Time dependence of the helium flux measured by PAMELA

Precision measurements of the Z = 2 component in cosmic radiation provide crucial information about the origin and propagation of the second most abundant cosmic ray species in the Galaxy (9% of the total). These measurements, acquired with the PAMELA space experiment orbiting Earth, allow to study solar modulation in details. Helium modulation is compared to the modulation of protons to study possible dependencies on charge and mass. The time dependence of helium fluxes on a monthly basis measured by PAMELA has been studied for the period between July 2006 to January 2016 in the energy range from 800 MeV/n to ~ 20 GeV/n.

Time Dependence of the Electron and Positron Components of the Cosmic Radiation Measured by the PAMELA Experiment between July 2006 and December 2015

Cosmic-ray electrons and positrons are a unique probe of the propagation of cosmic rays as well as of the nature and distribution of particle sources in our Galaxy. Recent measurements of these particles are challenging our basic understanding of the mechanisms of production, acceleration, and propagation of cosmic rays. Particularly striking are the differences between the low energy results collected by the space-borne PAMELA and AMS-02 experiments and older measurements pointing to sign-charge dependence of the solar modulation of cosmic-ray spectra. The PAMELA experiment has been measuring the time variation of the positron and electron intensity at Earth from July 2006 to December 2015 covering the period for the minimum of solar cycle 23 (2006-2009) until the middle of the maximum of solar cycle 24, through the polarity reversal of the heliospheric magnetic field which took place between 2013 and 2014. The positron to electron ratio measured in this time period clearly shows a sign-charge dependence of the solar modulation introduced by particle drifts. These results provide the first clear and continuous observation of how drift effects on solar modulation have unfolded with time from solar minimum to solar maximum and their dependence on the particle rigidity and the cyclic polarity of the solar magnetic field.

New upper limit on strange quark matter abundance in cosmic rays with the PAMELA space experiment

In this work we present results of a direct search for strange quark matter (SQM) in cosmic rays with the PAMELA space spectrometer. If this state of matter exists it may be present in cosmic rays as particles, called strangelets, having a high density and an anomalously high mass-to-charge (A/Z) ratio. A direct search in space is complementary to those from ground-based spectrometers. Furthermore, it has the advantage of being potentially capable of directly identifying these particles, without any assumption on their interaction model with Earth's atmosphere and the long-term stability in terrestrial and lunar rocks. In the rigidity range from 1.0 to ∼1.0×10^{3}  GV, no such particles were found in the data collected by PAMELA between 2006 and 2009. An upper limit on the strangelet flux in cosmic rays was therefore set for particles with charge 1≤Z≤8 and mass 4≤A≤1.2×10^{5}. This limit as a function of mass and as a function of magnetic rigidity allows us to constrain models of SQM production and propagation in the Galaxy.

Time dependence of X-ray polarizability of a crystal induced by an intense femtosecond X-ray pulse

The time evolution of the electron density and the resulting time dependence of Fourier components of the X-ray polarizability of a crystal irradiated by highly intense femtosecond pulses of an X-ray free-electron laser (XFEL) is investigated theoretically on the basis of rate equations for bound electrons and the Boltzmann equation for the kinetics of the unbound electron gas. The photoionization, Auger process, electron-impact ionization, electron-electron scattering and three-body recombination have been implemented in the system of rate equations. An algorithm for the numerical solution of the rate equations was simplified by incorporating analytical expressions for the cross sections of all the electron configurations in ions within the framework of the effective charge model. Using this approach, the time dependence of the inner shell populations during the time of XFEL pulse propagation through the crystal was evaluated for photon energies between 4 and 12 keV and a pulse width of 40 fs considering a flux of 10(12) photons pulse(-1) (focusing on a spot size of ∼1 µm). This flux corresponds to a fluence ranging between 0.8 and 2.4 mJ µm(-2). The time evolution of the X-ray polarizability caused by the change of the atomic scattering factor during the pulse propagation is numerically analyzed for the case of a silicon crystal. The time-integrated polarizability drops dramatically if the fluence of the X-ray pulse exceeds 1.6 mJ µm(-2).

Cosmic-ray positron energy spectrum measured by PAMELA

Precision measurements of the positron component in the cosmic radiation provide important information about the propagation of cosmic rays and the nature of particle sources in our Galaxy. The satellite-borne experiment PAMELA has been used to make a new measurement of the cosmic-ray positron flux and fraction that extends previously published measurements up to 300 GeV in kinetic energy. The combined measurements of the cosmic-ray positron energy spectrum and fraction provide a unique tool to constrain interpretation models. During the recent solar minimum activity period from July 2006 to December 2009, approximately 24,500 positrons were observed. The results cannot be easily reconciled with purely secondary production, and additional sources of either astrophysical or exotic origin may be required.

Quantitative genetic study of the circulating osteopontin in community-selected families

The study assessed contribution of genetic factors to variability of osteopontin (OPN) levels. Evidence of association of OPN levels with polymorphisms in its structural gene and integrin-binding sialoprotein gene loci was obtained. The results motivate research of OPN-related proteins and genes with respect to biomineralization and other biological processes.

INTRODUCTION

OPN is a major phosphoprotein in bone, which plays key role in regulation of bone mineralization process. It is considered as a promising biomarker for osteoarthritis and osteoporosis, and various other pathological conditions. However, the contribution of genetics and other confounding factors to OPN circulating levels variation in general population has never been specifically determined. The main aims of the present study included (1) evaluation of the putative genetic and familial factors' effect on OPN variability and (2) testing the hypothesis that OPN plasma levels are associated with the genetic polymorphisms in its structural gene locus (SPP1) and in integrin-binding sialoprotein gene locus (IBSP).

METHODS

To address these questions, we used a family-based sample of 925 apparently healthy Caucasian individuals. Association of OPN levels with three SNPs in each of the two selected gene loci was explored using pedigree disequilibrium tests.

RESULTS

Some 58% and 13% of the OPN levels variability were attributable to genetic factors and common spouse environment, respectively. Three SNPs showed nominally significant association with OPN (p < 0.05). Of these, rs2616262 linked to IBSP promoter region remained significant after correction for multiple testing (p = 0.003). Significant association of this SNP and rs10516799 (distal segment of SPP1) with OPN was confirmed in several statistical tests. Using a special modification of variance component analysis, we examined gene-gene and gene-sex interaction effects, but found non-significant confirmation for these hypotheses.

CONCLUSIONS

Further studies are required to confirm the observed results and to explore the underlying molecular and physiological mechanisms.

Quantitative genetic study of amphiregulin and fractalkine circulating levels--potential markers of arthropathies

OBJECTIVE

Amphiregulin (AREG) and Fractalkine (FRACT), are involved in a variety of normal and pathological processes, and are both suggested to be relevant to joint degeneration. The aims of the present study included (1) testing association between circulating levels of these biomarkers and joint pathologies, (2) evaluation of the putative genetic and familial factors' effect on AREG and FRACT variability.

DESIGN

The study was conducted in the family-based sample of 923 Caucasian individuals. Variance component analysis was used to assess contribution of genetic and environmental factors to variability of AREG and FRACT concentration.

RESULTS

The mean levels of FRACT were significantly higher in the affected group with arthropathies (synovial joints osteoarthritis (OA) and disc degenerative disease, DDD) then in the control group (P<0.0004). Circulating AREG levels were higher in DDD (P=0.0272). Genetic factors constituted the main source of the interindividual differences of the AREG and FRACT levels in our sample, and explained 29.68% and 41.68% of the total variation, respectively. The phenotypic correlation between AREG and FRACT was substantial (r=0.55, P=0.0001) and was associated with both common genetic and environmental factors. Specifically, 30% of the phenotypic correlation between AREG and FRACT was due to common genetic effects.

CONCLUSIONS

Further studies are required to assess relevancy of FRACT to clinical diagnosis and prognosis of arthropathies, to investigate the mechanisms behind the observed phenotypic and genetic covariation among the studied biomarkers, and to explore specific genetic polymorphisms affecting AREG and FRACT variation.

Cosmic-ray electron flux measured by the PAMELA experiment between 1 and 625 GeV

Precision measurements of the electron component in the cosmic radiation provide important information about the origin and propagation of cosmic rays in the Galaxy. Here we present new results regarding negatively charged electrons between 1 and 625 GeV performed by the satellite-borne experiment PAMELA. This is the first time that cosmic-ray e⁻ have been identified above 50 GeV. The electron spectrum can be described with a single power-law energy dependence with spectral index -3.18 ± 0.05 above the energy region influenced by the solar wind (> 30 GeV). No significant spectral features are observed and the data can be interpreted in terms of conventional diffusive propagation models. However, the data are also consistent with models including new cosmic-ray sources that could explain the rise in the positron fraction.

PAMELA results on the cosmic-ray antiproton flux from 60 MeV to 180 GeV in kinetic energy

The satellite-borne experiment PAMELA has been used to make a new measurement of the cosmic-ray antiproton flux and the antiproton-to-proton flux ratio which extends previously published measurements down to 60 MeV and up to 180 GeV in kinetic energy. During 850 days of data acquisition approximately 1500 antiprotons were observed. The measurements are consistent with purely secondary production of antiprotons in the Galaxy. More precise secondary production models are required for a complete interpretation of the results.

New measurement of the antiproton-to-proton flux ratio up to 100 GeV in the cosmic radiation

A new measurement of the cosmic-ray antiproton-to-proton flux ratio between 1 and 100 GeV is presented. The results were obtained with the PAMELA experiment, which was launched into low-Earth orbit on-board the Resurs-DK1 satellite on June 15th 2006. During 500 days of data collection a total of about 1000 antiprotons have been identified, including 100 above an energy of 20 GeV. The high-energy results are a tenfold improvement in statistics with respect to all previously published data. The data follow the trend expected from secondary production calculations and significantly constrain contributions from exotic sources, e.g., dark matter particle annihilations.

Dosimetric results from the Mir orbital station

The Mir Orbital Station provided a unique platform on which to carry out a variety of space radiation dosimetry measurements. A number of experiments were conducted using a combination of passive detectors on the interior of the Mir during 1996-97. Thermoluminescent detectors were used to measure absorbed dose. CR-39 plastic nuclear track detectors were used to measure the LET spectra > or =5 keV.microm(-1). Results from TLDs and CR-39 PNTDs were combined to determine total dose and dose equivalent. Mean dose rate was found to decrease while mean dose equivalent rate and average quality factor increased with increasing shielding. Secondary particles from proton-induced target fragmentation interactions, not primary HZE particles, were found to be the largest contributor to the LET spectrum above 100 keV.microm(-1). During the 1997 measurements, mean quality factor was found to vary from 1.7 to 2.1 as a function of location within the Mir.

Direct localization by cryo-electron microscopy of secondary structural elements in Escherichia coli 23 S rRNA which differ from the corresponding regions in Haloarcula marismortui

Insertions were introduced by a two-step mutagenesis procedure into each of five double-helical regions of Escherichia coli 23 S rRNA, so as to extend the helix concerned by 17 bp. The helices chosen were at sites within the 23 S molecule (h9, h25, h45, h63 and h98) where significant length variations between different species are known to occur. At each of these positions, with the exception of h45, there are also significant differences between the 23 S rRNAs of E. coli and Haloarcula marismortui. Plasmids carrying the insertions were introduced into an E. coli strain lacking all seven rrn operons. In four of the five cases the cells were viable and 50 S subunits could be isolated; only the insertion in h63 was lethal. The modified subunits were examined by cryo-electron microscopy (cryo-EM), with a view to locating extra electron density corresponding to the insertion elements. The results were compared both with the recently determined atomic structure of H. marismortui 23 S rRNA in the 50 S subunit, and with previous 23 S rRNA modelling studies based on cryo-EM reconstructions of E. coli ribosomes. The insertion element in h45 was located by cryo-EM at a position corresponding precisely to that of the equivalent helix in H. marismortui. The insertion in h98 (which is entirely absent in H. marismortui) was similarly located at a position corresponding precisely to that predicted from the E. coli modelling studies. In the region of h9, the difference between the E. coli and H. marismortui secondary structures is ambiguous, and the extra electron density corresponding to the insertion was seen at a location intermediate between the position of the nearest helix in the atomic structure and that in the modelled structure. In the case of h25 (which is about 50 nucleotides longer in H. marismortui), no clear extra cryo-EM density corresponding to the insertion could be observed.