Can the redshifts of quasi-stellar objects be gravitational?
Quasar models examined for gravitational red shift
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Quasar models examined for gravitational red shift
Absorption red shifts in quasar spectra from spectroscopic observations of PHL 5200 and B194
Bolometric luminosity-red shift relations of Friedmann dust universes corrected for inhomogeneities, using locally inhomogeneous Swiss cheese models
Quasars red shifts distribution interpreted as due to cosmological and gravitational red shifts distribution, noting analysis error
Strong and weak emission red shifts of N galaxy 3C 390.3 in Balmer lines, indicating nonisothermal source and gas ejection
Large and small red shift quasars relative probability correlation with cataloged galaxies clusters direction
A hydrogen maser clock is proposed for enclosure in an orbiting satellite to measure the gravitational effect on time scales with high accuracy. This experiment is used to test the principle of equivalence for clocks in space. Extremely narrow linewidth of Fe-57 radiation and absorption due to Mossbauer effect over 75 ft vertical distance was used to confirm the prediction of the equivalence principle to 1 part in 100. The fractional frequency shift of a satellite-borne oscillator observed from earth is also given.
Direct measurements of the effects of gravitation on time are discussed. Using the earth's gravity these measurements can now be made to 20 parts per million. At present, there is a 1% verification of the equivalence principle for clocks made over a 75-ft vertical distance by use of Mossbauer gamma ray emission and absorption. Measurements made to greater accuracy and spanning distances where appreciable curvature of the metric of spacetime will help verify the equivalence principle, a postulate upon which Einstein developed his General Theory of Relativity.
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The radio spectral data of OH471 and OQ172 are shown in a graph along with decompositions of the spectra into canonical self-absorbed synchrotron components. The minimum number of canonical components consistent with the data is used. Theoretically expected angular radii and time scales are presented in a table. The estimation of the angular size of a compact radio source with known spectral form rests upon the establishment of its maximum brightness temperature.
The layout of a center frequency 2203.1 MHz antenna is presented. The four to one taped layout was photograph reduced and a single section was etched. Initial impedance and frequency mismatches were corrected, and impedance plots of each of the two sections are shown. With the 2203.1 MHz layout as a reference, initial layouts were made for the remaining two frequencies 2117.7 and 2299.7 MHz, and single sections were fabricated.
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