Relativistic type 3 solar radio bursts

Details Relativistic type 3 solar radio bursts Relativistic type 3 solar radio bursts

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286..611p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 286, no. 2, p. 611-625

Astronomy and Astrophysics

Astronomy

15

Frequency Shift, Nonthermal Radiation, Plasma Jets, Radio Astronomy, Relativistic Electron Beams, Solar Corona, Solar Electrons, Solar Spectra, Type 3 Bursts, Decimeter Waves, Spectrographs, Ultrahigh Frequencies, Very High Frequencies

Scientific paper

Observations with the ARTEMIS multichannel radiospectrograph reveal a new class of type III solar radio bursts, generated by the relativistic head of electron beams. Compared to normal type III bursts, these bursts, which we call type IIId's, drift faster towards lower frequencies, have a shorter duration at fixed frequency and start at higher frequencies. An even more dramatic difference is that they often disappear suddenly before reaching the 100 MHz level. Sometimes they occur in front of normal type III's, forming characteristic pairs which cannot be fundamental-harmonic pairs because of the large difference in drift rates between the two components, giving a highly variable frequency ratio. The shortest characteristic drift times (0.0 +/- 0.1 s) are inconsistent with the differential group delay of fundamental radiation which must be 0.3 s or more; we conclude that type IIId's are emitted on the harmonic mode (2x plasma frequency). Fundamental-harmonic pairs occur mainly at f approximately less than 100 MHz. Type IIId - normal type III pairs, which occur at frequencies f approximately greater than 100 MHz, turn out to be of a different nature. We interpret them as due to the generation of plasma waves by the usual bump-on-the-tail instability in two zones along the electron beam, both radiating on the harmonic mode.

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