Abstract
THE existence of a number of radio sources with an angular extension less than 1″ is well known1. Some of them were identified with star-like objects and therefore they are referred to as radio stars. Among these are 3C-48, 3C-119, 3C-147, 3C-273, 3C-286. Their non-thermal spectra and the evidence of a rather strong linear polarization suggest the synchrotron mechanism of radio emission. Twiss2, Razin3, and Le Roux4 have shown that a self-absorption of synchrotron radiation by relativistic electrons must occur at frequencies f < f1, f1 depending on relativistic electrons concentration, normal component of magnetic field H⊥, spectral index of radio emission α (the spectrum being of the form S(f) ∝ f−a), and on linear dimension of radio-emitting region. At frequencies below f1 the spectrum of radio emission is S(f) ∝ f2.5 whatever α is, thus f1 is a frequency where maximum flux density of a radio source occurs.
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Allen, L. R., Anderson, B., Conway, R. G., Palmer, H. P., Reddish, V. C., and Rowson, B., Mon. Not. Roy. Astro. Soc., 124, 477 (1962).
Twiss, R. Q., Phil. Mag., 45, 249 (1954).
Razin, V. A., Izvestya Vyssh. Uch. Zav., sez. ‘Radiophysica’, 3, 584 (1960).
Le Roux, E., Ann. d'Astrophys., 24, 71 (1961).
Conway, R. G., Kellermann, K. I., and Long, R. J., Mon. Not. Roy. Astro. Soc., 125, 313 (1963).
Kellermann, K. I., Long, R. J., Allen, R. J., and Moran, M., Nature, 195, 692 (1962).
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SLISH, V. Angular Size of Radio Stars. Nature 199, 682 (1963). https://doi.org/10.1038/199682a0
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DOI: https://doi.org/10.1038/199682a0
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