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Ramaty, R.

Publications and source records attributed to Ramaty, R..

At least 199 records · Page 11
All sourcesNASA NTRSDOE OSTI
NASA NTRS1972

Interstellar electron intensity

Two independent methods for measuring the electron intensity in interstellar space are proposed. The positron method involves the production of pions in proton-proton collisions, the decay of the pions into muons, and the subsequent decay of the muons into positrons. Results from detailed calculations of these processes are given in graphical form. The second method involves cosmic electron emitted synchrotron radiation in the interstellar magnetic field. These two methods are also used to analyze the spatial and temporal constancy of cosmic ray electrons in the galaxy.

Ramaty, R.↗
NASA NTRS1971

Origin of cosmic electrons from about 100 to 1,000,000 GeV.

The origin of high-energy cosmic electrons is considered. It is found that electrons of energies below 1000 GeV could have been produced by local supernovae associated with known radio remnants. At higher energies, observations of muon-poor air showers indicate the existence of electrons at 1,000,000 GeV which may have originated entirely from the supernova Vela X.

Ramaty, R.↗
NASA NTRS1971

Cosmic-ray effects in the Gum nebula

The effects of low energy heavy nuclei from the supernova explosion on nearby interstellar space were investigated. In addition to the ionization and heating of the Gum nebula, these particles may produce detectable fluxes of X-rays and gamma rays, both as continuum radiation and line emission.

Ramaty, R.↗
NASA NTRS1971

Cosmic ray effects in the Gum Nebula

Ionization of Gum nebula by energetic charged particles from supernova Vela X with estimate of gamma ray line emission from ambient gas, energetic nuclei interaction

Boldt, E. A.↗
NASA NTRS1971

The effects of propagation and source distribution on cosmic ray composition and anisotropy.

We consider the propagation and source distribution of cosmic rays. The principal requirement for the various models we consider is that they should be capable of holding particles in dense regions of the galactic disk for periods of time sufficient to produce the observed fragmentation products of cosmic rays. This can be achieved by both simple and compound diffusion provided that suitable mean free paths and boundary conditions are chosen. The bulk of the anisotropy is caused by the discrete nature of the cosmic ray sources. However, models which reproduce the fragmentation products will in general yield anisotropies consistent with available upper limits.

Ramaty, R.↗