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A Matter-Antimatter Model for Quasi-Stellar Objects

Published online by Cambridge University Press:  14 August 2015

Aina Elvius
Aina Elvius*
Affiliation:
Stockholm Observatory, Sweden

Abstract

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Observations of quasi-stellar objects and radio galaxies indicate that the total energy radiated from such objects is so large that the most likely source of energy is annihilation.

The demand for symmetry in the universe between ordinary matter and antimatter indicates that there must be equal quantities of the two kinds of matter in every galaxy. From this it seems likely that a galaxy is born as an ambiplasma body, in which separation of matter from antimatter leads to reasonably stable configurations.

The violent events observed in quasi-stellar objects are then interpreted in terms of collisions between stars of opposite kinds of matter. Such collisions are expected to occur frequently in very young galaxies with a high stellar density in the nucleus. Most of the gamma-radiation released in the annihilation will be absorbed in the gases of the colliding bodies, causing strong heating and violent explosions. Strong ionizing radiation and expanding gas clouds will give rise to the observed optical line emission. Expanding clouds of light ambiplasma will emit synchrotron radiation.

Type
Research Article
Information
Symposium - International Astronomical Union , Volume 44: External Galaxies and Quasi-Stellar Objects , 1972 , pp. 306 - 310
Copyright
Copyright © Reidel 1972 

References

Alfvén, H.: 1965, Rev. Mod. Phys. 37, 652.Google Scholar
Alfvén, H. and Elvius, A.: 1969, Science 164, 911.Google Scholar
Alfvén, H. and Klein, O.: 1963, Arkiv Fysik 23, No. 19.Google Scholar
Colgate, S. A.: 1969, Physics Today 22, 27.CrossRefGoogle Scholar
Elvius, A.: 1968, Lowell Obs. Bull. 7, 55.Google Scholar
Field, G. B.: 1964, Astrophys. J. 140, 1434.Google Scholar
Kellermann, K. I., Clark, B. G., Bare, C., Rydbeck, O. E. H., Ellder, J., Hansson, B., Kollberg, E., Höglund, B., Cohen, M. H., and Jauncey, D. L.: 1968, Astron. J. 73, S 101 and Astrophys. J. Letters 153, L209.Google Scholar
Kellermann, K. I. and Pauliny-Toth, I. I. K.: 1969, Astrophys. J. Letters 155, L71.CrossRefGoogle Scholar
Kinman, T. D., Lamla, E., and Wirtanen, C. A.: 1966, Astrophys. J. 146, 964.Google Scholar
Kinman, T. D., Lamla, E., Ciurla, T., Harlan, E., and Wirtanen, C. A.: 1968, Astrophys. J. 152, 357.Google Scholar
Kleinmann, D. E. and Low, F. J.: 1970, Astrophys. J. Letters 159, L165.Google Scholar
Low, F. J.: 1970, Astrophys. J. Letters 159, L173.CrossRefGoogle Scholar