Despite the significant progress achieved in recent years, the physical mechanisms underlying the origin of solar energetic particles (SEPs) are still a matter of debate. The complex nature of both ...particle acceleration and transport poses challenges to developing a universal picture of SEP events that encompasses both the low-energy (from tens of keV to a few hundreds of MeV) observations made by space-based instruments and the GeV particles detected by the worldwide network of neutron monitors in ground-level enhancements (GLEs). The high-precision data collected by the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) satellite experiment offer a unique opportunity to study the SEP fluxes between ∼80 MeV and a few GeV, significantly improving the characterization of the most energetic events. In particular, PAMELA can measure for the first time with good accuracy the spectral features at moderate and high energies, providing important constraints for current SEP models. In addition, the PAMELA observations allow the relationship between low- and high-energy particles to be investigated, enabling a clearer view of the SEP origin. No qualitative distinction between the spectral shapes of GLE, sub-GLE and non-GLE events is observed, suggesting that GLEs are not a separate class, but are the subset of a continuous distribution of SEP events that are more intense at high energies. While the spectral forms found are to be consistent with diffusive shock acceleration theory, which predicts spectral rollovers at high energies that are attributed to particles escaping the shock region during acceleration, further work is required to explore the relative influences of acceleration and transport processes on SEP spectra.
Precise measurements of the time-dependent intensity of the low-energy (<50 GeV) galactic cosmic rays (GCRs) are fundamental to test and improve the models that describe their propagation inside the ...heliosphere. In particular, data spanning different solar activity periods, i.e., from minimum to maximum, are needed to achieve comprehensive understanding of such physical phenomena. The minimum phase between solar cycles 23 and 24 was peculiarly long, extending up to the beginning of 2010 and followed by the maximum phase, reached during early 2014. In this Letter, we present proton differential spectra measured from 2010 January to 2014 February by the PAMELA experiment. For the first time the GCR proton intensity was studied over a wide energy range (0.08-50 GeV) by a single apparatus from a minimum to a maximum period of solar activity. The large statistics allowed the time variation to be investigated on a nearly monthly basis. Data were compared and interpreted in the context of a state-of-the-art three-dimensional model describing the GCRs propagation through the heliosphere.
The article studies the relationship between particle precipitation from the Earth’s radiation belt and cosmic gamma-ray bursts. For this purpose, experimental measurements of charged cosmic ray ...fluxes in the PAMELA experiment and gamma-ray burst observations by the Fermi Observatory are used. Both instruments operated simultaneously in Earth orbit between 2008 and 2016. For the time of each gamma-ray burst detected by the Fermi Observatory during the specified period, the count rate of the PAMELA detectors is analyzed. In order to search for a possible signal from the interaction of a gamma-ray burst with charged particles in the near-Earth space, annual background maps of count rates of the time-of-flight detectors are constructed. The difference between the background count rate and the count rate at the time of the gamma-ray burst arrival (in the time interval several minutes before and after) is analyzed. Several cases are found in which the count rate significantly deviated from the background value at the time of the gamma-ray burst arrival and lasted up to 5–10 min after it.
Enzymatic deamination of bases in DNA or RNA leads to an alteration of flow of genetic information. Adenosine deaminases edit RNA (ADARs, TADs). Specialized cytidine deaminases are involved in ...RNA/DNA editing in lipid metabolism (APOBEC1) and in innate (APOBEC3 family) and humoral (AID) immunity. APOBEC2 is required for proper muscle development and, along with AID, was implicated in demethylation of DNA. The functions of APOBEC4, APOBEC5, and other deaminases recently discovered by bioinformatics approaches are unknown. What is the basis for the diverse biological functions of enzymes with similar enzyme structure and the same principal enzymatic reaction? AID, APOBEC1, lamprey CDA1, and APOBEC3G enzymes cause uracil DNA glycosylase-dependent induction of mutations when overproduced ectopically in bacteria or yeast. APOBEC2, on the contrary, is nonmutagenic. We studied the effects of the expression of various deaminases in yeast and bacteria. The mutagenic specificities of four deaminases, hAID, rAPOBEC1, hAPOBEC3G, and lamprey CDA1, are strikingly different. This suggests the existence of an intrinsic component of deaminase targeting. The expression of yeast CDD1 and TAD2/TAD3, human APOBEC4, Xanthomonas oryzae APOBEC5, and deaminase encoded by Micromonas sp. gene MICPUN_56782 was nonmutagenic. A lack of a mutagenic effect for Cdd1 is expected because the enzyme functions in the salvage of pyrimidine nucleotides, and it is evolutionarily distant from RNA/DNA editing enzymes. The reason for inactivity of deaminases grouped with APOBEC2 is not obvious from their structures. This cannot be explained by protein insolubility and peculiarities of cellular distribution and requires further investigation.
On the 15th of June 2006, the PAMELA (Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics) satellite-borne experiment was launched onboard the Russian Resurs-DK1 satellite by a ...Soyuz rocket from the Baikonur space centre. The satellite was placed in a quasi-polar 70°inclination orbit at an altitude varying between 350 km and 600 km.
New results on the antiparticle component of the cosmic radiation were obtained. The positron energy spectrum and positron fraction were measured from 400 MeV up to 200 GeV revealing a positron excess over the predictions of commonly used propagation models. This can be interpreted either as evidence that the propagation models should be revised or in terms of dark matter annihilation or a pulsar contribution. The antiproton spectrum was measured over the energy range from 60 MeV to 350 GeV. The antiproton spectrum is consistent with secondary production and significantly constrains dark matter models.
The energy spectra of protons and helium nuclei were measured up to 1.2 TV. The spectral shapes of these two species are different and cannot be described well by a single power law. For the first time the electron spectrum was measured up to 600 GeV complementing the information obtained from the positron data. Nuclear and isotopic composition was obtained with unprecedented precision.
The variation of the low energy proton, electron and positron energy spectra was measured from July 2006 until December 2009 accurately sampling the unusual conditions of the most recent solar minimum activity period (2006–2009). Low energy particle spectra were accurately measured also for various solar events that occurred during the PAMELA mission.
The Earth’s magnetosphere was studied measuring the particle radiation in different regions of the magnetosphere. Energy spectra and composition of sub-cutoff and trapped particles were obtained. For the first time a belt of trapped antiprotons was detected in the South Atlantic Anomaly region. The flux was found to exceed that for galactic cosmic-ray antiprotons by three order of magnitude.
Abstract
Using measurements from the PAMELA and ARINA spectrometers on board the Resurs-DK1 satellite, we have examined the 27 day intensity variations in galactic cosmic ray (GCR) proton fluxes in ...2007–2008. The PAMELA and ARINA data allow for the first time a study of time profiles and the rigidity dependence of the 27 day variations observed directly in space in a wide rigidity range from ∼300 MV to several gigavolts. We find that the rigidity dependence of the amplitude of the 27 day GCR variations cannot be described by the same power law at both low and high energies. A flat interval occurs at rigidity
GV with a power-law index
γ
= −0.13 ± 0.44 for PAMELA, whereas for
R
≥ 1 GV, the power-law dependence is evident with index
γ
= −0.51 ± 0.11. We describe the rigidity dependence of the 27 day GCR variations for PAMELA and ARINA data in the framework of the modulation potential concept using the force-field approximation for GCR transport. For a physical interpretation, we have considered the relationship between the 27 day GCR variations and solar wind plasma and other heliospheric parameters. Moreover, we have discussed possible implications of MHD modeling of the solar wind plasma together with a stochastic GCR transport model concerning the effects of corotating interaction regions.
Precise time-dependent measurements of the Z = 2 component in the cosmic radiation provide crucial information about the propagation of charged particles through the heliosphere. The PAMELA ...experiment, with its long flight duration (2006 June 15-2016 January 23) and the low energy threshold (80 MeV/n) is an ideal detector for cosmic-ray solar modulation studies. In this paper, the helium nuclei spectra measured by the PAMELA instrument from 2006 July to 2009 December over a Carrington rotation time basis are presented. A state-of-the-art three-dimensional model for cosmic-ray propagation inside the heliosphere was used to interpret the time-dependent measured fluxes. Proton-to-helium flux ratio time profiles at various rigidities are also presented in order to study any features that could result from the different masses and local interstellar spectra shapes.
A simple and robust method of reconstruction of the geomagnetically trapped proton fluxes detected with the PAMELA spectrometer is proposed. Instead of multiple calculations of the effective area for ...different pitch-angles and different orientations of the instrument relative to the geomagnetic field vector, a value of an effective geometrical factor (GF) is estimated using one simulation sample with additional information about the instrument’s orientation relative to the vector of the Earth magnetic field. In this procedure, the additivity of the geometrical factor for different parts of the instrument’s field of view (FOV) is used. The simulation data sample is obtained in a standard way using Monte Carlo calculations of the isotropic flux. The method was tested on the task of reconstruction of the angular distribution of the Galactic proton flux. The fluxes in the Earth’s Inner Radiation Belt (IRB) recovered with this method were compared with the measurements of the NOAA-17 experiment and showed a good agreement.
Protons and helium nuclei are the most abundant components of the cosmic radiation. Precise measurements of their fluxes are needed to understand the acceleration and subsequent propagation of cosmic ...rays in our Galaxy. We report precision measurements of the proton and helium spectra in the rigidity range 1 gigavolt to 1.2 teravolts performed by the satellite-borne experiment PAMELA (payload for antimatter matter exploration and light-nuclei astrophysics). We find that the spectral shapes of these two species are different and cannot be described well by a single power law. These data challenge the current paradigm of cosmic-ray acceleration in supernova remnants followed by diffusive propagation in the Galaxy. More complex processes of acceleration and propagation of cosmic rays are required to explain the spectral structures observed in our data.
PDF
