These payloads operate through the Mission Data Processor (MDP) that acts as an integrated system for Hermean environmental studies by the
in situ
observation of charged and energetic neutral particles, magnetic and electric fields, plasma waves, dust, and the remote sensing of radio waves and exospheric emissions. The MDP produces three kinds of coordinated data sets: Survey (L) mode for continuous monitoring, Nominal (M) mode for standard analyses of several hours in length (or more), and Burst (H) mode for analysis based on 4–20-min-interval datasets with the highest cadence. To utilize the limited telemetry bandwidth, nominal- and burst-mode data sets are partially downlinked after selections of data based on L- or L/M-mode data, respectively. Burst-mode data can be taken at preset timings, or by onboard automatic triggering. The MDP functions are implemented and tested on the ground as well as cruising spacecraft; they are responsible for conducting full scientific operations aboard spacecraft.
MAP-PACE (MAgnetic field and Plasma experiment—Plasma energy Angle and Composition Experiment) on SELENE (Kaguya) has completed its ∼1.5-year observation of low-energy charged particles around the ...Moon. MAP-PACE consists of 4 sensors: ESA (Electron Spectrum Analyzer)-S1, ESA-S2, IMA (Ion Mass Analyzer), and IEA (Ion Energy Analyzer). ESA-S1 and S2 measured the distribution function of low-energy electrons in the energy range 6 eV–9 keV and 9 eV–16 keV, respectively. IMA and IEA measured the distribution function of low-energy ions in the energy ranges 7 eV/q–28 keV/q and 7 eV/q–29 keV/q. All the sensors performed quite well as expected from the laboratory experiment carried out before launch. Since each sensor has a hemispherical field of view, two electron sensors and two ion sensors installed on the spacecraft panels opposite each other could cover the full 3-dimensional phase space of low-energy electrons and ions. One of the ion sensors IMA is an energy mass spectrometer. IMA measured mass-specific ion energy spectra that have never before been obtained at a 100 km altitude polar orbit around the Moon. The newly observed data show characteristic ion populations around the Moon. Besides the solar wind, MAP-PACE-IMA found four clearly distinguishable ion populations on the dayside of the Moon: (1) Solar wind protons backscattered at the lunar surface, (2) Solar wind protons reflected by magnetic anomalies on the lunar surface, (3) Reflected/backscattered protons picked-up by the solar wind, and (4) Ions originating from the lunar surface/lunar exosphere.
The 3‐D velocity distribution functions of nonthermal ions observed in the vicinity of the Moon have been analyzed to understand the interaction between the solar wind and the Moon. The observation ...was made during the lunar swing‐by of the Nozomi spacecraft, and the closest approach was about 1.6 RL from the Moon's surface. Both Nozomi and the Moon were located in the solar wind, and nonthermal ions were observed only when the spacecraft was very close to the Moon. The nonthermal ions were measured by a Particle Spectrum Analyzer/Ion Spectrum Analyzer (PSA/ISA) on board the Nozomi. After analyses and careful examination of the 3‐D velocity distribution of the nonthermal ions, the characteristics of the nonthermal ions were revealed as follows: The nonthermal ions have a partial ring structure in the phase space, they are protons, their source location is the dayside of the Moon, and they have large velocities when they are generated. We propose the following scenario of a solar wind interaction with the Moon: The electromagnetic field in the vicinity of the Moon must have a dynamic structure, possibly a miniature bow shock associated with a local magnetic anomaly, where some of the solar wind protons are deflected violating their first adiabatic invariant. After the deflection, they move under the force of the convection electric field and gyrate around the magnetic field in the solar wind. This motion forms a partial ring structure with large initial velocities in the velocity phase space.
The modified mevalonate pathway is believed to be the upstream biosynthetic route for isoprenoids in general archaea. The partially identified pathway has been proposed to explain a mystery ...surrounding the lack of phosphomevalonate kinase and diphosphomevalonate decarboxylase by the discovery of a conserved enzyme, isopentenyl phosphate kinase. Phosphomevalonate decarboxylase was considered to be the missing link that would fill the vacancy in the pathway between mevalonate 5-phosphate and isopentenyl phosphate. This enzyme was recently discovered from haloarchaea and certain Chroloflexi bacteria, but their enzymes are close homologs of diphosphomevalonate decarboxylase, which are absent in most archaea. In this study, we used comparative genomic analysis to find two enzymes from a hyperthermophilic archaeon, Aeropyrum pernix, that can replace phosphomevalonate decarboxylase. One enzyme, which has been annotated as putative aconitase, catalyzes the dehydration of mevalonate 5-phosphate to form a previously unknown intermediate, trans-anhydromevalonate 5-phosphate. Then, another enzyme belonging to the UbiD-decarboxylase family, which likely requires a UbiX-like partner, converts the intermediate into isopentenyl phosphate. Their activities were confirmed by in vitro assay with recombinant enzymes and were also detected in cell-free extract from A. pernix. These data distinguish the modified mevalonate pathway of A. pernix and likely, of the majority of archaea from all known mevalonate pathways, such as the eukaryote-type classical pathway, the haloarchaea-type modified pathway, and another modified pathway recently discovered from Thermoplasma acidophilum.
Most visible matter in the Universe exists as plasma. How this plasma is heated, and especially how the initial non-equilibrium plasma distributions relax to thermal equilibrium (as predicted by ...Maxwell-Boltzman statistics), is a fundamental question in studies of astrophysical and laboratory plasmas. Astrophysical plasmas are often so tenuous that binary collisions can be ignored, and it is not clear how thermal equilibrium develops for these 'collisionless' plasmas. One example of a collisionless plasma is the Earth's plasma sheet, where thermalized hot plasma with ion temperatures of about 5 × 107 K has been observed. Here we report direct observations of a plasma distribution function during a solar eclipse, revealing cold ions in the Earth's plasma sheet in coexistence with thermalized hot ions. This cold component cannot be detected by plasma sensors on satellites that are positively charged in sunlight, but our observations in the Earth's shadow show that the density of the cold ions is comparable to that of hot ions. This high density is difficult to explain within existing theories, as it requires a mechanism that permits half of the source plasma to remain cold upon entry into the hot turbulent plasma sheet.
The mevalonate pathway is prevalent in eukaryotes, archaea, and a limited number of bacteria. This pathway yields the fundamental precursors for isoprenoid biosynthesis, i.e., isopentenyl diphosphate ...and dimethylally diphosphate. In the downstream part of the general eukaryote-type mevalonate pathway, mevalonate is converted into isopentenyl diphosphate by the sequential actions of mevalonate kinase, phosphomevalonate kinase, and diphosphomevalonte decarboxylase, while a partial lack of the putative genes of these enzymes is sometimes observed in archaeal and bacterial genomes. The absence of these genes has led to the recent discovery of modified mevalonate pathways. Therefore, we decided to investigate the mevalonate pathway of Flavobacterium johnsoniae, a bacterium of the phylum Bacteroidetes, which is reported to lack the genes of mevalonate kinase and phosphomevalonate kinase. This study provides proof of the existence of the general mevalonate pathway in F. johnsoniae, although the pathway involves the kinases that are distantly related to the known enzymes.
•Some Bacteroidetes species reportedly lack two genes of the mevalonate pathway.•Genes conserved only among the species were searched via comparative genome analysis.•Some of the genes encode putative enzymes distantly related to mevalonate kinase.•The enzymes from Flavobacterium johnsoniae catalyze the missing steps of the pathway.•The kinetic parameters of the enzymes are comparable to those of known enzymes.
The Small Carry-on Impactor (SCI) equipped on
Hayabusa2
was developed to produce an artificial impact crater on the primitive Near-Earth Asteroid (NEA) 162173 Ryugu (Ryugu) in order to explore the ...asteroid subsurface material unaffected by space weathering and thermal alteration by solar radiation. An exposed fresh surface by the impactor and/or the ejecta deposit excavated from the crater will be observed by remote sensing instruments, and a subsurface fresh sample of the asteroid will be collected there. The SCI impact experiment will be observed by a Deployable CAMera 3-D (DCAM3-D) at a distance of ∼1 km from the impact point, and the time evolution of the ejecta curtain will be observed by this camera to confirm the impact point on the asteroid surface. As a result of the observation of the ejecta curtain by DCAM3-D and the crater morphology by onboard cameras, the subsurface structure and the physical properties of the constituting materials will be derived from crater scaling laws. Moreover, the SCI experiment on Ryugu gives us a precious opportunity to clarify effects of microgravity on the cratering process and to validate numerical simulations and models of the cratering process.
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