Abstract
An electron moving at relativistic speed β = v/c in a medium of refractive index n will emit Cerenkov radiation if βn> 1, and for a given β, this condition may be satisfied over some small wavelength range next to atomic lines, under favourable physical conditions. The radiation so produced will than look like broad lines, asymmetrical in shape and characteristically displaced from the atomic line. For this reason, J.H. You called this radiation the “Cerenkov line radiation”. The necessary physical conditions are that there should be a sufficient number of the atom in question and of the relativistic electrons.
Access this chapter
Tax calculation will be finalised at checkout
Purchases are for personal use only
Preview
Unable to display preview. Download preview PDF.
References
Ambarzumian V.A. (ed.) “Theoretical Astrophysics”, English translation by J.B. Sykes, 1958, Pergamon Press, p.424.
Neugebauer G., Oke J.B., Becklin E.E. & Matthews K., (1979) Ap.J.230:79.
Puetter R.C., Smith H.E.,et al.(1981) Ap. J.243:345.
Author information
Authors and Affiliations
Editor information
Editors and Affiliations
Rights and permissions
Copyright information
© 1986 Springer Science+Business Media Dordrecht
About this chapter
Cite this chapter
Kiang, T., You, J.H. (1986). Cerenkov Line Radiation — a New Interpretation of the Emission Lines of Quasars. In: Giuricin, G., Mardirossian, F., Mezzetti, M., Ramella, M. (eds) Structure and Evolution of Active Galactic Nuclei. Astrophysics and Space Science Library, vol 121. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-4562-3_54
Download citation
DOI: https://doi.org/10.1007/978-94-009-4562-3_54
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-8528-1
Online ISBN: 978-94-009-4562-3
eBook Packages: Springer Book Archive