The polarization of second harmonic radio emission in Type III bursts

Details The polarization of second harmonic radio emission in Type III bursts The polarization of second harmonic radio emission in Type III bursts

Aug 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...101..250z&link_type=abstract

Astronomy and Astrophysics, vol. 101, no. 2, Aug. 1981, p. 250-258.

Astronomy and Astrophysics

Astrophysics

31

Harmonic Radiation, Plasma Waves, Polarized Electromagnetic Radiation, Solar Corona, Type 3 Bursts, Longitudinal Waves, Radiant Flux Density, Tensor Analysis, Wave Interaction

Scientific paper

The conversion of plasma waves into magneto-ionic modes in the solar corona is discussed as a possible origin of observed polarization of the second harmonic radio emission in Type III bursts. It is shown that earlier paper (Melrose and Sy, 1972; Melrose, Dulk and Smerd, 1978) concerning the subject involve an inaccuracy which results in omitting some important terms in the expression for the probability of longitudinal wave coalescence. In the present paper the problem is carefully analyzed. Along with the o-mode excess evident from the earlier theory, revised calculations explain the cosine law for centre-to-limb distribution of the second harmonic polarization. Observational data are in good agreement with the theory provided that the plasma waves excited by coronal electron streams and responsible for Type III bursts have nearly one-dimensional angular distribution. Corrected formula implies the magnetic fields in Type III sources to be of order B ≃ 4 Gauss. This field is stronger than that estimated by the fundamental polarization.

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