Abstract
The relation between angular size and flux density depends on the world model and more strongly on evolution in radio source properties with epoch. I shall consider here the simplest forms of evolution that explain the observed θ-S relations (Swarup 1975; Kapahi 1975a, b; Ekers, this symposium).
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References
Colla, G., Fanti, C., Fanti, R., Gioia, I., Lari, C., Lequeux, J., Lucas, R. and Ulrich, M.H.: 1975, Astron.Astrophys. 38, 209.
Kapahi, V.K.: 1975a, Ph.D. Thesis, Tata Institute of Fundamental Research, Bombay.
Kapahi, V.K.: 1975b, Monthly Notices Roy. Astron. Soc. 172, 513.
Katgert, P.: 1976, Astron.Astrophys. 49, 221.
Swarup, G.: 1975, Monthly Notices Roy. Astron. Soc. 172, 501.
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© 1977 International Astronomical Union
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Kapahi, V.K. (1977). The Angular Size — Flux Density Relation. In: Jauncey, D.L. (eds) Radio Astronomy and Cosmology. International Astronomical Union / Union Astronomique Internationale, vol 74. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-1260-7_14
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DOI: https://doi.org/10.1007/978-94-010-1260-7_14
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