Engineering Papers⌕ Search

SEARCH · Engineering Papers

Results for “heliosphere”

Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

Quote a phrase for an exact phrase match. Source license links do not imply unrestricted reuse.

At least 451 records · Page 25
All sourcesNASA NTRSDOE OSTI
NASA NTRS1977

Cosmic ray investigation for the Voyager missions: Energetic particle studies in the outer heliosphere - and beyond

The Voyager mission cosmic ray detector system, consisting entirely of solid-state charged-particle detectors, is designed to measure the energy spectrum of electrons in the range 3 to 110 MeV and the energy spectra and elemental composition of cosmic ray nuclei from hydrogen through iron in the range 1 to 500 MeV/nuc; for isotopes of hydrogen through sulfur the range is approximately 2 to 75 MeV/nuc. The cosmic ray investigation deals with the energy content, origin and acceleration process, and dynamics of cosmic rays in the galaxy, with particular attention given to low-energy phenomena in interstellar space and the outer solar system. The precise measurement of three-dimensional stream patterns of nuclei from H to Fe, as well as electrons over a wide energy range, is the data acquisition program emphasized.

Stone, E. C.↗
NASA NTRS1980

The corona and heliosphere

The eleven-year solar cycle is an especially appropriate period over which to study the solar output and its variation, because during this cycle most of the important types of solar variability (many characterized by periods shorter than eleven years) are manifested. Studies of solar variability over a solar cycle will improve understanding of solar structure and of the generation of the solar wind, and this improved understanding can be useful in the related studies of stellar structure and stellar winds, since stellar observations are necessarily less detailed and sophisticated than are solar observations. A particularly significant benefit that will accrue from a thorough study of the solar atmosphere and its variability over the next solar cycle is a great enhancement in the usefulness of so-called 'proxy' data in studying longer term solar variations and their terrestrial implication.

Holzer, T.↗
NASA NTRS1981

Simulation of the magnetic structure of the inner heliosphere by means of non-spherical source surface

A new method for mapping the Sun's magnetic field B from the photosphere through the corona and interplanetary space is presented. The method entails the derivation of B from a scalar potential within a current-free annular volume bounded inside by photosphere and outside by a prescribed nonspherical source surface to which B is made (as nearly as possible) perpendicular. As usual we obtain the potential for the part of B that arises from currents inside the Sun by fitting an expansion to the observed line-of-sight component of B at the photosphere. A second least-squares fit is introduced to obtain the part of B that arises from currents outside the source surface. Comparisons are made between this model and observed coronal and interplanetary structures. There is evidence that observation data underestimate the strength of photospheric polar magnetic fields.

Levine, R. H.↗
NASA NTRS1980

Galactic cosmic ray observations in the distant heliosphere

The energy spectra and radial gradient of galactic cosmic ray hydrogen and helium have been measured between 1 and 15 AU for two time intervals in 1977 using Pioneers 10, 11 and Helios I, II. The observed gradients decrease with increasing heliocentric distance. Above 1 GV the observations are consistent with conventional modulation theory. At low energies the apparent energy loss for low rigidity hydrogen and helium appears to be appreciably smaller than expected. Alternate approaches are discussed.

Mcdonald, F. B.↗
NASA NTRS1981

Numerical study of solar flare particle propagation in the heliosphere

Numerical solutions are presented for the propagation of solar cosmic rays in interplanetary space, including the effects of pitch-angle scattering and adiabatic focusing. The intensity-time profiles can be well fitted by a simple radial spatial diffusion equation. For low-rigidity particles the radial mean free path so obtained is significantly larger than the mean free path calculated from the scattering coefficient due to the inapplicability of the diffusive approximation early in the event. The well-known discrepancy between the scattering mean free path and the theoretical predictions may be resolved by these calculations.

Gombosi, T. I.↗
NASA NTRS1981

Solar wind helium and hydrogen structure near the heliospheric current sheet - A signal of coronal streamers at 1 AU

Solar wind flow properties associated with very low helium to hydrogen abundance ratios have been observed with Los Alamos instruments on IMP 6, 7, and 8 during 1971-1978. A characteristic pattern has been discovered consisting of correlated interplanetary field reversals, high plasma density, low and nearly identical H(+) and He(2+) bulk velocities, low H(+) and He(2+) kinetic temperatures, and minima in their ratios. Because coronal streamers straddle the current sheet close to the sun, the pattern discovered is the 'signal' of a coronal streamer at 1 AU. A superposed epoch analysis of 74 well-defined sector boundary crossings provides verification of the above correlation featuring a pronounced minimum in the helium to hydrogen abundance ratio at the sector boundary passage.

Borrini, G.↗
NASA NTRS1981

Energetic storm particle events in the outer heliosphere

The evolution of energetic particle events with increasing heliocentric distance is studied through events of Pioneers 10 and 11. Beyond 12 AU the events become the dominant type of solar particle event at 1 AU, and the combined effects of adiabatic cooling and volume expansion rule out the possibility that the particles represent the confinement of the original particle population behind the shock. It is not established whether the particles originate from the solar wind by injection via post-shock enhancements or are energetic solar particles further energized by the shock, although their very long lifetime favors the solar wind origin.

Mcdonald, F.↗
NASA NTRS1982

The galactic cosmic-ray radial intensity gradient and large-scale modulation in the heliosphere

Measurements of fluxes from 1 AU on the IMP 8 satellite to 11 AU on the Pioneer 11 and to greater than 24 AU on the Pioneer 10 spacecraft show that the nucleon integral gradient is a function of the level of the approximately 11-year solar modulation cycle. The gradient decreases from approximately 4.5% to 1.5% throughout the solar minimum of 1975-1977, and increases to approximately 2.5-3.0% per AU near maximum modulation. Pioneer 10 at greater than 24 AU is still deep in the modulation region, leading to estimates of 50-70 AU for the radial distance to the heliopause at both solar minimum and solar maximum modulation.

Mckibben, R. B.↗
NASA NTRS1982

Observations of the flow pattern of low-energy galactic cosmic rays in the outer heliosphere

The investigation is based on data obtained with the aid of Pioneer 10. The experimental observations of low-energy cosmic-ray anisotropies are presented for the period November 8, 1976 to December 15, 1977 when Pioneer 10 was at its maximum radial distance (11.5-14.7 AU) during the period of solar minimum conditions at the end of cycle 20. The azimuthal anisotropies obtained by integrating over this complete period are summarized in a table. For 30-56-MeV protons, a value of 7.4 plus or minus 2 percent in a direction of 110 deg is obtained. This direction is close to the 90 deg value expected from corotation or for particles flowing inward along the nominal filed line. The value obtained for helium is consistent with the value for hydrogen. There was no measureable flow for the 10-22-MeV/nuc anomalous helium. Attention is given to details of instrumentation and questions regarding the statistical significance of the data.

Mcdonald, F. B.↗
NASA NTRS1982

Theoretical analysis of low-energy proton and helium anisotropies in the outer heliosphere

Expressions for streaming components are considered along with aspects of azimuthal anisotropy, taking into account a calculation of mean free paths and a comparison with corotation conditions. Questions of polar anisotropy are also taken into account. It is found that the azimuthal anisotropy of 30 - 56 MeV protons near the ecliptic plane at 12 AU in 1977 was consistent with corotation, or slightly faster. This implies that the mean free path is approximately 16 AU. The azimuthal anisotropy of the anomalous 10-21 and 30 - 56 MeV/nucleon helium at the same time and place was an order of magnitude less than the corotation value. This implies a mean free path of approximately 5 AU.

Forman, M. A.↗