Primary electrons and positrons in the cosmic radiation.
Electron-positron components of primary cosmic radiation, noting energy spectrum, flux, charge composition, origin, etc
PRIMARY COSMIC RADIATION↗
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The flux and energy spectrum of primary cosmic ray electrons.
Flux and energy spectrum of primary electron component measured by balloon at period near solar activity minimum
ELECTRON FLUX↗
Measurements of the primary proton and helium spectra and their modulations using a balloon- borne Cerenkov-scintillation counter.
Balloon-borne Cerenkov scintillation counter for measurements of primary proton and helium spectra and modulations
CERENKOV COUNTER↗
Some implications of the relative spectra of the different charge components in the primary radiation.
Differential spectra of charge components of primary cosmic ray heavy nuclei at different solar modulation levels and effects of interstellar propagation
PARTICLE↗
The flux of heavy nuclei in the primary cosmic rays over Texas in March 1962, and the solar cycle modulation
Flux of heavy nuclein primary cosmic radiation and solar cycle modulation
SOLAR CYCLE↗
Observations of nuclei heavier than iron in the primary cosmic radiation
Charge and energy spectra of primary cosmic rays made with large area Cerenkov scintillation counter on baloon flights - heavier than iron nuclei
SPECTRAL ENERGY DISTRIBUTION↗
Measurement of the Energy Spectrum of Primary Cosmic Rays in the Energy Region from 1010 - 1014 EV with the Help of AES Proton-1
AES Proton I measurement of primary cosmic ray energy spectrum in high energy range
PROTON I SATELLITE↗
Estimates of primary and secondary particle doses behind aluminum and polyethylene slabs due to incident solar-flare and Van Allen belt protons
Primary and secondary particle radiation doses shielded from solar flare and Van Allen belt protons by aluminum and polyethylene slabs
PROTON↗
Determination of the Fragmentation Parameters of the Multi-charge Component of Primary Cosmic Rays
Determination of fragmentation parameters of multicharge component of primary cosmic rays
NUCLEAR EMULSION↗
The antiproton component of the primary cosmic ray flux
Solution of Fokker-Planck diffusion equation in intensity prediction of antiproton component of primary cosmic ray flux
FOKKER-PLANCK EQUATION↗
High-energy primary electrons and the universal blackbody radiation.
High energy primary electrons and universal body radiation
PRIMARY COSMIC RADIATION↗
Energy spectrum and geomagnetic cut-off of primary cosmic-ray alpha-particles near 41 deg N mag.
Energy spectrum of primary cosmic ray alpha particles measured by nuclear photographic emulsion, estimating geomagnetic cut-off energies
ENERGY SPECTRUM↗
Observations on nuclei heavier than iron in the primary by cosmic radiation.
Primary cosmic radiation abundance measurements on iron and heavier nuclei, using Cerenkov counter on balloon flights
CERENKOV COUNTER↗
The primary cosmic-ray electron spectrum near solar minimum.
Primary cosmic ray electron flux and energy spectrum near solar minimum compared with nonthermal radio emission from high galactic latitudes
SOLAR CYCLE↗
An apparently high flux of primary cosmic-ray He-nuclei at 41 deg N mag.
Unexpected excess of primary cosmic ray helium nuclei flux value in nuclear photographic emulsions
HEAVY NUCLEUS↗
The intensity of heavy nuclei in the primary cosmic rays over Texas in March 1962 and the solar cycle modulation.
Heavy nuclei intensity in primary cosmic rays, long term solar cycle modulation and time lag in various phases
SOLAR CYCLE↗
Fabrication and Testing of a Large Active Primary Reflector
This paper discusses the fabrication considerations and proposed testing concepts for a twelve meter, graphite-epoxy space truss that is being developed to provide structural support for the primary mirror system of the SpacE Laser ENErgy Beam Transmission Optical System.
primary mirror↗
High-degree Gravity Models from GRAIL Primary Mission Data
We have analyzed Ka‒band range rate (KBRR) and Deep Space Network (DSN) data from the Gravity Recovery and Interior Laboratory (GRAIL) primary mission (1 March to 29 May 2012) to derive gravity models of the Moon to degree 420, 540, and 660 in spherical harmonics. For these models, GRGM420A, GRGM540A, and GRGM660PRIM, a Kaula constraint was applied only beyond degree 330. Variance‒component estimation (VCE) was used to adjust the a priori weights and obtain a calibrated error covariance. The global root‒mean‒square error in the gravity anomalies computed from the error covariance to 320×320 is 0.77 mGal, compared to 29.0 mGal with the pre‒GRAIL model derived with the SELENE mission data, SGM150J, only to 140×140. The global correlations with the Lunar Orbiter Laser Altimeter‒derived topography are larger than 0.985 between l = 120 and 330. The free‒air gravity anomalies, especially over the lunar farside, display a dramatic increase in detail compared to the pre‒GRAIL models (SGM150J and LP150Q) and, through degree 320, are free of the orbit‒track‒related artifacts present in the earlier models. For GRAIL, we obtain an a posteriori fit to the S‒band DSN data of 0.13 mm/s. The a posteriori fits to the KBRR data range from 0.08 to 1.5 micrometers/s for GRGM420A and from 0.03 to 0.06 micrometers/s for GRGM660PRIM. Using the GRAIL data, we obtain solutions for the degree 2 Love numbers, k20=0.024615+/-0.0000914, k21=0.023915+/-0.0000132, and k22=0.024852+/-0.0000167, and a preliminary solution for the k30 Love number of k30=0.00734+/-0.0015, where the Love number error sigmas are those obtained with VCE.
Primary 1↗