A stochastic simulation of the propagation of Galactic cosmic rays reflecting the discreteness of cosmic ray sources. Age and path length distribution

The path length distribution of Galactic cosmic rays (GCRs) is the fundamental ingredient for modeling the propagation process of GCRs based on the so-called weighted slab method. We try to derive this distribution numerically by taking into account the discreteness in both space and time of occurrences of supernova explosions where GCRs are suspected to be born. We solve numerically the stochastic differential equations equivalent to the Parker diffusion-convection equation which describes the propagation process of GCR in the Galaxy. We assume the three-dimensional diffusion is an isotropic one without any free escape boundaries. We ignore any energy change of GCRs and the existence of the Galactic wind for simplicity. We also assume axisymmetric configurations for the density distributions of the interstellar matter and for the surface density of supernovae. We have calculated age and path length of GCR protons arriving at the solar system with this stochastic method. The obtained age is not the escape time of GCRs from the Galaxy as usually assumed, but the time spent by GCRs during their journey to the solar system from the supernova remnants where they were born. The derived age and path length show a distribution spread in a wide range even for GCR protons arriving at the solar system with the same energy. The distributions show a cut-off at a lower range in age or path length depending on the energy of GCRs. These cut-offs clearly come from the discreteness of occurrence of supernovae. The mean age of GeV particles obtained from the distributions is consistent with the age obtained by direct observation of radioactive secondary nuclei. The energy dependence of the B/C ratio estimated with the path length distribution reproduces reliably the energy dependence of B/C obtained by recent observations in space.Comment: 5 pages, 5 figures. Accepted for publication in A&

Emission from Bow Shocks of Beamed Gamma-Ray Bursts

Beamed gamma-ray burst (GRB) sources produce a bow shock in their gaseous environment. The emitted flux from this bow shock may dominate over the direct emission from the jet for lines of sight which are outside the angular radius of the jet emission, theta. The event rate for these lines of sight is increased by a factor of 260*(theta/5_degrees)^{-2}. For typical GRB parameters, we find that the bow shock emission from a jet with half-angle of about 5 degrees is visible out to tens of Mpc in the radio and hundreds of Mpc in the X-rays. If GRBs are linked to supernovae, studies of peculiar supernovae in the local universe should reveal this non-thermal bow shock emission for weeks to months following the explosion.Comment: ApJ, submitted, 15 pages, 3 figure

Synthesis of a Novel D-Glucose-Conjugated 15-Crown-5 Ether with a Spiro Ketal Structure

Abstract: This paper describes a synthetic approach to a novel D-glucose-conjugated 15-crown-5 ether having a spiroketal structure starting from a 1-C-vinylated glucose derivative. The approach consists of the glycosylation of the vinylated glucose derivative to give an ethyleneoxy spacer derivative using bismuth(III) triflate, the conversion of the 1-C-vinyl group of the glucoside produced into a carboxylic acid group, and the intramolecular condensation between the carboxyl group and the terminal hydroxyl group in the ethyleneoxy spacer. A D-glucose-conjugated 15-crown-5 ether having a unique spiroketal structure was thus successfully synthesized

No evidence yet for hadronic TeV gamma-ray emission from SNR RX J1713.7-3946

Recent TeV-scale gamma-ray observations with the CANGAROO II telescope have led to the claim that the multi-band spectrum of RX J1713.7-3946 cannot be explained as the composite of a synchrotron and an inverse Compton component emitted by a population of relativistic electrons. It was argued that the spectrum of the high-energy emission is a good match to that predicted by pion decay, thus providing observational evidence that protons are accelerated in SNR to at least TeV energies. In this Letter we discuss the multi-band spectrum of RX J1713.7-3946 under the constraint that the GeV-scale emission observed from the closely associated EGRET source 3EG J1714-3857 is either associated with the SNR or an upper limit to the gamma-ray emission of the SNR. We find that the pion-decay model adopted by Enomoto et al. is in conflict with the existing GeV data. We have examined the possibility of a modified proton spectrum to explain the data, and find that we cannot do so within any existing theoretical framework of shock acceleration models.Comment: in press as Letter to Astronomy & Astrophysic

ダイ4ジ ナンキョク チイキ カンソクタイ チジキ ブモン センジョウ カンソク ホウコク

The geomagnetic total force observations along the navigation route from Japan to the Antarctic Ocean via Singapore and Cape Town were carried out using the Proton Precession Magnetometer which was used in the second (1957-58) and the third (1958-59) expeditions for the same purpose. We got nearly the same results at the Indian Ocean as on former observations. In this paper, the results of observation from Cape Town to the Antarctic Ocean are chiefly reported. 1. We discovered about 10 discrepancy between the total force of our measurement by Proton Magnetometer and that of Hermanus Observatory, Cape Province, South Africa obtain from Variometers. Fig. 1. 2. The iso-total force lines diagram deduced from the results of observation at the second and fourth expedition are illustrated in Fig. 2. 3. The annual changes of the total force between Cape Town and the Antarctic Ocean deduced from the results at the second, third and fourth expeditions are shown in Fig. 3, where no corrections for diurnal variation are applied. 4. The tso-total force lines diagram in the Lutzow-Holm Bay deduced from the results at the second and fourth expeditions are illustrated in Fig. 4. 5. Anomaly changes of about 400 were observed which are presumed to be caused by the submarine relief. Two examples are illustrated in Fig. 5

The Uptake of ACNU in the Experimental Brain Tumor and the Effect of Induced Hypertension - Part II -

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A two-zone model for the emission from RX J1713.7-3946

We study the acceleration and radiation of charged particles in the shock waves of supernova remnants using a recent version of the "box model". According to this, particles are accelerated in an energy-dependent region around the shock by the first order Fermi mechanism and lose energy through radiation. The particle distribution function is obtained from a spatially averaged kinetic equation that treats the energy losses self-consistently. There exists also a second population that consists of those particles that escape behind the shock where they also radiate. The energy distribution of this population is calculated in a similar manner. The application of the model to the supernova remnant RX J1713.7-3946, which was recently confirmed as a TeV source by H.E.S.S., shows that the X-ray emission can be attributed to electron synchrotron radiation while in gamma-rays there are contributions from both electrons and protons, with protons playing the dominant role. Additionally, there are strong indications that particles diffuse in turbulence that has a Kolmogorov spectrum.Comment: 6 pages, 2 figures, accepted by Astronomy and Astrophysic