2 edition of A measurement of the energy spectra of cosmic rays from 20 to 1000 GeV per AMU found in the catalog.
A measurement of the energy spectra of cosmic rays from 20 to 1000 GeV per AMU
by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va
Written in English
|Statement||Dr. John C. Gregory, principal investigator, Dr. Arthur Smith, co-investigator.|
|Series||[NASA contractor report] -- NASA CR-195246., NASA contractor report -- NASA CR-195246.|
|Contributions||Gregory, John C., Smith, Arthur., United States. National Aeronautics and Space Administration.|
|The Physical Object|
Abstract. The solar modulation of galactic cosmic rays (GCR) can be studied in detail by examining long-term variations of the GCR energy spectrum (e.g. on the scales of a solar cycle).With almost 20 years of data, the Electron Proton Helium INstrument (EPHIN) onboard the SOlar and Heliospheric Observatory (SOHO) is well suited for this kind of Cited by: Cosmic rays are high-energy protons and atomic nuclei which move through space at nearly the speed of originate from the sun, from outside of the solar system, or even from distant galaxies. Upon impact with the Earth's atmosphere, cosmic rays can produce showers of secondary particles that sometimes reach the from the Fermi Space Telescope .
Fitting Energy Spectrum to Astrophysical Models 22 Study of the Declination Dependence of the Energy Spectrum 24 6 Conclusions and Outlook 26 1 Introduction The origin of cosmic rays (CRs) is an important problem in modern astrophysics. Extrater-restrial particles of energies greater than and even exceeding eV are measured. Fermi-LAT electron spectrum from 20 GeV to 1 TeV 9Cited 38 times within a month 9APS Viewpoint Phys. Rev. Letters , () Total statistics collected for 6 months of Fermi LAT observations: > 4 million electrons above 20 GeV > electrons in last energy bin ( GeV).
Abstract New results are described on the energy spectra and relative abundances of primary cosmic ray nuclei from carbon to iron. The measurement was performed on the Spacelab-2 mission of the Space Shuttle Challenger in , and extends to energies beyond 1 TeV per amu. Motivation Motivation • Pamela,ATIC,H.E.S.S. and PPB-BETS report deviations from model. – Pamela: an increase e + with respect to e-+e + at energy above a few GeV – ATIC,PPB-BETS: prominent spectral feature at around GeV in the total e-plus e + spectrum 3 – H.E.S.S: significant steeping of the spectrum above GeV →These indicate the presence of a .
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Get this from a library. A measurement of the energy spectra of cosmic rays from 20 to GeV per amu: final report on NASA grant NAGW [J C Gregory; United States. National Aeronautics and Space Administration.;]. Get this from a library. A measurement of the energy spectra of cosmic rays from 20 to GeV per amu: semiannual report.
[J C Gregory; United. A measurement of the energy spectra of cosmic rays from 20 to GeV per amu by J. Gregory,University of Alabama in Huntsville, National Aeronautics and Space Administration edition, Microform in English.
A Measurement of the Energy Spectra of Cosmic Rays from 20 to GeV Per Amu Summary of Program The original BUGS4 instrument was designed and partly built in Bristol (United Kingdom) in the 's. In it was shipped to the University of Alabama in Huntsville, Alabama, where it was completely refurbished, calibrated and prepared for flight.
2 Energy spectrum Thus, the cosmic ray energy spectrum extends, amazingly, for more than eleven orders of magnitude. All along this vast energy span, the spectrum follows a power law of index ∼ Therefore, the CR ﬂux decreases approxi-mately 30 orders of magnitude from ∼ m 2sec−1 at few GeV to ∼ 1 km− per century at EeV.
The IceCube Collaboration publishes today a new measurement of the all-particle cosmic ray energy spectrum in the energy range from PeV to EeV using data from IceTop, the surface component of the IceCube Neutrino Observatory.
The measured spectrum exhibits clear deviations from power law behavior. dividual energy spectra of the major primary cosmic-ray nuclei from oxygen (Z = 8) to iron (Z = 26), covering the energy range from ∼1 GeV amu−1 to several TeV amu−1.
In total en-ergy, the measurement reached energies well above eV for the more abundant species. The results from this ﬂight indicate. The individual energy spectra for the major elements (O, Ne, Mg, Si and Fe) extend from GeV/amu to several GeV/amu and for S, Ar and Ca from GeV/amu to GeV/amu. These results represent the highest energies for which spectral measurements with individual charge resolution have been reported.
In terms of total energy per. The differential energy spectrum of the electron component has been determined in the momentum interval between and GeV/c.
This spectrum can be described by two power laws, one below MeV with a spectral index of −± and the other above this energy with an index of −±Cited by: Most galactic cosmic rays have energies between MeV and 10 GeV. If those cosmic rays are protons, which they are most of the time, they are traveling at speeds between 45% and % of the speed of light.
Lower energy cosmic rays, which are the most abundant, are usually studied with small detectors in balloons and satellites. On the left. composition and the energy spectra of cosmic rays from hydrogen to iron over the energy range eV in a series of ﬂights (Seo et al.
Sincefour instruments were successfully ﬂown on long-duration balloons in Antarctica. The instrument conﬁgurations varied slightly in each mission due to various detector upgrades. arXivv1  2 Jul PROCEEDINGS OF THE 31st ICRC, Ł OD´ Z ´ 1 Measurement of the Cosmic Ray e++e− spectrum from 20 GeV to 1 TeV with the Fermi Large Area Telescope L.
Latronico∗ for the Fermi LAT Collaboration ∗Istituto Nazionale di Fisica Nucleare, Sezione di Pisa, I Pisa, Italy Abstract. ELEMENTAL SPECTRA Elemental intensities in seven energy bins, corresponding to cosmic rays stopping in each of the detectors E2–E8, for the – solar minimum are given in Appendix B in Table 6.
These data are plotted in Figure 3, where we have applied arbitrary energy-independent scale factors to allow for / = 20). The flux of cosmic rays at the top of the atmos phere is given in Table I (2). The attenuation meam free path is about gm/cm2, and the spectrum is given by: ∫Eo ∞ N (E) dE ∞ E °-1,67 At mountain top elevations and for energies above GeV the ratio of pions to nucleons at a given energy is about 20 - 30%, although.
New results on the energy spectra of the cosmic-ray nuclei boron, carbon, nitrogen, and oxygen up to energies around 1 TeV per amu are described.
The measurements were performed on. The elements _(18)Ar and _(20)Ca, which at a few GeV per amu are mixtures of primary and secondary components, display abundances relative to. balloon ﬂight (LDB) in Antarctica. The measurement included eight primary cosmic-ray species from oxygen to iron up to energies of GeV and even higher for the more abundant nuclei.
The observed energy spectra are shown in ﬁgure 1. More details on this measurement are given in . Fig. Energy spectra measured with TRACER in GeVamu 1, solar modulation obscures the interstellar energy spectra, and beyond GeV amu 1, the propagation path length is unknown.
Beyond GeV amu 1, even for the primary nuclei, at most the energy spectra of groups of ele-ments have been determined in direct measurements above the atmosphere (Takahashi et al. ; Apanasenko et al. Cosmic-ray Energy Spectrum»»» shows where students could discuss/think about a topic/concept.
shows where an activity is introduced.»»» IceTop is a cosmic-ray detector. It is an array of instruments that observe the air showers of secondary particles created by cosmic rays when they interact with the Earth’s atmosphere.
4 A. KARELIN et al. MEASUREMENT OF CR PROTONS ENERGY d= GeV/mip3. 0 20 40 60 80 0 E, GeV Etot/Estr, mip Fig. 8: The initial energy of primary proton E (GeV) as function of mean value of Etot/Estr (mip) IV. CONCLUSION The method of measurement of cosmic ray proton energy with electromagnetic calorimeter of.
For high latitude anomalous cosmic ray (ACR) component has also a significant influence on the atmospheric ionization. We propose an empirical model for differential spectra D(E) of galactic and anomalous cosmic rays in energy interval 1 MeV– GeV during solar cycle.
In the model data are used which cover three solar cycles: 20, 22 and Cited by: 7.An instrument designed to measure elemental cosmic ray abundances from boron to nickel in the energy region – GeV nucl −1 was flown on a high altitude balloon from Sioux Falls, South Dakota, on 30 September through 1 October at an average atmospheric depth of ∼5 g cm −ential energy spectra of B, C, N, O, Ne, Mg, Si and Fe, extrapolated to the top of the Cited by: 2.30 TH INTERNATIONAL C OSMIC R AY C ONFERENCE Measurement of Cosmic Ray Neutron Spectra in the Energy Region of MeV at the Summit of Mauna Kea and Several Different Altitudes R YOZO T AKASU 1, Y OSHIHARU T OSAKA 1, H IDEYA M ATSUYAMA 2, H IDEO E HARA 2, Y UJI K ATAOKA 1, A TSUSHI K AWAI 3, M ASAHIKO H AYASHI 3, AND Y .