2 edition of Gradients and anisotropies of high energy cosmic rays in the outer heliosphere found in the catalog.
Gradients and anisotropies of high energy cosmic rays in the outer heliosphere
1985 by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English
|Statement||Fillius, Walker ... [et al.].|
|Series||NASA contractor report -- NASA CR-176944.|
|Contributions||Fillius, Walker., United States. National Aeronautics and Space Administration.|
|The Physical Object|
An early motivation for studying high-energy cosmic rays was the expectation that anisotropies in the arrival directions would be found. However, as more and more information became available about galactic magnetic field strengths, it was realised that protons with energies at least as great as 30 EeV must be studied to pick out point : Lu Lu, Alan Watson. MAGNETIC RECONNECTION AS THE CAUSE OF COSMIC RAY EXCESS FROM THE HELIOSPHERIC TAIL A. Lazarian1 and P. Desiati2 It is known that cosmic rays arrival direction has an energy- shown for reference at high energy and with the amplitude multiplied by 1/4 to account for the larger anisotropy amplitude at high energy), Nagoya. Figure spectrum of primary cosmic rays (on a logarithmic scale): (a) differential spectrum (dependence of intensity / on energy ε) in the moderate-energy region for protons (p) and alpha particles (experimental points are also plotted), (b) integral spectrum (for all particles) in the high-energy region (the experimental points were obtained by satellites of the Proton series [1, 2. The intensity of Galactic cosmic rays in the heliosphere is modulated by solar activities. The outer boundary where the solar modulation begins has always been a subject matter of debate in the cos Cited by:
Anomalous cosmic rays in the distant heliosphere and the reversal of the Sun’s magnetic polarity in Cycle 23 F. B. McDonald,1 E. C. Stone,3 A. C. Cummings,3 W. R. Webber,2 B. C. Heikkila,4 and N. Lal4 Received 28 November ; revised 5 January ; accepted 17 .
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Get this from a library. Gradients and anisotropies of high energy cosmic rays in the outer heliosphere. [Walker Fillius; United States. National Aeronautics and Space Administration.;]. GRADIENTS AND ANISOTROPIES OF HIGH ENERGY COSMIC RAYS IN THE OUTER HELIOSPHERE Fillius, Walker [I], E.
Roelof , Edward J. Smith , David Wood [I], and Wing-Huen Ip  I University of California, San Diego, La Jolla, CA 2 Johns Hopkins University Applied Physics Laboratory, Laurel, MD 3 Jet Propulsion Laboratory, Pasadena, CA The jump condition across the shock prescribes that both the cosmic ray phase space density, f, and the the normal component of the net flux, S~, must be the same on both sides of the shock + + f~ =0 and SnI 0 (2) Cosmic-Ray Gradients (6) with S~ being the radial component S~ in our case SrCfVw+Krr~ (3) These jump conditions represent the Cited by: 4.
components of solar modulation and produce streaming (anisotropies) of particles in the heliosphere. The anisotropies can be investigated at Earth by examining the count rates of cosmic ray detectors.
The anisotropic streams appear as diurnal and semi-diurnal variations in the count rates of cosmic ray recorders in solar and sidereal time. diffusion, convection and adiabatic energy loss. Our analysis indicates that adiabatic energy may play an impor-tant role in the radial distribution of galactic cosmic rays in the inner heliosphere.
In the outer region diffusion and convection are the dominant processes. Key words: Cosmic ray modulation, transport equation, gradients. Introduction. A durable reduction of cosmic ray intensity in the outer heliosphere James A. Van Allen and Bruce A. Randall Department of Physics and Astronomy, University of Iowa, Iowa City Abstract.
This paper reports Pioneer 10 (P10) and Pioneer 11 (Pll) observations of the intensity J(Ep > 80 MeV) of galactic cosmic rays in the heliosphere near theFile Size: KB. The observed intensities at the minimum of negative solar Cycle 21 are plotted as a function of radial distance for galactic and anomalous cosmic rays in Fig.
radial dependences appear to be described by a power of radial distance through 1 to ∼40 AU, suggesting that the dependences are not so much different in the inner and outer by: Cummings, A.
C., E. Stone, F. McDonald, B. Heikkila, N. Lal, and W. Webber, "Evolution of the Energy Spectra of Low-Energy Particles at Voyagers 1 and 2 in the Outer Heliosphere and Implications for the Source Location of Anomalous Cosmic Rays", American Geophysical Union, Fall Meetingabstract #SH11A, For high-energy cosmic rays, however, it is more efficient to exploit the atmosphere, measuring each cosmic ray indirectly by observing the shower of particles it produces in the air.
An air shower occurs when a fast-moving cosmic ray particle strikes an air molecule high in. The spatial distribution of galactic and anomalous cosmic rays in the heliosphere at solar minimum Z. Fujii a,b,*, F.B. McDonald b a Solar Terrestrial Environment Laboratory, Nagoya University, Chikusa-ku, NagoyaJapan b Institute for Physical Science and Technology, University of Maryland, College Park, MDUSA Received 31 October ; received in revised form 10 January This is a rapporteur paper for the XXIV International Cosmic-Ray Conference covering topics of anomalous cosmic rays, shock acceleration, modulation and transport theory, cosmic-ray gradients, corotating interaction regions, coronal-mass ejections, and solar neutrinos.
Among the highlights of the meeting are —conclusive proof that most anomalous cosmic rays are singly Cited by: 2. latitudinal gradients of cosmic ray electrons in the inner heliosphere. While less statistically conclusive than one might desire, our analysis provides the only measurement ever made of these gradients.
In this paper we consider electrons unresolved as to charge sign, that is we use the term electrons to include both negatrons and positrons.
Four-dimensional Transport of Galactic Cosmic Rays in the Outer Heliosphere and Heliosheath. This analysis also leads to an interstellar galactic cosmic ray energy density of ≡ eV cm The distribution of galactic cosmic ray particles in the heliosphere is influenced (modulated) by the Sun's interplanetary magnetic field (IMF) and the solar wind.
The particles diffuse inward, convect outward and have drifts in the motion of their gyro-centres. They are also scattered from their gyro-orbits by irregularities in the by: 4. The strong shocks, bounding the supernova remnants, are the sites of high-energy particle acceleration (cosmic rays), which fill, and diffuse through, the whole galactic disk, eventually entering.
discuss the Galactic Cosmic Ray (GCR) spectrum, as well as the extragalactic Ultra High Energy Cosmic Rays (UHE-CRs), their chemical abundances and anisotropies. UHECRs may include a proton component from many radio galaxies integrated over vast distances, visible already below 3 EeV.
1 Introduction The spectrum of Cosmic Rays (CRs) ranges from. Near-Earth Measurements and Modeling ta Physics Department, Shinshu University, MatsumotoJapan modulation models, cosmic-ray density gradients, anisotropies, en-ergyspectraandcomposition,presentedinsessionsSH,SH,SH,SH The average spatial gradients of cosmic rays in the heliosphere are calcu.
New model connects the origins of very high-energy neutrinos, ultrahigh-energy cosmic rays, and high-energy gamma rays with black-hole jets embedded in their environments. origin and propagation of these Extremely High Energy (EHE) cosmic rays in the Universe.
After a brief review of the observed cosmic rays in general and their possible sources and acceleration mechanisms, a detailed discussion is given of possible “top-down” (non-acceleration) scenarios of origin of EHE cosmic.
30 TH INTERNATIONAL C OSMIC R AY C ONFERENCE Horizons and Anisotropies of Ultra-High Energy Cosmic Rays A. O LINTO 1 ;2, D.A LLARD 1, E.A RMENGAUD 3, A. K RAVTSOV. This is an investigation into time-dependent cosmic ray modulation in the outer heliosphere.
This talk highlighted our ndings regarding the sensitivity of in-tensities to variations in the boundary position and possible asym-metry of the heliosphere. Next phase is to predict a. Global gradients for cosmic-ray (CR) protons in the heliosphere are computed with a comprehensive modulation model for the recent prolonged solar minimum of Cycle 23/ Fortunately, the PAMELA (Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics) and Ulysses/KET (Kiel Electron Telescope) instruments simultaneously observed proton intensities for the period Cited by: ) predict the latitudinal distribution of galactic cosmic ray (GCR) protons and electrons.
In the s and in the s, during an A. Hill, M.E., Investigating the Heliosphere with Low-Energy Anolmalous Cosmic Rays, Physics of the Outer Heliosphere: Third International IGPP Conference, edited. Lecture Notes on High Energy Cosmic Rays prepared for the th Jyv¨askly¨a Summer School, August M.
Kachelrieß Institutt for fysikk, NTNU, Trondheim, Norway Abstract: I give a concise introduction into high energy cosmic ray physics, including also few related aspects of high energy gamma-ray and neutrino as-trophysics. Anisotropies of High-Energy Cosmic Rays CosmologicalCompton-Gettingeﬁectandγ-rays diﬁuseextragalacticγ-raybackgroundiscalorimeterfor el-mag.
HEenergyinjection MichaelKachelrie AnisotropiesofExtragalacticCRs. Small-scaleclustering Medium-scaleanisotropies Dipoleanisotropy. cosmic rays (CRs) and anomalous cosmic rays (ACRs). The origin of the ACRs is briefly discussed with emphasis on their acceleration in the outer heliosphere.
The causes of the CR cycles are reviewed, with emphasis on the year and year cycles, step modulation, charge-sign dependent modulation and particle drifts. The. Abstract We have made a new analysis of cosmic-ray data from the CRS experiment on the Voyager 2 (V2) spacecraft.
This analysis, which includes both penetrating and stopping particles in the HET telescope, extends the energy range from an upper energy limit of MeV nucleon-1 for stopping particles to over 1 GeV nucleonThis analysis provides almost continuous spectra over this broad.
Evolution of the energy spectra of anomalous cosmic rays in the outer heliosphere ( (v.2)) by Stone, Edward C: Detection of VHE gamma-rays from Mrk with the CAT imaging telescope ( (v.3)) by Punch, M: Results from the CACTI experiment: Air Cherenkov & particle measurements of PeV air showers at Los Alamos ( (v.5)) by.
In the outer heliosphere the ion population in the energy range to 30 MeV/nucleon may contain contributions from interplanetary acceleration, remnants of large solar energetic particle events, and the anomalous cosmic ray component (ACRs). Observations from the Voyager 1 and 2 Low Energy Charged Particle (LECP) instruments indicate that the ACR.
The Heliospheric Physics Laboratory develops instruments and models to investigate the origin and evolution of the solar wind, low-energy cosmic rays, and the interaction of the Sun's heliosphere with the local interstellar medium.
The Laboratory designs and implements unique multimission and multidisciplinary data services to advance NASA's solar-terrestrial program and our understanding of.
An inter-comparison of the first two harmonics has been made so as to understand the basic reason for the occurrence of cosmic ray anisotropies during the period and – using the Neutron monitor data from and Haleakala Neutron Monitoring Stations.
The annual average values of the first two (daily) harmonic amplitudes and phases for neutron monitor data due to the change in. different energies of cosmic rays [Alanko et al., ].  For many purposes it is important to know the differential energy spectrum of cosmic rays and its temporal variations.
For example, the direct use of a linear relation between the energy-integrated cosmic ray flux and solar activity may lead to large uncertainties in long-term studies. The propagation of high-energy cosmic rays (CRs) through giant molecular clouds constitutes a fundamental process in astronomy and astrophysics.
The diffusion of CRs through these magnetically turbulent environments is often studied through the use of energy-dependent diffusion coefﬁcients, although these are not always well.
thick. One can ﬁgure out the diffusion coefﬁcient of cosmic rays in the Galactic magnetic ﬁeld is very large, in the order of j ism ¼ cm2s 1 for cosmic rays of 1GeV (see, e.g., Ginzburg and Syrovatsky,2 Strong and Moskalenko,3 Ptuskin,4 Busching and Potgieter5).
If the cosmic rays in the vicinity of the solar system are represented. Study of High Energy Cosmic Ray Anisotropies with Solar and Geomagnetic Disturbance Index.
Figure 4. Shows the crossplot between the yearly mean Ap index vs. first harmonic (diurnal variation) annual average phase (hours) for Kiel as well as for Haleakala, for the period for Kiel and 19 for Haleakala. Figure 5. A team of scientists from Russia and China has developed a model explaining the nature of high-energy cosmic rays (CRs) in our galaxy.
These. We present initial results from our new 2-D, self-consistent model of galactic cosmic rays in the heliosphere.
This work can be viewed as an extension of a number of self-consistent 1-D models reported by several authors during the past years. Even in 1-D models, cosmic rays have a signiﬁcant impact in the outer heliosphere,Cited by: Mysteries of the Sun The heliosphere is the outer atmosphere of the Sun and marks the edge of the Sun’s magnetic influence in space.
The solar wind that streams out in all directions from the rotating Sun is a magnetic plasma, and it fills the vast space between the planets in our solar sys tem.
Cosmic rays beyond the boundary of the heliosphere V. Florinski 1. Introduction The heliopause is a pressure equilibrium boundary of the heliosphere, a giant “bubble” in space ﬁlled with plasma from the sun and surrounded by the cold and relatively dense interstellar : Vladimir Florinski, Edward Stone, Alan Cummings, Jakobus le Roux.
Oct. 13, — Cosmic rays of very high energy have their origin outside of our own galaxy, the Milky Way. This is suggested by a study of the .Solar gamma rays and modulation of cosmic rays Elena Orlando more difﬁcult to analyze was not the subject of that study.
Preliminary results of the on-going analysis of the two components of the solar emission have been presented in . The gamma-ray ﬂux from the Sun was evaluated using Pass 8 Author: Elena Orlando, Nicola Giglietto, Igor Moskalenko, Silvia Raino, Andrew W. Strong.Solar Cycle in the Heliosphere and Cosmic Rays Fig.
2 Heliolatitudinal distribution of the daily solar wind velocities measured by Ulysses spacecraft (data from OMNIweb). The upper (blue dots)andlower (red dots) panels are built for the solar minimum (– and –) and solar maximum (, –) conditions, respectively.