Radio astronomy
Radio astronomy studies in 18-cm line emission sources, fringe visibility of bright radio sources, and spectral features of Venus and Jupiter
INTERFEROMETRY↗
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Radio astronomy
Radio astronomy - millimeter and microwave techniques and observations
MILLIMETER WAVE↗
Radio astronomy
Radio astronomy - Haystack-Millstone OH INTERFEROMETER, K-band spectrum measurements of sun, inference of atmospheric attenuation from balloon flights, and microwave emission
RADIO ASTRONOMY↗
Radio astronomy
Radio astronomy techniques and telescopes, solar and galactic radio spectroscopy, and cosmic radio signal observations
RADIO SPECTROSCOPY↗
The Radio JOVE Project - Shoestring Radio Astronomy
Radio JOVE is an education and outreach project intended to give students and other interested individuals hands-on experience in learning radio astronomy. They can do this through building a radio telescope from a relatively inexpensive kit that includes the parts for a receiver and an antenna as well as software for a computer chart recorder emulator (Radio Skypipe) and other reference materials
Thieman, J.↗
Radio astronomy
Radio astronomical studies of microwave spectrum, radial velocity, dielectric constants, and emissions
MICROWAVE SPECTRUM↗
Radio Astronomy
Radio astronomical studies in OH interferometry, discrete radio sources, and spectrum measurements of Venus and Jupiter
SPECTRAL EMISSION↗
Mission and Design of an Orbiting Radio Astronomy Explorer
Radio Astronomy Explorer /RAE/ satellite for measuring intensity of radio signals from celestial sources
ASTRONOMICAL OBSERVATORY↗
The Helios radio astronomy experiment
Radio bursts traveling between the Sun and the Earth were tracked by radio astronomy experiments on Helios 1 and 2. A relatively short dipole antenna with a well-defined toroidal reception pattern was flown. The antenna spins in the ecliptic at 60.3 rpm and 2 frequencies are measured in each revolution. The signal analysis determines the strength of the signal, the direction of the source in the ecliptic, and the degree of modulation, and estimates source size. The experiments provide three-dimensional direction finding in space. They extend the radio frequency window beyond what is observable on Earth, and offer a long triangulation baseline.
Kayser, S.↗
Space radio astronomy
Space radio astronomy, discussing frequency range in terrestrial atmosphere, RAE-1 satellite, cosmic and solar emissions and magnetopause generation, propagation and absorption processes
Stone, R. G.↗
The Astronomical Low Frequency Array: A Proposed Explorer Mission for Radio Astronomy
A radio interferometer array in space providing high dynamic range images with unprecedented angular resolution over the broad frequency range from 0.030 - 30 MHz will open new vistas in solar, terrestial, galactic, and extragalactic astrophysics.
radio astronomy VLBJ interferometry explorer missi↗
Radio Astronomy, Planetary
Planetary radio astronomy is the study of the physical characteristics of the planets in the Solar System by means of the electromagnetic radio radiation emitted by these objects.
Radio Astronomy Planets↗
Thunderstorms and ground-based radio noise as observed by radio astronomy Explorer 1
Radio Astronomy Explorer (RAE) data were analyzed to determine the frequency dependence of HF terrestrial radio noise power. RAE observations of individual thunderstorms, mid-ocean areas, and specific geographic regions for which concommitant ground based measurements are available indicate that noise power is a monotonically decreasing function of frequency which conforms to expectations over the geographic locations and time periods investigated. In all cases investigated, active thunderstorm regions emit slightly higher power as contrasted to RAE observations of the region during meteorologically quiet periods. Noise levels are some 15 db higher than predicted values over mid-ocean, while in locations where ground based measurements are available a maximum deviation of 5 db occurs. Worldwide contour mapping of the noise power at 6000 km for five individual months and four observing frequencies, examples of which are given, indicate high noise levels over continental land masses with corresponding lower levels over ocean regions.
Caruso, J. A.↗
User friendly database for Neptune planetary radio astronomy observations
Planetary Radio Astronomy (PRA) data from the Voyager Neptune encounter were cleaned and reformatted in a variety of formats. Most of these formats are new and have been specifically designed to provide easy access and use of the data without the need to understand esoteric characteristics of the PRA instrument or the Voyager spacecraft. Several data sets were submitted to the Planetary Data System (PDS) and have either appeared already on peer reviewed CDROM's or are in the process of being reviewed for inclusion in forthcoming CD-ROM's. Many of the data sets are also available online electronically through computer networks; it is anticipated that as time permits, the PDS will make all the data sets that were a part of this contract available both online and on CD-ROM's.
Evans, David R.↗
Radio Astronomy Explorer /RAE/. I - Observations of terrestrial radio noise.
Radio Astronomy Explorer (RAE) I data are analyzed to establish characteristics of HF terrestrial radio noise at an altitude of about 6000 km. Time and frequency variations in amplitude of the observed noise well above cosmic noise background are explained on the basis of temporal and spatial variations in ionospheric critical frequency coupled with those in noise source distributions. It is shown that terrestrial radio noise regularly breaks through the ionosphere and reaches RAE with magnitudes 15 dB and more above cosmic noise background, on frequencies above the F-layer critical frequency.
Herman, J. R.↗
Planetary radio astronomy receiver
The planetary radio astronomy (PRA) experiment on the Voyager spacecraft will measure the amplitude, spectrum, time variations, and polarization of radio emissions over a frequency range of 1.2 kHz to 40.5 MHz with the aid of the PRA receiver (PRAR) and two 10-m orthogonal monopoles. Sensitivity and dynamic range will allow observation of a wide range of Jovian emissions from near earth to encounter. This paper describes the system elements, including the preamp/attenuator/calibrator, the LF polarization discriminator, the four LF-IF amplifier stages, the HF polarization discriminator, the translation LO, the log-IF and detector, the frequency synthesizer, the data processor, control system, power supply, and antennas.
Lang, G. J.↗