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Salpeter, E. E.

Publications and source records attributed to Salpeter, E. E..

At least 37 records · Page 2
All sourcesNASA NTRSDOE OSTI
NASA NTRS1986

Moderate resolution spectroscopy for the Space Infrared Telescope Facility (SIRTF)

A conceptual design for an IR spectrometer capable of both low resolution (lambda/Delta-lambda = 50; 2.5-200 microns) and moderate resolution (1000; 4-200 microns) has been developed. This instrument will allow the spectroscopic study in the infrared of objects ranging from within the solar system to distant galaxies. The spectroscopic capability provided by this instrument for SIRTF will give astronomical orders of magnitude greater sensitivity for the investigation of faint objects than has been previously available.

Houck, J. R.↗
NASA NTRS1986

Moderate resolution spectroscopy for the Space Infrared Telescope Facility (SIRTF)

The conceptual design presented for a low-to-moderate resolution IR spectrometer is expected to allow the spectroscopic study of objects whose location ranges from within the solar system to distant galaxies, with far greater sensitivity than previously available for the study of faint objects. The low resolution mode will allow detailed continuum radiation studies to be conducted, while the moderate resolution mode will facilitate studies encompassing the IR spectral signatures of small outer solar system bodies and the nature of more luminous active galaxies and QSOs at greater distances. The five spectrometer modules share a common aperture, and all gratings share a single scan mechanism. All heat sources other than the detectors operate at 7 K and are separated from the 4 K cold station. Two-dimensional area detector arrays are used in the 2.5- to 120-micron bands to simultaneously monitor adjacent regions in extended objects and to measure the background near point sources.

Houck, J. R.↗
NASA NTRS1985

H I properties of dwarf irregular galaxies in the Virgo Cluster

A neutral hydrogen survey was carried out at Arecibo on 91 dwarf irregular galaxies, with morphological types Sdm through Im, in and around the direction of the Virgo Cluster. Only nine of these were found to be background galaxies, and 19 remain undetected, i.e., most of the candidate galaxies are indeed members of the Virgo Cluster or Supercluster. The distribution of positions and systemic velocities (compared with large spirals) shows no evidence for mass segregation. The H I depletion for dwarfs in the cluster core is only moderate, no more than for spirals. The magnitude-velocity width correlation is continous from spirls to dwarfs. Satistics on H I masses agree only partially with a simple stochastic star formation model.

Hoffman, G. L.↗
NASA NTRS1979

Distribution and composition of interstellar matter

Some of the problems associated with the observation of interstellar matter are described. The characteristics of the high resolution spectrograph are summarized and observations of matter distribution are given.

Salpeter, E. E.↗
NASA NTRS1977

The phase diagram and transport properties for hydrogen-helium fluid planets

The properties of pure hydrogen and helium are examined, taking into account metallic hydrogen, molecular hydrogen, and the molecular-metallic transition. Metallic hydrogen-helium mixtures are considered along with molecular hydrogen-helium mixtures, the total phase diagram, and minor constituents, including deuterium. The transport properties of the metallic and the molecular phase are also discussed, giving attention to electrical conductivity, thermal conductivity, viscosity, self-diffusion, interdiffusion, radiative opacity, and second-order transport coefficients.

Stevenson, D. J.↗
NASA NTRS1977

The dynamics and helium distribution in hydrogen-helium fluid planets

The simple case of a homogeneous planet without first-order phase transitions is considered and an investigation is conducted concerning a pure hydrogen planet in which a first-order phase transition takes place from fluid molecular hydrogen to fluid metallic hydrogen. Attention is also given to convection in the presence of a compositional gradient, the effects of helium insolubility in a cooling hydrogen-helium planet, a hydrogen-helium planet in its early evolution, and the case in which influence of phase transition occurs much later in the evolution of the planet.

Stevenson, D. J.↗
NASA NTRS1976

Particles, environments, and possible ecologies in the Jovian atmosphere

The possible existence of indigenous Jovian organisms is investigated by characterizing the relevant physical environment of Jupiter, discussing the chromophores responsible for the observed coloration of the planet, and analyzing some permissible ecological niches of hypothetical organisms. Values of the eddy diffusion coefficent are estimated separately for the convective troposphere and the more stable mesosphere, and equilibrium condensation is studied for compounds containing Na, Cl, or both. The photoproduction of chromophores and nonequilibrium organic molecules is analyzed, and the motion of hypothetical organisms is examined along with the diffusion of metabolites and the consequent growth of organisms. Four kinds of organisms are considered: primary photosynthetic autotrophs ('sinkers'), larger autotrophs or heterotrophs that actively maintain their pressure level ('floaters'), organisms that seek out others ('hunters'), and organisms that live at almost pyrolytic depths ('scavengers'). It is concluded that ecological niches for sinkers, floaters, and hunters appear to exist in the Jovian atmosphere.

Sagan, C.↗
NASA NTRS1976

Particles, environments and possible ecologies in the Jovian atmosphere

The eddy diffusion coefficient is estimated as a function of altitude, separately for the Jovian troposphere and mesosphere. Complex organic molecules produced by the Ly alpha photolysis of methane may possibly be the absorbers in the lower mesosphere which account for the low reflectivity of Jupiter in the near ultraviolet. The optical frequency chromophores are localized at or just below the Jovian tropopause. Candidate chromophore molecules must satisfy the condition that they are produced sufficiently rapidly that convective pyrolysis maintains the observed chromophore optical depth. The condition is satisfied if complex organic chromophores are produced with high quantum yield by NH3 photolysis at less than 2,300 A. Jovian photoautotrophs in the upper troposphere satisfy this condition well, even with fast circulation, assuming only biochemical properties of comparable terrestrial organisms. An organism in the form of a thin, gas filled balloon can grow fast enough to replicate if (1) it can survive at the low mesospheric temperatures, or if (2) photosynthesis occurs in the troposphere.

Sagan, C.↗
NASA NTRS1976

Heat transport in a stratified two-phase fluid

A self-gravitating fluid, stratified into two phases of appreciably different densities and heated from within is considered. The heat flux, viscosity, and thermal diffusivity are assumed to be small enough so that, away from the interface between the phases, the flux is mainly carried by turbulent convection with a very small superadiabaticity. Different modes are investigated for transporting the heat flux across the interface, and both possible signs of the latent heat L are considered. A thermal boundary layer, distortion of the interface, and the nucleation, growth and motion of droplets and bubbles are included. It is shown that, under a specified range of conditions, the transition region near the interface is thin with a small change in the temperature T across it. The entropy difference between the two phases is then L/T. These considerations probably apply to the interior of Jupiter.

Salpeter, E. E.↗
NASA NTRS1976

Interior models of Jupiter

Understanding the interior of Jupiter depends upon our knowledge of the thermodynamics and transport properties of hydrogen-helium mixtures at high pressures and temperatures. The current status of this knowledge is reviewed, and attention is given to the metallic-molecular hydrogen transition and the limited solubility of helium in hydrogen. Models of Jupiter are constructed which are consistent with all the observations to date, but which make various assumptions about the thermodynamics and composition of the interior. These models typically consist of a rocky core surrounded by a nearly-solar fluid mixture. In contrast to the models of Podolak and Cameron, a large enhancement of water or helium is not found to be essential. It is concluded that further progress in constructing interior models requires a better understanding of the thermodynamics of dense molecular hydrogen.

Stevenson, D. J.↗
NASA NTRS1973

On convection and gravitational layering in Jupiter and in stars of low mass.

Neutral helium is probably insoluble in metallic hydrogen below some critical temperature. When Jupiter has cooled sufficiently, helium droplets can form, grow, and fall under gravity, leading to chemical separation and gravitational layering in spite of rapid convection. Applications to cool stars are discussed.

Salpeter, E. E.↗
NASA NTRS1973

Interpretation of far infra-red emission from interstellar grains

Application of the Kramers-Kronig relations to grains in the interstellar medium. It is found that the recent UV, visual, and infrared extinction curves provide marginal evidence against silicates as the major cause of this extinction. In the far infrared, grains contribute little to the extinction, but can be observed in thermal emission. It is shown that the far infrared emission from grains in a given bandwidth sets a lower limit to the grain temperature. From observed intensities from the galactic plane at 100 microns and from Orion at 350 microns, minimum grain temperatures are found which are larger than the observed brightness temperature. The emission and extinction data can be used together to constrain the allowable range of parameters for the grains.

Caroff, L. J.↗