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By Peter G. Bergmann (auth.), Peter C. Aichelburg, Roman U. Sexl (eds.)

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A number of other research groups found nothing. A group in Tokyo and a group in Munich and Rome found smaller numbers of signals. These observations are very controversial. With improved sensitivity, it is hoped that there will be successful detection of radiation from sources as far away as the Virgo cluster of galaxies, by observatories throughout the world. Search for Radiation at Low Frequencies For very low frequencies, the earth and moon may be employed as elastic solid antennas. The earth may have oscillations excited at a frequency of one cycle every fifty-four minutes, and higher overtone frequencies.

G. Roll und D. T. Wilkinson, "Cosmic-black-body radiation", Astrophys. J. 142, p. 414 (1965). [14] G. Gamow. "The evolution of the universe", Nature 162, p. 680, (1948). [15] R. A. Alpher und R. C. Herman, "Evolution of the universe", Nature 162, p. 774 (1948). [16] G. M. Smoot, M. V Gorenstein und R. A. Miiller, "Detection of anisotropy in the cosmic blackbody radiation", Phys. Rev. Lett. 39, 14, p. 898 (1977). [17] S. W. Hawking und R. Penrose, "The singularity of gravitational collapse and cosmology", Proc.

As long ago as 1931, Subrahmanyan Chandrasekhar calculated that there must be a maximum mass above which a white dwarf could not sustain itself against even further gravitational contraction despite Pauli's Exclusion Principle. 5 times that of the sun. What is going to happen to them? The answer depends on just how heavy the star is. Consider a star of twice the mass of the sun. Like the sun it will also expand to an enormous size and then recontract, but being more massive than Chandrasekhar's limit for a white dwarf it will be unable to settle down to final equilibrium in the white dwa rf state.

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